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8603517

Olowin, Ronald Paul

PROBING THE LARGE-SCALE STRUCTURE OF THE UNIVERSE: AN ANALYSIS OF 55 BRIGHT SOUTHERN CLUSTERS OF

The University of Oklahom a Ph.D. 1985

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University Microfilms International

THE UNIVERSITY OF OKLAHOMA GRADUATE COLLEGE

PROBING THE LARGE-SCALE STRUCTURE OF THE UNIVERSE: AN ANALYSIS OF 55 BRIGHT SOUTHERN CLUSTERS OF GALAXIES

A DISSERTATION SUBMITTED TO THE GRADUATE FACULTY in partial fulfillment of the requirements for the degree of Doctor of Philosophy

by Ronald Paul Olowin

Norman, Oklahoma PROBING THE LARGE-SCALE STRUCTURE OF THE UNIVERSE: AN ANALYSIS OF 55 BRIGHT SOUTHERN CLUSTERS OF GALAXIES

A DISSERTATION APPROVED FOR THE DEPARTMENT OF PHYSICS AND ASTRONOMY

By

I Gnldo L. Chincarinl, Chair

--- David R. Branch

Tibor J. H^rcVeg

Ronald Kantowski

Thomas M. Smith DEDICATION

This thesis is dedicated to my family: in levins rnemory of my parents Clement Jan and Sophia Ann Olowin a n i with grateful appreciation of Mary Dreisbach, Aaron Benjamin and Frederick Alexander.

m DESIDERATUM

Melius est enim in via clauiicare quam praeter viam fortiter ambulare. Nam qui in via claudicat, etiam si parum proficiscatur, appropinquat ad terminum; qui vero extra viam ambulat, quanto fortius currit, tanto magis a termina elongatur. — Aquinas In laonnem

IV ACKNOWLEDGEMENTS

Financial support for this work came from the Department of Physics and As­ tronomy and the Associates of The University of Oklahoma. Without their generous infusion of funds, resources and equipment this effort would have been impossible. In particular, I would like to thank the Departmental Chairs during my tenure, David Golden and David Branch, for making so many facilities available so readily. Special thanks for the valuable and continued aid are given to A1 Schwarzkopf of the Statistical Consulting Laboratory of the Energy Resources Institute of the Univer­ sity of Oklahoma and Lynn Wellborn of the Physics and Astronomy Branch of the University of Oklahoma Libraries. My gratitude is also extended to Russell Cannon of the U. K. Schmidt Telescope Unit of the Royal Observatory, Edinburgh, Scotland for providing survey plates of the of Galaxies and to Wayne H. War­ ren of the National Space Science Data Center for providing a machine-readable version of the Smithsonian Astrophysical Observatory Catalogue.

My Professors have been patient and tolerant individuals. In particular, I have been privUedged to work under the guidance of David Branch, Guido Chincarini, John Cowan, Tibor Herczeg, Ronald Kantowski, Michael Morrison, Gregory Parker, Stan Robertson and Deborah Watson all of whom have made lasting contributions to my academic development.

During the production of this thesis the special assistance of Judith Tucker at Printing Concepts, Inc. has been extremely helpful. Likewise, my thanks go to Richard Henry and, in particular, to Michael Morrison who unraveled the mysteries of for me. My close friends have been invaluable. Sherman and Laura Kent have been steadfast, robust and nourishing allies. Lome Thomas and John Schiff have been marvelous role models of genuine scholarship in the highest academic tradition; they have rescued me innumenrable times from the arms of ignorance. I greatly appre­ ciate their unselfish support. Klaus Rossberg quietly maintained me throughout.

The special help and encouragement of Tibor Herczeg has been sustaining. His deep grasp of the History of Astronomy and his impeccable scholarship will always be an influence. The expert guidance and help from Harold Corwin has been immeasurable. The eager and generous support and advice he has given has illuminated for me what it means to do professional astronomy.

To Doris Jane Chediak I owe a sincere debt of gratitude and thanks. She has made a living and deep contribution to my growth and development and has been an invaluable asset to my family.

The advice and guidance of ray thesis advisor, Guido Chincarini, has been in­ dispensable. He has provided my first exposure to research on clusters of galaxies and throughout this effort has given me encouragement and unencumbered oppor­ tunities to broaden my astronomical experience. For this, for his sometimes painful honesty, and for his deep scientific integrity, I give Professor Chincarini my great and sincere thanks. I am extremely grateful for his time and friendship.

Finally, I wish to express my deepest appreciation to my family. That they tolerated this eff’ort and suffered my neglect with patience, unselfishness and wit is remarkable.

VI Table of Contents vii

TABLE OF CONTENTS

Page

D edication ...... iii

Desideratum ...... iv

Acknowledgements ...... v

Table of Contents ...... vii

List of Tables ...... ix

List of Illustrations ...... ixx

A b stra ct ...... xxxii

Chapter 1. The Discovery of Clusters of Galaxies ...... 1

Chapter 2. Data Acquisition and Preparation ...... 8

2.1. Measuring the Clusters ...... 10

2.2. The Step-Scale Calibrations ...... 14

2.3. Coordinate Transformation of Measurements ...... 18

2.4. Determination of Cluster Centers ...... 27

2.5. The Classification of Clusters ...... 35

vu Table of Contents viii

Page

Chapter 3. The Cluster Catalogue ...... 43

3.1. Catalogue of Bright Southern Galaxy Clusters ...... 47

3.2. Descriptions of Bright Southern Galaxy Clusters ...... 50

Chapter 4. An Isothermal Analysis of Clusters of Galaxies ...... 251

4.1. Theory of the Isothermal Gas Sphere ...... 255

4.2. Isothermal Fitting Procedure Utilizing ...... 259

4.3. The Isothermal Analysis ...... 262

4.4. Isothermal Analysis of Bright Southern Galaxy Clusters ...... 266

Chapter 5. The Abell Clusters ...... 467

5.1. Description and Isothermal Analysis of 5 Abell Clusters ...... 468

Chapter 6. Conclusion ...... 507

6.1. Observational Features of Bright Southern Clusters of Galaxies .. . 512

6.2. Cluster Parameters ...... 514

Bibliography ...... 521

vm List of Tables

LIST OF TABLES

Table Page

2.5.01. Abell Richness Subdivisions for Galaxy Clusters ...... 35

2.5.02. The Bautz-Morgan ClassiBcation ...... 38

2.5.03. T ie Rood-Sastry Cluster ClassiScation Scheme ...... 40

3.1.01. (a.-b.) Catalogue of Bright Soutieru Galaxy Clusters ...... 48-49

3.2.01. 01: Cluster Population Description ...... 53

3.2.02. Galaxy Cluster 02: Cluster Population Description ...... 57

3.2.03. Galaxy Cluster 03: Cluster Population Description ...... 61

3.2.04. Galaxy Cluster 04: Cluster Population Description ...... 65

3.2.05. Galaxy Cluster 05: Cluster Population Description ...... 69

3.2.06. Galaxy Cluster 06: Cluster Population Description ...... 73

3.2.07. Galaxy Cluster 07: Cluster Population Description ...... 77

3.2.08. Galaxy Cluster OS: Cluster Population Description ...... 81

3.2.09. Galaxy Cluster 09: Cluster Population Description ...... 85

3.2.10. Galaxy Cluster 10: Cluster Population Description ...... 89

3.2.11. Galaxy Cluster 11: Cluster Population Description ...... 93

3.2.12. Galaxy Cluster 12: Cluster Population Description ...... 97

ix List of Tables

3.2.13. Galaxy Cluster 13: Cluster Population Description ...... 101

3.2.14. Galaxy Cluster 14: Cluster Population Description ...... 105

3.2.15. Galaxy Cluster 15: Cluster Population Description ...... 109

3.2.16. Galaxy Cluster 16: Cluster Population Description ...... 113

3.2.17. Galaxy Cluster 17: Cluster Population Description ...... 117

3.2.18. Galaxy Cluster 18: Cluster Population Description ...... 121

3.2.19. Galaxy Cluster 19: Cluster Population Description ...... 125

3.2.20. Galaxy Cluster 20: Cluster Population Description ...... 129

3.2.21. Galaxy Cluster 21: Cluster Population Description ...... 133

3.2.22. Galaxy Cluster 22: Cluster Population Description ...... 137

3.2.23. Galaxy Cluster 23: Cluster Population Description ...... 141

3.2.24. Galaxy Cluster 24: Cluster Population Description ...... 145

3.2.25. Galaxy Cluster 25: Cluster Population Description ...... 149

3.2.26. Galaxy Cluster 26: Cluster Population Description ...... 153

3.2.27. Galaxy Cluster 27: Cluster Population Description ...... 157

3.2.28. Galaxy Cluster 28: Cluster Population Description ...... 161

3.2.29. Galaxy Cluster 29: Cluster Population Description ...... 165

3.2.30. Galaxy Cluster 30: Cluster Population Description ...... 169 List of Tables

3.2.31. Galaxy Cluster 31: Cluster Population Description ...... 173

3.2.32. Galaxy Cluster 32: Cluster Population Description ...... 177

3.2.33. Galaxy Cluster 33: Cluster Population Description ...... 181

3.2.34. Galaxy Cluster 34: Cluster Population Description ...... 185

3.2.35. Galaxy Cluster 35: Cluster Population Description ...... 189

3.2.36. Galaxy Cluster 36: Cluster Population Description ...... 193

3.2.37. Galaxy Cluster 37: Cluster Population Description ...... 197

3.2.38. Galaxy Cluster 38: Cluster Population Description ...... 201

3.2.39. Galaxy Cluster 39: Cluster Population Description ...... 205

3.2.40. Galaxy Cluster 40: Cluster Population Description ...... 209

3.2.41. Galaxy Cluster 41: Cluster Population Description ...... 213

3.2.42. Galaxy Cluster 42: Cluster Population Description ...... 217

3.2.43. Galaxy Cluster 43: Cluster Population Description ...... 221

3.2.44. Galaxy Cluster 44: Cluster Population Description ...... 225

3.2.45. Galaxy Cluster 45: Cluster Population Description ...... 229

3.2.46. Galaxy Cluster 46: Cluster Population Description ...... 233

3.2.47. Galaxy Cluster 47: Cluster Population Description ...... 237

3.2.48. Galaxy Cluster 48: Cluster Population Description ...... 241

XI List of Tables

2.2.49. Galaxy Cluster 49: Cluster Population Description ...... 245

3.2.50. Galaxy Cluster 50: Cluster Population Description ...... 249

4.4.01. (a.) Ring Count Data for Galaxy Cluster 01 ...... 268

4.4.01. (h.) Cluster Parameters for Galaxy Cluster 01 ...... 270

4.4.02. (a.) Ring Count Data for Galaxy Cluster 02 ...... 272

4.4.02. (b.) Cluster Parameters for Galaxy Cluster 02...... 274

4.4.03. (a.J Ring Count Data for Galaxy Cluster 03 ...... 276

4.4.02. (b.) Cluster Parameters for Galaxy Cluster 03 ...... 278

4.4.04. (a.) Ring Count Data for Galaxy Cluster 04 ...... 280

4.4.04. (b.) Cluster Parameters for Galaxy Cluster 04 ...... 282

4.4.05. (a.) Ring Count Data for Galaxy Cluster 05 ...... 284

4.4.05. (b.) Cluster Parameters for Galaxy Cluster 05 ...... 286

4.4.06. (a.) Ring Count Data for Galaxy Cluster 06 ...... 288

4.4.06. (b.) Cluster Parameters for Galaxy Cluster 06...... 290

4.4.07. (a.) Ring Count Data for Galaxy Cluster 07...... 292

4.4.07. (b.) Cluster Parameters for Galaxy Cluster 07...... 294

4.4.08. (a.) Ring Count Data for Galaxy Cluster 08...... 296

4.4.08. (b.) Cluster Parameters for Galaxy Cluster 08...... 298

Xll List of Tables

4.4.09. (a.) Riag Count Data for Galaxy Cluster 09 ...... 300

4.4.09. (b.) Cluster Parameters for Galaxy Cluster 09 ...... 302

4.4.10. (a.J Ring Count Data for Galaxy Cluster 10 ...... 304

4.4.10. (b.) Cluster Parameters for Galaxy Cluster 10 ...... 306

4.4.11. (a.) Ring Count Data for Galaxy Cluster 11 ...... 308

4.4.11. (b.) Cluster Parameters for Galaxy Cluster 11 ...... 310

4.4.12. (a.) Ring Count Data for Galaxy Cluster 12...... 312

4.4.12. (b.) Cluster Parameters for Galaxy Cluster 12 ...... 314

4.4.13. (a.) Ring Count Data for Galaxy Cluster 13 ...... 316

4.4.13. (b.) Cluster Parameters for Galaxy Cluster 13 ...... 318

4.4.14. (a.) Ring Count Data for Galaxy Cluster 14 ...... 320

4.4.14. (b.) Cluster Parameters for Galaxy Cluster 14 ...... 322

4.4.15. (a.) Ring Count Data for Galaxy Cluster 15 ...... 324

4.4.15. (b.) Cluster Parameters for Galaxy Cluster 15 ...... 326

4.4.16. (a.) Ring Count Data for Galaxy Cluster 16 ...... 328

4.4.16. (b.) Cluster Parameters for Galaxy Cluster 16 ...... 330

4.4.17. (a.) Ring Count Data for Galaxy Cluster 17...... 332

4.4.17. (b.) Cluster Parameters for Galaxy Cluster 17...... 334

xm List of Tables

4.4.18. (a.) Ring Count Data for Galaxy Cluster IS. 336

4.4.18. b.) Cluster Parameters for Galaxy Cluster 18 ...... 338

4.4.19. I.) Ring Count Data for Galaxy Cluster 19 ...... 340

4.4.19. b.) Cluster Parameters for Galaxy Cluster 19 ...... 342

4.4.20. a.J Ring Count Data for Galaxy Cluster 20 ...... 344

4.4.20. b.) Cluster Parameters for Galaxy Cluster 20 ...... 346

4.4.21. a.) Ring Count Data for Galaxy Cluster 21...... 348

4.4.21. b.J Cluster Parameters for Galaxy Cluster 21 ...... 350

4.4.22. a.) Ring Count Data for Galaxy Cluster 22 ...... 352

4.4.22. b.) Cluster Parameters for Galaxy Cluster 22. 354

4.4.22. a.) Ring Count Data for Galaxy Cluster 23 ...... 356

4.4.23. b.) Cluster Parameters for Galaxy Cluster 23 ...... 358

4.4.24. a.) Ring Count Data for Galaxy Cluster 24. 360

4.4.24. b.) Cluster Parameters for Galaxy Cluster 24 ...... 362

4.4.25. a.) Ring Count Data for Galaxy Cluster 25 ...... 364

4.4.25. b.) Cluster Parameters for Galaxy Cluster 25 ...... 366

4.4.26. a.) Ring Count Data for Galaxy Cluster 26 ...... 368

4.4.26. b.) Cluster Parameters for Galaxy Cluster 26 ...... 370

XIV List of Tables

4.4.27. (a.) Ring Count Data for Galaxy Cluster 27...... 372

4.4.27. (b.) Cluster Parameters for Galaxy Cluster 27...... 374

4.4.28. (a.) Ring Count Data for Galaxy Cluster 28 ...... 376

4.4.28. (b.) Cluster Parameters for Galaxy Cluster 28 ...... 378

4.4.29. (a.) Ring Count Data for Galaxy Cluster 29 ...... 380

4.4.29. (b.) Cluster Parameters for Galaxy Cluster 29...... 382

4.4.30. (a.) Ring Count Data for Galaxy Cluster 30 ...... 384

4.4.30. (b.) Cluster Parameters for Galaxy Cluster 30 ...... 386

4.4.31. (a.) Ring Count Data for Galaxy Cluster 31 ...... 388

4.4.31. (b.) Cluster Parameters for Galaxy Cluster 31 ...... 390

4.4.32. (a.) Ring Count Data for Galaxy Cluster 32...... 392

4.4.32. (b.) Cluster Parameters for Galaxy Cluster 32...... 394

4.4.33. (a.) Ring Count Data for Galaxy Cluster 33 ...... 396

4.4.33. (b.) Cluster Parameters for Galaxy Cluster 33 ...... 398

4.4.34. (a.) Ring Count Data for Galaxy Cluster 34 ...... 400

4.4.34. (b.) Cluster Parameters for Galaxy Cluster 34 ...... 402

4.4.35. (a.) Ring Count Data for Galaxy Cluster 35 ...... 404

4.4.35. (b.J Cluster Parameters for Galaxy Cluster 35 ...... 406

XV List of Tables

4.4.36. (a.) Riag Count Data for Galaxy Cluster 36 ...... 408

4.4.36. (b.) Cluster Parameters for Galaxy Cluster 36 ...... 410

4.4.37. (a.) Ring Count Data for Galaxy Cluster 37...... 412

4.4.37. (b.J Cluster Parameters for Galaxy Cluster 37...... 414

4.4.38. (a.j Ring Count Data for Galaxy Cluster 38 ...... 416

4.4.38. (b.J Cluster Parameters for Galaxy Cluster 38 ...... 418

4.4.39. (a.) Ring Count Data for Galaxy Cluster 39 ...... 420

4.4.39. (b.J Cluster Parameters for Galaxy Cluster 39 ...... 422

4.4.40. (a.) Ring Count Data for Galaxy Cluster 40 ...... 424

4.4.40. (b.J Cluster Parameters for Galaxy Cluster 40 ...... 426

4.4.41. (a.) Ring Count Data for Galaxy Cluster 41...... 428

4.4.41. fb.) Cluster Parameters for Galaxy Cluster 41 ...... 430

4.4.42. (a.) Ring Count Data for Galaxy Cluster 42...... 432

4.4.42. (b.) Cluster Parameters for Galaxy Cluster 42...... 434

4.4.43. (a.) Ring Count Data for Galaxy Cluster 43 ...... 436

4.4.43. (b.J Cluster Parameters for Galaxy Cluster 43 ...... 438

4.4.44. (a.) Ring Count Data for Galaxy Cluster 44 ...... 440

4.4.44. (b.) Cluster Parameters for Galaxy Cluster 44 ...... 442

xvi List of Tables

4.4.45. (a.) Ring Count Data for Galaxy Cluster 45 ...... 444

4.4.45. (b.J Cluster Parameters for Galaxy Cluster 45 ...... 446

4.4.46. (a.) Ring Count Data for Galaxy Cluster 46 ...... 448

4.4.46. (b.) Cluster Parameters for Galaxy Cluster 46 ...... 450

4.4.47. (a.) Ring Count Data for Galaxy Cluster 47...... 452

4.4.47. (b.J Cluster Parameters for Galaxy Cluster 47...... 454

4.4.48. (a.j Ring Count Data for Galaxy Cluster 48 ...... 456

4.4.48. (b.J Cluster Parameters for Galaxy Cluster 48 ...... 458

4.4.49. (a.j Ring Count Data for Galaxy Cluster 49 ...... 460

4.4.49. (b.J Cluster Parameters for Galaxy Cluster 49 ...... 462

4.4.50. (a.J Ring Count Data for Galaxy Cluster 50 ...... 464

4.4.50. (b.J Cluster Parameters for Galaxy Cluster 50...... 466

5.1.01. (a.j Abell Cluster 0428: Population Description ...... 470

5.1.01. (b.J Ring Count Data for Abell Cluster 0428 ...... 473

5.1.01. (c.J Cluster Parameters for Abell Cluster 0428 ...... 475

5.1.02. (a.j Abell Cluster 0514: Population Description ...... 477

5.1.02. (b.J Ring Count Data for Abell Cluster 0514 ...... 481

5.1.02. (c.J Cluster Parameters for Abell Cluster 0514 ...... 483

xvii List of Tables

5.1.03. (a.) Abell Cluster 0533: Population Description ...... 485

5.1.03. (b.) Ring’ Count Data for Abell Cluster 0533 ...... 489

5.1.03. (c.) Cluster Parameters for Abell Cluster 0533 ...... 491

5.1.04. (a.) Abell Cluster 1736: Population Description ...... 493

5.1.04. (b.) Ring Count Data for Abell Cluster 1736 ...... 497

5.1.04. (c.) Cluster Parameters for Abell Cluster 1736 ...... 499

5.1.05. (a.) Abell Cluster 2538: Population Description ...... 501

5.1.05. (b.) Ring Count Data for Abell Cluster 2538 ...... 504

5.1.05. (c.) Cluster Parameters for Abell Cluster 2538 ...... 506

6.1.01. (a.-b.) Catalogue of Bright Southern Clusters of Galaxies 509-510

XVlIl List of Illustrations

LIST OF ILLUSTRATIONS

Figure Page

2.1.1. Schematic of X-Y Digitizer ...... 11

2.1.2. Circle Counting Mask Divided Into Abell-radii and Sectors ...... 13

2.2.1. Typical Step-Scales for Magnitude Determination ...... 14

2.2.2. Step-Scale Calibration Curve ...... 17

2.3.1. Plane Coordinates. Cross Section of the Celestial Sphere ...... 19

2.3.2. Tangential or Standard Coordinate System ...... 20

2.3.3. 0-C Diagram for Standard Star Reductions ...... 23

2.3.4. Spherical Triangle GTP...... 24

2.4.1. Isolines Representing a Bivariate Normal Distribution ...... 33

2.4.2. N-S and E-W Strip Counts for Galaxy Clusters ...... 34

3.2.01. (a.) Field of Galaxy Cluster 01: 00 00 46 -36 19 ...... 51

3.2.01. (b.-h.) Cluster Morphology and Statistical Distributions ...... 52-53

3.2.02. (a.) Field of Galaxy Cluster 02: 00 03 14 -35 04 ...... 55

3.2.02. (b.-h.) Cluster Morphology and Statistical Distributions ...... 56-57

3.2.03. (a.) Field of Galaxy Cluster 03: 00 06 49 -35 44 ...... 59

3.2.03. (b.-b.) Cluster Morphology and Statistical Distributions ...... 60-61

xix List of Illustrations

3.2.04. (a.) Field of Galaxy Cluster 04: 00 0 7 29 -57 15 ...... 63

3.2.04. (b.-b.) Cluster Morphology’ and Statistical Distributions ...... 64-65

3.2.05. (a.) Field of Galaxy Cluster 05: 00 18 08 -49 32...... 67

3.2.05. (b.-h.) Cluster Morphology and Statistical Distributions ...... 68-69

3.2.06. (a.) Field of Galaxy Cluster 06: 00 22 50 -33 1 7...... 71

3.2.06. (b.-h.) Cluster Morphology and Statistical Distributions...... 72-73

3.2.07. (a.) Field of Galaxy Cluster 07: 01 29 34 -51 33 ...... 75

3.2.07. (b.-h.) Cluster Morphology and Statistical Distributions ...... 76-77

3.2.08. (a.) Field of Galaxy Cluster 08: 01 39 50 -42 24 ...... 79

3.2.08. (b.-h.) Cluster Morphology and Statistical Distributions...... 80-81

3.2.09. (a.) Field of Galaxy Cluster 09: 02 55 44 -52 56 ...... 83

3.2.09. (b.-h.) Cluster Morphology and Statistical Distributions ...... 84-85

3.2.10. (a.) Field of Galaxy Cluster 10: 03 44 05 -41 21 ...... 87

3.2.10. (b.-h.) Cluster Morphology and Statistical Distributions ...... 88-89

3.2.11. (a.) Field of Galaxy Cluster 11: 04 04 04 -39 00 ...... 91

3.2.11. (b.-h.) Cluster Morphology and Statistical Distributions ...... 92-93

3.2.12. (a.) Field of Galaxy Cluster 12: 05 24 00 -45 01 ...... 95

3.2.12. (b.-b.) Cluster Morphology and Statistical Distributions ...... 96-97

XX List of Illustrations

3.2.13. (a.) Field of Galaxy Cluster 13: 06 21 39 -64 56 ...... 99

3.2.13. (b.-h.) Cluster Morphology and Statistical Distributions. . . 100-101

3.2.14. (a.) Field of Galaxy Cluster 14: 06 25 02 -53 39 ...... 103

3.2.14. (b.-h.) Cluster Morphology and Statistical Distributions. . . , 104-105

3.2.15. (a.) Field of Galaxy Cluster 15: 06 26 25 -54 22 ...... 107

3.2.15. (b.-h.) Cluster Morphology and Statistical Distributions. . . 108-109

3.2.16. (a.) Field of Galaxv Cluster 16: 12 51 41 -28 44 ...... I l l

3.2.16. (b.-h.) Cluster Morphology and Statistical Distributions. . . , , 112-113

3.2.17. (a.) Field of Galaxy Cluster 17: 13 03 25 -37 18 ...... 115

3.2.17. (b.-h.) Cluster Morphology and Statistical Distributions. . . , . . 116-117

3.2.18. (a.) Field of Galaxy Cluster 18: 14 00 41 -33 44 ...... 119

3.2.18. (b.-h.) Cluster Morphology and Statistical Distributions...... 120-121

3.2.19. (a.) Field of Galaxy Cluster 19: 14 09 18 -32 50 ...... 123

3.2.19. (b.-h.) Cluster Morphology and Statistical Distributions...... 124-125

3.2.20. (a.) Field of Galaxy Cluster 20: 14 09 28 -34 01 ...... 127

3.2.20. (b.-h.) Cluster Morphology and Statistical Distributions. . . 128-129

3.2.21. (a.) Field of Galaxy Cluster 21: 14 30 26 -31 33 ...... 131

3.2.21. (b.-h.) Cluster Morphology and Statistical Distributions. . . 132-133

xxi List of Illustrations

3.2.22. (a..) Field of Galaxy Cluster 22: 19 56 35 -38 33 ...... 135

3.2.22. (b.-b.) Cluster Morpholep and Statistical Distributions. . . , ,, 136-137

3.2.23. (a.) Field of Galaxy Cluster 23: 20 38 34 -35 24 ...... 139

3.2.23. (b.-h.) Cluster Morphology and Statistical Distributions...... 140-141

3.2.24. (a.) Field of Galaxy Cluster 24: 20 48 41 -52 08 ...... 143

3.2.24. (b.-h.) Cluster Morphology and Statistical Distributions. . . , , , 144-145

3.2.25. (a.) Field of Galaxy Cluster 25: 2113 10 -59 36...... 147

3.2.25. (b.-h.) Cluster Morphology and Statistical Distributions. . . 148-149

3.2.26. (a.) Field of Galaxy Cluster 26: 21 22 58 -35 00...... 151

3.2.26. (b.-h.) Cluster Morphology and Statistical Distributions. . . 152-153

3.2.27. (a.) Field of Galaxy Cluster 27: 21 26 10 -51 04 ...... 155

3.2.27. (b.-h.) Cluster Morphology and Statistical Distributions. . . 156-157

3.2.28. (a.) Field of Galaxy Cluster 28: 21 29 13 -35 23 ...... 159

3.2.28. (b.-h.) Cluster Morphology and Statistical Distributions. . . 160-161

3.2.29. (a.) Field of Galaxy Cluster 29: 21 31 14 -62 15 ...... 163

3.2.29. (b.-h.) Cluster Morphology and Statistical Distributions. . . 164-165

3.2.30. (a.) Field of Galaxy Cluster 30: 21 31 06 -53 50 ...... 167

3.2.30. (b.-h.) Cluster Morphology and Statistical Distributions. . . 168-169

xxii List of Illustrations

3.2.31. (a.) Field of Galaxy Cluster 31: 21 32 18 -52 44 ...... 171

3.2.31. (b.-b.) Cluster Morphology and Statistical Distributions. .. . . , 172-173

3.2.32. (a.) Field of Galaxy Cluster 32: 21 41 46 -51 44 ...... 175

3.2.32. (b.-h.) Cluster Morphology and Statistical Distributions...... 176-177

3.2.33. (a.) Field of Galaxy Cluster 33: 21 42 51 -57 30 ...... 179

3.2.33. (b.-h.) Cluster Morphology and Statistical Distributions. .. 180-181

3.2.34. (a.) Field of Galaxy Cluster 34: 21 43 46 -44 06 ...... 183

3.2.34. (b.-h.) Cluster Morpholog}'and Statistical Distributions. .. 184-185

3.2.35. (a.) Field of Galaxy Cluster 35: 21 44 41 -46 13 ...... 187

3.2.35. (b.-h.) Cluster Morphology and Statistical Distributions. .. 188-189

3.2.36. (a.) Field of Galaxy Cluster 36: 21 50 32 -58 04 ...... 191

3.2.36. (b.-h.) Cluster Morphology and Statistical Distributions. .. 192-193

3.2.37. (a.) Field of Galaxy Cluster 37: 21 55 17 -60 35 ...... 195

3.2.37. (b.-h.) Cluster Morphology and Statistical Distributions. . . ., , 196-197

3.2.38. (a.) Field of Galaxy Cluster 38: 21 58 08 -60 11 ...... 199

3.2.38. (b.-h.) Cluster Morphology and Statistical Distributions. . . , 2 0 0 - 2 0 1

3.2.39. (a.) Field of Galaxy Cluster 39: 22 01 11 -58 18 ...... 203

3.2.39. (b.-h.) Cluster Morphology and Statistical Distributions...... 204-205

XXlll List of Illustrations

3.2.40. (a.) Field o f Galaxy Cluster 40: 22 01 07 -50 18 ...... 207

3.2.40. (b.-b.) Cluster Morpbology and Statistical Distributions. . . , , , 208-209

3.2.41. (a.) Field of Galaxy Cluster 41: 2219 59 -50 23 ...... 2 1 1

3.2.41. (b.-b.) Cluster Morpbology and Statistical Distributions. . . , . 212-213

3.2.42. (a.) Field o f Galaxy Cluster 42: 22 21 25 -56 38...... 215

3.2.42. (b.-b.) Cluster Morpbology and Statistical Distributions. . . , , , 216-217

3.2.43. (a.) Field of Galaxy Cluster 43: 22 22 36 -56 06 ...... 219

3.2.43. (b.-b.) Cluster Morpbology and Statistical Distributions. . . 2 2 0 - 2 2 1

3.2.44. (a.) Field of Galaxy Cluster 44: 22 24 46 -30 52 ...... 223

3.2.44. (b.-b.) Cluster Morpbology and Statistical Distributions. .. 224-225

3.2.45. (a.) Field o f Galaxy Cluster 45: 23 16 35 -42 22...... 227

3.2.45. (b.-b.) Cluster Morpbology and Statistical Distributions. .. 228-229

3.2.46. (a.) Field of Galaxy Cluster 46: 23 27 36 -39 37...... 231

3.2.46. (b.-b.) Cluster Morpbology and Statistical Distributions. . . 232-233

3.2.47. (a.) Field of Galaxy Cluster 47: 23 34 24 -69 35 ...... 235

3.2.47. (b.-b.) Cluster Morpbology' and Statistical Distributions. . . 236-237

3.2.48. (a.) Field of Galaxy Cluster 48: 23 38 42 -30 30 ...... 239

3.2.48. (b.-b.) Cluster Morpbology and Statistical Distributions. . . ,, , 240-241

xxiv List of Illustrations

3.2.49. (a.) Field of Galaxy Cluster 49: 23 44 55 -28 25 ...... 243

3.2.49. (b.-b.) Cluster Morphology and Statistical Distributions. .. , . 244-245

3.2.50. (a.) Field of Galaxy Cluster 50: 23 59 06 -44 07...... 247

3.2.50. (b.-b.) Cluster Morpbology and Statistical Distributions. . . 248-249

4.1.1. Idealized Isothermal Sphere of Galaxies ...... 255

4.1.2. Coordinate Projections on the Celestial Sphere ...... 257

4.2.1. Function in an n-Dimensional Hvperspace ...... 260

4.4.01. (a.-d.) Galaxy Cluster 01: Surface Density Statistics ...... 267

4.4.01. (e.) Isothermal Fit for Galaxy Cluster 01 ...... 269

4.4.02. (a.-d.) Galaxy Cluster 02: Surface Density Statistics ...... 271

4.4.02. (e.) Isothermal Fit for Galaxy Cluster 02 ...... 273

4.4.03. (a.-d.) Galaxy Cluster 03: Surface Density Statistics ...... 275

4.4.03. (e.) Isothermal Fit for Galaxy Cluster 03 ...... 277

4.4.04. (a.-d.) Galaxy Cluster 04: Surface Density Statistics ...... 279

4.4.04. (e.) Isothermal Fit for Galaxy Cluster 04 ...... 281

4.4.05. (a.-d.) Galaxy Cluster 05: Surface Density Statistics ...... 283

4.4.05. (e.) Isothermal Fit for Galaxy Cluster 05 ...... 285

4.4.06. (a.-d.) Galaxy Cluster 06: Surface Density Statistics ...... 287

XXV List of Illustrations

4.4.06. (e.) Isothermal Fit for Galaxy Cluster 06 ...... 289

4.4.07. (a.-d.) Galaxy Cluster 07: Surface Density Statistics...... 291

4.4.07. (e .) Isothermal Fit for Galaxy Cluster 07...... 293

4.4.08. (a.-d.) Galaxy Cluster 08: Surface Density Statistics ...... 295

4.4.08. (e .) Isothermal Fit for Galaxy Cluster 08 ...... 297

4.4.09. (a.-d.) Galaxy Cluster 09: Surface Density Statistics...... 299

4.4.09. (e .) Isothermal Fit for Galaxy Cluster 09 ...... 301

4.4.10. (a.-d.) Galaxy Cluster 10: Surface Density Statistics ...... 303

4.4.10. (e.) Isothermal Fit for Galaxy Cluster 10 ...... 305

4.4.11. (a.-d.) Galaxy Cluster 11: Surface Density Statistics ...... 307

4.4.11. (e .) Isothermal Fit for Galaxy Cluster 11 ...... 309

4.4.12. (a.-d.) Galaxy Cluster 12: Surface Density Statistics ...... 311

4.4.12. (e .) Isothermal Fit for Galaxy Cluster 12. 313

4.4.13. (a.-d.) Galaxy Cluster 13: Surface Density Statistics...... 315

4.4.13. (e.) Isothermal Fit for Galaxy Cluster 13 ...... 317

4.4.14. (a.-d.) Galaxy Cluster 14: Surface Density Statistics ...... 319

4.4.14. (e.) Isothermal Fit for Galaxy Cluster 14 ...... 321

4.4.15. (a.-d.) Galaxy Cluster 15: Surface Density Statistics ...... 323

xxvi List of Illustrations

4.4.15. (e.) Isothermal Fit for Galaxy Cluster 15 ...... 325

4.4.16. (a.-d.) Galaxy Cluster 16: Surface Density Statistics ...... 327

4.4.16. (e.) Isothermal Fit for Galaxy Cluster 16 ...... 329

4.4.17. (a.-d.) Galaxy Cluster 17: Surface Density Statistics ...... 331

4.4.17. (e.) Isothermal Fit for Galaxy Cluster 17...... 333

4.4.18. (a.-d.) Galaxy Cluster 18: Surface Density Statistics ...... 335

4.4.18. (e.) Isothermal Fit for Galaxy Cluster 18 ...... 337

4.4.19. (a.-d.) Galaxy Cluster 19: Surface Density Statistics ...... 339

4.4.19. (e.) Isothermal Fit for Galaxy Cluster 19 ...... 341

4.4.20. (a.-d.) Galaxy Cluster 20: Surface Density Statistics ...... 343

4.4.20. (e.) Isothermal Fit for Galaxy Cluster 20 ...... 345

4.4.21. (a.-d.) Galaxy Cluster 21: Surface Density Statistics ...... 347

4.4.21. (e .) Isothermal Fit for Galaxy Cluster 21 ...... 349

4.4.22. (a.-d.) Galaxy Cluster 22: Surface Density Statistics ...... 351

4.4.22. (e .) Isothermal Fit for Galaxy Cluster 22...... 353

4.4.23. (a.-d.) Galaxy Cluster 23: Surface Density Statistics ...... 355

4.4.23. (e .) Isothermal Fit for Galaxy Cluster 23 ...... 357

4.4.24. (a.-d.) Galaxy Cluster 24: Surface Density Statistics ...... 359

xxvii List of Illustrations

4.4.24. (e.) Isothermal Fit for Galaxy Cluster 24 ...... 361

4.4.25. (a.-d.) Galaxy Cluster 25: Surface Density Statistics ...... 363

4.4.25. (e.) Isothermal Fit for Galaxy Cluster 25 ...... 365

4.4.26. (a.-d.) Galaxy Cluster 26: Surface Density Statistics ...... 367

4.4.26. (e.) Isothermal Fit for Galaxy Cluster 26 ...... 369

4.4.27. (a.-d.) Galaxy Cluster 27: Surface Density Statistics ...... 371

4.4.27. (e.) Isothermal Fit for Galaxy Cluster 27...... 373

4.4.28. (a.-d.) Galaxy Cluster 28: Surface Density Statistics ...... 375

4.4.28. (e.) Isothermal Fit for Galaxy Cluster 28 ...... 377

4.4.29. (a.-d.) Galaxy Cluster 29: Surface Density Statistics ...... 379

4.4.29. (e.) Isothermal Fit for Galaxy Cluster 29 ...... 381

4.4.30. (a.-d.) Galaxy Cluster 30: Surface Density Statistics...... 383

4.4.30. (e.) Isothermal Fit for Galaxy Cluster 30 ...... 385

4.4.31. (a.-d.) Galaxy Cluster 31: Surface Density Statistics ...... 387

4.4.31. (e.) Isothermal Fit for Galaxy Cluster 31 ...... 389

4.4.32. (a.-d.) Galaxy Cluster 32: Surface Density Statistics...... 391

4.4.32. (e.) Isothermal Fit for Galaxy Cluster 32 ...... 393

4.4.33. (a.-d.) Galax}’ Cluster 33: Surface Density Statistics ...... 395

xxviii List of Illustrations

4.4.32. (e.) Isothermal Fit for Galaxy Cluster 33 ...... 397

4.4.34. (a.-d.) Galaxy Cluster 34: Surface Density Statistics ...... 399

4.4.34. (e.) Isothermal Fit for Galaxy Cluster 34 ...... 401

4.4.35. (a.-d.) Galaxy Cluster 35: Surface Density Statistics ...... 403

4.4.35. (e.) Isothermal Fit for Galaxy Cluster 35 ...... 405

4.4.36. (a.-d.) Galaxy Cluster 36: Surface Density Statistics ...... 407

4.4.36. (e.) Isothermal Fit for Galaxy Cluster 36 ...... 409

4.4.37. (a.-d.) Galaxy Cluster 37: Surface Density Statistics ...... 411

4.4.37. (e.) Isothermal Fit for Galaxy Cluster 27...... 413

4.4.38. (a.-d.) Galaxy Cluster 38: Surface Density Statistics ...... 415

4.4.38. (e.) Isothermal Fit for Galaxy Cluster 38 ...... 417

4.4.39. (a.-d.) Galaxy Cluster 39: Surface Density Statistics ...... 419

4.4.39. (e.) Isothermal Fit for Galaxy Cluster 39 ...... 421

4.4.40. (a.-d.) Galaxy Cluster 40: Surface Density Statistics ...... 423

4.4.40. (e.) Isothermal Fit for Galaxy Cluster 40 ...... 425

4.4.41. (a.-d.) Galaxy Cluster 41: Surface Density Statistics ...... 427

4.4.41. (e.) Isothermal Fit for Galaxy Cluster 41 ...... 429

4.4.42. (a.-d.) Galaxy Cluster 42: Surface Density Statistics ...... 431

xxix List of Illustrations

4.4.42. (e.) Isothermal Fit for Galaxy Cluster 42 ...... 433

4.4.43. (a.-d.) Galaxy Cluster 43: Surface Density Statistics...... 435

4.4.43. (e.) Isothermal Fit for Galaxy Cluster 43 ...... 437

4.4.44. (a.-d.) Galaxy Cluster 44: Surface Density Statistics...... 439

4.4.44. (e.) Isothermal Fit for Galaxy Cluster 44...... 441

4.4.45. (a.-d.) Galaxy Cluster 45: Surface Density Statistics...... 443

4.4.45. (e.) Isothermal Fit for Galaxy Cluster 45 ...... 445

4.4.46. (a.-d.) Galaxy Cluster 46: Surface Density Statistics. . , ...... 447

4.4.46. (e.) Isothermal Fit for Galaxy Cluster 46 ...... 449

4.4.47. (a.-d.) Galaxy Cluster 47: Surface Density Statistics...... 451

4.4.47. (e.) Isothermal Fit for Galaxy Cluster 47...... 453

4.4.48. (a.-d.) Galaxy Cluster 48: Surface Density Statistics...... 455

4.4.48. (e.) Isothermal Fit for Galaxy Cluster 48 ...... 457

4.4.49. (a.-d.) Galaxy Cluster 49: Surface Density Statistics...... 459

4.4.49. (e.) Isothermal Fit for Galaxy Cluster 49 ...... 461

4.4.50. (a.-d.) Galaxy Cluster 50: Surface Density Statistics...... 463

4.4.50. (e.) Isothermal Fit for Galaxy Cluster 50...... 464

5.1.01. (a.-g.) Abell Cluster 0428: Morphology' and Distributions. ___ 469-470

XXX List of Illustrations

5.1.01. (b.-k.) Abell Cluster 0428: Surface Density Statistics ...... 472

5.1.01. (1.) Isothermal Fit for Abell Cluster 0428 ...... 474

5.1.02. (a..-g.) Abell Cluster 0514: Morpbology and Distributions 476-477

5.1.02. (b.-k.) Abell Cluster 0514: Surface Density Statistics ...... 480

5.1.02. (1.) Isothermal Fit for Abell Cluster 0514 ...... 482

5.1.03. Abell Cluster 0533: Morpbology and Distributions 484-485

5.1.03. (b.-k.) Abell Cluster 0533: Surface Density Statistics ...... 488

5.1.03. (1.) Isothermal Fit for Abell Cluster 0533 ...... 490

5.1.04. ^a.-gj Abell Cluster 1736: Morpbology and Distributions 492-493

5.1.04. (b.-k.) Abell Cluster 1736: Surface Density Statistics ...... 496

5.1.04. (1.) Isothermal Fit for Abell Cluster 1736 ...... 498

5.1.05. (s.-g.) Abell Cluster 2538: Morpbology and Distributions 500-501

5.1.05. (b.-k.) Abell Cluster 2538: Surface Density Statistics ...... 503

5.1.05. (1.) Isothermal Fit for Abell Cluster 2538 ...... 505

6.0.01. Galaxy Cluster Locations on the Celestial Sphere ...... 511

6.2.01. Core Population from Dispersion Ellipse Calculations ...... 514

6.2.02. Function for 55 Bright Southern Clusters of Galaxies. . 518

XXXI ABSTRACT

Here was very fine discourses — and experiments; but I do lack philosophy enough to understand them, and so cannot remember them. — Samuel Pepys Diary, 1 march 1666

This dissertation presents the description of 55 bright, close [z < 0.1) clusters of galaxies as a homogeneous sample taken from a new effort to catalogue galaxy clusters in the Southern Hemisphere. The positions of some 21,000 galaxies in clusters have been catalogued along with visual magnitudes, morphological types, position angles of extended objects and pertinent remarks. For all of the clusters, various cluster parameters have been determined and form the basis of comparative studies for these fundamental aggregates of matter in the universe.

The aims of this study are to produce a homogeneous sample of galaxy clusters measured to a uniform limiting magnitude of m„=19.0; catalogued with accurate positions relative to nearby astrometric standard ; morphologically classified and population typed; and statistically analysed in a uniform fashion to deduce certain cluster parameters. The cluster parameters of interest include an estimate of cluster distance, center and richness; galaxy distributions as a function of mor­ phological type, magnitude distribution and core radius. The core radius has been determined by fitting surface density information to an Isothermal Model by means of a minimization procedure.

xxxii PROBING THE LARGE-SCALE STRUCTURE OF THE UNIVERSE: AN ANALYSIS OF 55 BRIGHT SOUTHERN CLUSTERS OF GALAXIES

C H A P T E R I

THE DISCOVERY OF CLUSTERS OF GALAXIES

Nothing can astound the stars. They have long lived. And you are not the first To come to such a place seeking the most difficult knowledge. — Robert Penn Warren

The history of the studies of the physical properties of clusters of galaxies is short by the standards of many other astronomical topics, but it has been elaborated in the service of the history of astronomy with many interesting and varied lines of development-

In the great flurry of astronomical cataloguing during the eighteenth and nine­ teenth centuries astronomers not only busied themselves with the positions of stars, but also with the mysterious “nebulae” as well. In 1755 de la Caille published a cat­ alogue of 42 southern nebulae which was followed in 1781 by the famous catalogue of Charles Messier of 104 nebulae used by comet hunters to avoid spurious identi­ fications (Landmark (1927), Jones: (1968)). Thirty-three of the objects identified by Messier (1781) in his third and last catalogue are now recognized to be extra- galactic, but even at the time the catalogue was published, these objects served Discovery of Clusters of Galaxies 2 §1.0 to illustrate an unusual concentration of nebulae in the of and Virgo. In 1784 William Herschel (Herschel, 1784) published an even larger catalogue of stars and nebulae of which over a thousand are extra-galactic ob­ jects. He further confirmed the concentration of these objects in the region modern astronomers regard as the galactic poles (Herschel, 1785). Sir William Herschel’s catalogue was extended to the Southern Hemisphere by Sir John Herschel during his residence in the Cape Province in South Africa. Here he published his Gen­ eral Catalogue of Nebulae and Star Clusters in 1864 which contains 5079 entries (Herschel, 1864). The distribution of the nebulae found in this catalogue was in­ vestigated by Proctor (1869) who confirmed their striking avoidance of the and used this information to prove the connection of our galaxy with the neb­ ulae as independent stellar systems. Probable multiple clustering (Waters, 1873) and the appearance of “nebular spots” (von Humboldt, 1866) were noticed in these catalogues as well as being more clearly detectable in the later catalogues of Dreyer (1888,1895, 1908) by Waters (1894).

With the advent of astronomical photography, the structures of the spiral neb­ ulae were catalogued and studied in large numbers. A photographic catalogue was compiled by Isaac Roberts in 1885-1904 and later published by his wife in 1922 (see Lundmark (1927), p. 15). A similar catalogue was published by James Keeler in 1908 (Keeler (1908)). A whole-sky photographic survey was undertaken by Franklin-Adams at this time, obtaining 206 overlapping plates at a scale of approximately 30 arcmin/cm (Hardcastle (1914)).

Other distinct groupings located in the constellations Ursa Major, Virgo and Fornax were noticed in the distribution of nebulae found in the first widely used catalogue of galaxies compiled by Shapley and Ames (1932a,b) which listed a total of 1249 objects and claimed to be complete to the 13th magnitude. This important work gleaned its source material from several existing catalogues including the NGC Discovery of Clusters of Galaxies 3 §1.0

of Dreyer, the Path list (1914), the Reinmuth catalogues (1926,1928) and those of the Harvard Observatorj’, and was put to use in later with investigations by de Vaucouleurs (1953) and Humason, Mayall and Sandage (1956). Here, the most important work is the catalogue by Sandage and Tammann (1974a,b,c,d; 1975a,b) - the Revised Shapley-Ames Catalogue - and the resulting analysis by Sandage, Tammann and Yahil (1979).

It is now known that these concentrations can be treated as isolated entities, as nearby clusters of galaxies, their whole-sky distribution masked to some extent by obscuration by the plane of our Galaxy. It was in the early part of this century that astronomers paid them serious scrutiny within the larger context of the whole- sky distribution of the nebulae (Hinks, 1911). Lundmark (1927) compiled a list of 55 concentrations of galaxies from various sources as did Shapley (1933). Galaxy counts by Holmberg (1937, p.52) using the of galaxies as an indication of their distance and allowing for any dispersion in luminosity, indicated the existence of a local metagalactic cloud with a density of more than five times that of the surrounding background. But by 1934, only about twenty great clusters of galaxies were known within 40 million light-years (on the old distance scale) (Zwicky, 1938). Not so surprisingly, this caused Hubble (1934,1936) to comment that rich clusters of galaxies were “relatively rare.”

Subsequently, the rate of discovery of clusters of galaxies soon overtook the abilities of astronomers to study them in detail and it was Hubble himself who

declared that an estimated 1 % of all visible galaxies are members of rich clusters which are distributed on the average of one per 50 square degrees of the celestial sphere. Zwicky (1952) likened the cosmos as divided into cluster cells of a given volume; something similar to a bubble-raft of soap suds. At the time, Zwicky (1957a) estimated these cells to average 37.5/h M pc in diameter and 440,000/(h*) cubic Mpc in volume (h = Ro/lOO Am/aec/Mpc) with a cluster membership on the Discovery of Clusters of Galaxies 4 §1.0 order of two to four thousand galaxies.

The belief of many that the universe was homogeneous and smooth prompted astronomers to suggest that given a large enough volume of space, these irregulari­ ties would tend to average out, and the overall distribution of galaxies would tend towards randomness. But tests of this Cosmological Principle were impossible at that time since the volume of space sampled till then were actually quite limited.

With the appearance of extensive sky surveys, most notably those made by Shapley and colleagues (Shapley, 1933,1938,1947) and in particular the deep pho­ tographic plates of the Lick Observatory and the National Geographic Society- Palomar Observatory Sky Survey, there was recognized the truly vast numbers of clusters of galaxies. Shapley and, later, Shane and Wirtanen (1954), were inter­ ested in the distribution of galaxies at large. Shapley’s main point was the irregular distribution of the galaxies he surveyed. This conclusion was in contrast to the idea of Hubble who, at that time, considered clusters rare. As a result, we may consider Shapley a precursor to the modern studies of the large-scale structure of the universe.

The continued search for and the description of the properties of galaxies showed a general hierarchy of organization indicating a smooth transition between double galaxies, multiple galaxies, groups of galaxies and clusters of galaxies. In other words, there seemed to be clustering at all observable levels. Pioneering work on clustering was taken up by Zwicky at the California Institute of Technology using plates taken with various Schmidt telescopes. Not only did he discover new clusters such as Pisces (Zwicky (1937)) but also he reinvestigated those clusters already known (Cancer Zwicky (1950ab); Coma: Zwicky (1937a, 1951); Hydra: Zwicky (1941); Pegasus; Edson and Zwicky (1941); Perseus: Zwicky (I942cd)). He deduced that clusters, not galaxies, constituted the fundamental building blocks of Discover}’ of Clusters of Galaxies 5 §1.0 the universe.

Zwicky believed that clusters represented very large entities and that they were physically connected to each other and superposed onto a uniform background of galaxies. This concept, however, has recently been modified. Clusters of galaxies are in fact imbedded in large structures which characterize the distribution of visible matter in the universe (Chincarini and Martins, (1975); Chincarini, (1984)), and a background of galaxies is not observed (Vettolani, de Sousa and Chincarini (1985)). Further, large regions with a literal absence of galaxies, called voids, have now been observed between large structures or (Chincarini (1978); Vettolani et al. (1985)).

The conclusion that clustering is a fact urged the introduction of statistical methods to interpret the data being amassed from galaxy counts made from pho­ tographic plates (Neyman and Scott ,1952,1955; Neyman, Scott and Shane, 1953, 1954; Scott, Shane and Swanson, 1954). These investigations indicated that clusters of galaxies may be fundamental units of matter and are far more numerous than formerly thought. In a major survey, Abell (1958) compiled a catalogue of 2712 rich clusters of galaxies discovered on the National Geographic-Palomar Observa­ tory Sky Survey (POSS) and selected a homogeneous sample of 1682 clusters for statistical study.

In the catalogue, a cluster was defined operationally as an association of galax­ ies containing at least 50 members not more than two magnitudes fainter than the third brightest member. The so-defined cluster must be compact enough for the galaxies to be counted to within an arbitrary distance r from the center of the clus­ ter where r = 4.6 x 10®/cz mm on the plate which transplates into a linear distance of 1.5/h Mpc (h = JIo/100] at the scale of the POSS. The object of these efi’orts was to study the distribution of the clusters as a function of depth in space, the Discovery of Clusters of Galaxies 6 §1.0 isotropy of the distribution of clusters and the evidence available for second-order clustering, that is, for the existence of clusters of clusters of galaxies. We must stress that this is the most fundamental survey work to date on the clustering of galaxies because of its and completeness and homogeneity.

Extensions of these surveys and catalogues are continuing with lists of Southern clusters of galaxies made by Klemola (1969), Snow (1970), Sersic (1974), Rose (1976) and Braid and MacGillivray (1977). More recently, new cataloguing efforts to include a homogeneous sample of clusters of galaxies in the Southern hemisphere have begun. Before his untimely death in 1984, Abell had planned and organized a large Southern effort as an all-sky completion of his work carried out in the Northern hemisphere. The project (in progress) will be carried out by his successors (Abell et al. (1985)) and initially analysed for the distribution of rich clusters by Chincarini et al. (1985).

In general, the limit of most previous and current surveys has been z < 0.5, but various groups are now searching for clusters at z > 0.5. Deep surveys giving counts of galaxies have been undertaken by Kron and colleagues (Kron, et al. (1977)) as well as by Tyson and Jarvis (1980) and Gunn et al. (1985) in an effort to detect clusters at z > 0.4 — 0.5. This is the extreme limit of Abell’s effort which was essentially imposed by limitations of the Schmidt telescope.

These fundamental surveys and studies have been undertaken with the aim of understanding the distribution of galaxies as fundamental aggregates of matter in the universe. Current findings suggest that galaxies and clusters of galaxies are parts of very large structures. In addition, regions devoid of galaxies have been detected (Chincarini and Rood (1976); Gregory and Thompson (1978); Tarenghi et al. (1979); Kirshner et al. 1983)) as well as large irregular structures. Using this material, Peebles (1980) has developed the powerful statistical methods of Discovery of Clusters of Galaxies 7 §1.0 the autocorrelation function directed at understanding the distribution of matter in the universe at large and its implications, as well as opening the possibility of discriminating between various cosmological models.

The observed distribution of galaxies appears at this time to be very clumpy. These agglomerations define very large structures (Chincarini (1984)) of which no boundary has been found. These very irregular forms have density peaks which coincide with the observed clusters of galaxies, and such structures seem to be connected to each other and never seem to be isolated. This model was spawned on the basis of early observational evidence gathered by Chincarini and Rood (1978), motivated by the theories of Zel’dovich and colleagues (1978) and Einasto et al. (1978), in which it would appear unlikely to detect an isolated cluster of galaxies. Indeed, if positive density fluctuations form, as we see with clusters of galaxies, one can also expect negative density fluctuations where the density of galaxies is very low. And these regions have been observed. For instance, a particularly large has been detected by Kishner et al. (1981,1983) in the direction of the Bootes. The perhaps unexpected result of the observations (Chincarini, (1984)) is that no galaxy has been seen in such voids. What is less clear, as pointed out by Peebles (1983), is whether these voids have some physical significance or are a natural by-product of a hierarchical clustering of galaxies.

It is now seen that the distribution of galaxies in space is characterized in various surveys by clustering on a large scale, observed as superclusters or chains, and by voids, regions of space where galaxies have not been detected (Oort, (1983); Vettolani et al. (1984)). There is general agreement on the fact that a uniform background of galaxies upon which clusters and groups of galaxies are superposed as conceived by the pioneering efforts of Hubble and Zwicky does not exist. C H A P T E R II

DATA ACQUISITION AND PREPARATION

The explorations of space end on a note of uncertainty... tpe measure shadows... we search among the ghostly errors of measurement... - Edwin Hubble, 1935

The most recent collection of positions of clusters of galaxies is the data gleaned by Abell and Corwin (unpublished). This important body of information will be incorporated into a new Southern Galaxy Cluster Survey (Abell et al. (1986)) and will be consistent throughout with the Northern Survey of Abell (1957). It is from this preliminary data that we have acquired the cooordinates of the positions of 50 clusters of galaxies found in the Southern Hemisphere. These were chosen for their proximity {z < 0 .1 ) and their richness, with the intent to measure the clusters in a consistent fashion and produce a homogeneous sample.

We are interested in the extent of the clusters on the sky; the accurate positions and orientations of the cluster members; the morphological types of the galaxies in the clusters and their total mix and the brightness of each of the cluster galaxies

8 D ata Acquisition 9 §2.0 measured consistently to some limiting magnitude. The result of this effort is a ho­ mogeneous catalogue of data for 50 clusters of galaxies in the Southern Hemisphere. We have also chosen to measure 5 Abell clusters of galaxies located in the Equa­ torial Region to serve as a basis of comparison and provide a link of compatability with earlier work.

In the following sections we address the acquisition of the data and the prepa­ ration of the catalogue. We begin with the digitization of the position of galaxies in a selected cluster. Once accurate positions have been measured, estimates are made of position angle and individual morphological type as well as magnitude. The positions as measured conform to the standard astrometric conventions of East preceding, West following; and position angles adhere to the convention of angles being measured from the North, positive Eastwards. Similarly, magnitudes are measured as visual magnitudes, m„, by virtue of a step-scale calibrated against photoelectric magnitudes of Virgo Cluster and Indus galaxies as well as AT87 globular clusters. The morphological classification is based on the coding of revised morphological types by de Vaucouleurs and de Vaucouleurs (1964), but due to the small size of the images of cluster galaxies on the photographic plates, only a general classification of E, SO, SA, SB, or P are given. Relevant comments complete the entry, the comments being a coded visual appearance of the observed galaxies. With the completion of the measurements of a given cluster, the positional data recovered from the plates are transformed to celestial coordinates to assist in later observations of the cluster members.

From the final form of the catalogued data we obtain several important cluster parameters that are useful in comparing cluster information from other sources. Of the many schemes that we will describe, we select the Abell type and Abell richness classifications as well as the Bautz-Moryap. Classification as most compatible with and representative of earlier work. Data Acquisition 10 §2.1

t.l Measuring the Clusters

The data are contained on photographic film negative copies of the ESO/SERC Southern Sky Atlas. The 606 J plates were taken on the UK 1.2m Schmidt Telescope on Siding Spring Mountain, near Coonabarabran in New South Wales, Australia. The basic optical parameters of the telescope are very similar to the Palomar 48- inch Schmidt: aperture 1.24m, focal length 3.07m, giving a plate scale of 67.2 arcsec/mm, /-ratio of f/2.5, and a fuU field of 6.4® x 6.4®, with an unvingnetted field of 5.4® diameter. The J refers to the Eastman-Kodak type IHaJ emulsion used for the atlas survey; the plates were hypersensitised before exposure by a combination of nitrogen and hydrogen gas soaking techniques. All exposures were done through a 2mm-thick Schott (Jena) GG395 glass filter. The elective bandpass is thus from about 3950A to 5400A

Measurements of the positions of galaxies on the ESO/SERC J Plates were made using a Houston Instrument Series 7000 precision microprocessor-based Digi­ tizer for converting plate positions into Cartesian (X — P) digital data, which then inputs the data to a VAX 11/780 host computer for analysis. The digitizer employs a translucent active digitizing surface (including a 30mm wide perimeter set aside as a Menu area) which allows backlighting and provides uniform high resolution and accuracy over the entire Specification Area (see Figure 2.1.1).

The resolution setting was fixed at 0.025 mm (0.001”) with a maximum digi­ tization rate of one X - P coordinate point per second. A serial single coordinate record format was chosen for the data in which the X and P magnitudes are repre­ sented by seven characters in millimeter scale, plus a sign character, field delimiters and a tag character. The digitizer was set to automatically average eight consec­ utive strobe-scans per reading with the resultant Coordinate output to the host computer. This averaging yields coordinate values deviating none or only ±0.025 Data Acquisition 11 §2.1

-INOT ON 7012) ■INPUT DEVICE SOCKETS-

MENU AREA

-Active Area- (Window)

-Specification Area

■flENU "area " ÜC PAÆL FRAME

Figure 2.1.1 Schematic of X -Y Digitizer mm of each other if the data cursor is maintained in the same position. The input device is a 12 button cursor with crosshairs modified to include a 7X eyepiece and a second set of crosshairs to eliminate parallax during measurement.

During the measurement operation, a plate was secured to the digitizing surface within the Specification Area and the coordinates of the fiducial marks on the plate were digitized. These points were used to determine digitizer offsets, the skew correction angle, and finally the metric plate center as found by the intersection of the N — S, E — W fiducial marks. All measures were subsequently referred to this point with the convention chosen such that North and East are taken positive, that is, with the x-axis reversed in the Cartesian sense. Position angles follow a similar convention with angles being measured positive East of North, with the North point (as measured from the intersection of the N — S fiducial marks) as the origin.

The actual measurement of a galaxy position consisted of laying the cursor over the geometric center of the image, digitizing the point, and optionally measuring the major and minor axes of the image under program control. The errors found D ata Acquisition 12 §2.1 in determining the geometric center of the image have been estimated by repeat­ edly measuring the same point on differing occasions and combining the results to assess our ability to recover a given object from a given field. We find that the measurements are repeatable in this fashion to erx,j; = 0.286 mm or approximately 19.4 arcseconds for the worst case on the ESO/SERC fields. This virtually excludes misidentifications of galaxies in the field, in particular if morphological information is available.

For extended objects, the procedure was generally to measure along the as­ sumed major and minor axes of the object until the image faded into the background density. A word of caution, however, is that although the major axis measurements are repeatable to within = 0.06 mm, the minor axis measurement fiuctuates as a result of the inability to bisect the major axis readily. Similarly, the construction of position angles is such that the poles of the major axis are projected to intersect the line connecting the N — S fiducial marks with a = 6.08 degrees. In general, major and minor axes and position angles were not measured for objects whose diameter was less than 0 . 1 mm or did not display an obvious ellipticity.

The preliminary cluster center was taken from Corwin’s (1985) unpublished data and each cluster was located on finding charts prepared both by the author and the RGO. The cluster counting area was determined by using the criteria set down by Abell (1956) the radius being a function of mio- The counts themselves were done in the defined circle which was divided into eight segments and masked so that only a sector at a time was available for measurement. The circle is shown in Figure 2.1.2. This was done to facilitate and standardize the measurement process.

During measurement, the cursor was positioned over the central portion of the image, the coordinates of the center of the galaxy image digitized, the major Data Acquisition 13 §2.1

Figure 2.1.2 Circle counting mask divided into Abell-radii and sectors. and minor axes digitized when desired. A step scale estimate was made using a lOX loup and entered as input data, an estimate of morphological type made and entered, and finally, any remarks concerning the object entered. An on-line reduction program then converted these inputs from digitizer units to distances and angles measured from the geometric plate center under the above conventions. Similarly, the step-scale estimate was converted to a magnitude measure by virtue of an interpolation routine using the step scale calibration curve described later. All of this data provides the raw material for later reduction and construction of the cluster catalogue. Data Acquisition 14 §2.2

8.2 The Step-Scale Calibrations

At the moment the writer and Dr. H. Corwin are curently engaged in extend­ ing the rich galaxy cluster survey (Abell, 1957) to the south celestial pole using the ESO/SERC Hla-J plates. As in the 1957 work, the magnitude of the cluster members is estimated with a step-scale of galaxy images. A typical set of step-scales for various morphological types of galaxies is shown in Figure 2.2.1

PIRAL GALAXY STEP-SCALE

bPIRAL GALAXY STEP-SCALE

ELLIPTICAL GALAXY STEP-SCALE

Figure 2.2.1 Typical Step-Scaleg for Magnitude Determination

Step-scales of this type are produced by locating photoelectrically or otherwise calibrated galaxy images on a film copy of a galaxy cluster field. The galaxy images D ata Acquisition 15 §2.2 are then excised from the film and mounted in a sequential array of increasing magnitude. This template is then compared to images on program plates and the magnitudes estimated by direct comparison.

The step scale used in this work is entirely composed of images. A calibration curve for this step scale was generated by estimating step readings to one tenth of a step for galaxies in the central thirty-six square degrees of the Virgo Cluster as seen on UK Schmidt plate J2137. Many galaxies to my ~ 14.0 in this field have well determined total magnitudes listed by de Vaucouleurs and Head (1978). These are in the system of RC2, but with the addition of data from other sources and with a small systematic error depending on inclination removed (see de Vaucouleurs and Corwin, 1977 and de Vaucouleurs et al., 1977).

In the poorly observed range 14.0 < m j < 17.0, a large portion of the photo­ electric calibrating data come from Corwin (1980). The data for the 19 Indus area galaxies plus one galaxy in A2670 act as secondary standards in this range.

The calibration at fainter levels rests on photoelectric observations of three galaxies in the galaxy cluster A1553 by Sandage (1972), and on photoelectrically calibrated photographic photometry of galaxies, stars and globular clusters around M87 by Hanes (1975,1977). Hanes’ work verifies earlier photographic photometry of objects around M87 by Racine(1968) and Abies et al. (1974).

The mean errors in the calibrating data at all magnitude levels are better than

Cb .v ~ ±0.15. However, systematic errors in estimating step-scale readings de­ pend on surface brightness. Low surface brightness galaxies are generally estimated too faint because ” integration” by eye of the light in the object’s image is difficult (this is the primary reason for surface brightness errors in the survey photometry of Shapley and Ames 1932 and in the CGCG. See Holmberg (1958), de Vaulcouleurs Data Acquisition 16 §2.2

(1957), de Vaucouleurs and Pence (1979), and Corwin (1979) for details.) Similarly, compact high surface brightness objects have their magnitudes underestimated be­ cause their light is concentrated in overexposed star-like "dots” and the eye has only the diameter of these objects to use as a clue to luminosity.

In both cases - high and low surface brightness - the luminosity profile of the unknown object generally does not match that of the elliptical galaxies on the step scale. At faint levels, the effects cannot yet be quantified with any certainty because of a lack of precise photometry for comparison. However, preliminary indications of order-of-magnitude reliability come from the studies of Pickup (1979) and Hawkins (1981). These seem to indicate that systematic errors are indeed present, but that they do not exceed ±0.5 magnitudes. Another indication of systematic error is related to magnitude determinations of difi'erent morphological types, but for the moment the reliability of the step scale is taken as being able to provide total magnitudes of about ±0.5 magnitude accuracy.

The step scale calibration curve is shown in Figure 2 . 2 . 2 .

Prime calibrators are photoelectrically {step < 12) or photographically {step > 12) observed galaxies in the Virgo Cluster area; secondary calibrators are photoelec­ trically observed galaxies in the Indus area; in addition there is a photoelectrically observed galaxy in A2670, and photo graphically observed globular clusters and stars around M87. The step scale has been calibrated using both originals and film copies of the ESO/SERC J plates. We then calibrate our measurements against those made by Abell and Corwin by remeasuring those same galaxies, recording the appropriate step-scale readings and comparing the two. The results are in quite good agreement and once more suggest the ±0.5 magnitude accuracy. An indepen­ dent source of comparison comes from our measurements ofm i,m s and mio which do not deviate by more than a few tenths of calculated magnitudes from estimates Data Acquisition 17 §2.2 STEP-SCALE CALIBRATION

0 2 4 6 e 10 12 14 15 ST£P-SCfl;.E NUMBER Figure 2.2.2 Siep-scate Calibration Curve made by Corwin.

It had been suspected (Corwin, 1985) th at because of difFerences in background density between originals [D ~ 1.0) and copies {D ~ 0.35) of the ESO/SERC J plates there would be a small zero point difference in the sense that magnitudes will be estimated brighter on the copies, but no such difference was found in the actual numbers. On the J plates the calibration is made using visual magnitudes, on the assumption that all galaxies have the same color index, that is, the step scale is calibrated for zero velocity E galaxies of intrinsic color B — V ~ 0.9. This means that K-reddening between J and V plates introduces a scale error in magnitude. The counts of galaxies in a particular cluster are unaffected since one can define a counting interval, say m„(3) 4-2, and all galaxies in a given cluster having the same z will have the same K-correction. However, background counts will be affected. D ata Acquisition 18 §2.3

3.3 Coordinate Transformation of Measurements

Once a given plate has been measured, the resulting rectangular plate coordi­ nates must be transformed to the celestial sphere in order to provide positions of objects for telescopic observations. These positions form an important subgroup of data in the cluster catalogue and constitute the main spacial representation of the projected surface density of clusters of galaxies.

Since the earliest days of astronomy stellar positions have been determined by measuring absolute right ascensions and . This fundamental approach to spherical has been extended to fainter stars and galaxies by mea­ suring their positions on photograpic plates with respect to a set of standard stars such as those found in the Smithsonian Astrophysical Observatory Star Catalog which gives the positions and proper motions of a large number of stars for the and equinox of 1950.0. Measurements on wide-angle photographs such as the ESO/SERC J plates yield plane coordinates, which are then reduced to spher­ ical (equatorial) coordinates in accordance with the SAO positions. The procedure requires our ability to project a portion of the celestial sphere onto a plane and re­ late the resulting ideal standard coordinates to the measured standard coordinates. The underlying projective geometry assumes that the telescope is equivalent to a pinhole camera for which the gnomic projection is appropriate. The ideal standard coordinates (, q comprise a rectangular coordinate system on the photographic plate which is assumed to be planar. For Schmidt plate astrometry this assumption breaks down and one must introduce the effects of plate curvature in the analysis, but over small enough regions it is thought that the gnomic projection is adequate (Eichorn, 1985). The measured standard coordinates x, y are approximations to the ideal coordinates. Our first task is to relate the ideal standard coordinates to the corresponding equatorial coordinates. Data Acquisition 19 §2.3

We are primarily concerned with the portrayal of a portion of the celestial sphere on an image plane registered by a photographic plate, so we consider the relationships between spherical coordinates and the corresponding coordinates on a plane tangent to the sphere. The plane tangential coordinate system is defined as lying in the plane tangent to the celestial sphere, the tangent point T being the origin of the coordinates, with right ascension oq and Sq as seen in Figure 2.3.1.

Figure 2.3.1. Plane coordinates. Cross section of the celestial sphere and the tangential plane. T = tangential point; S = central projection of star S q onto the plane tangent to the celestial sphere.

The y — axis is tangent to the hour circle through T, and its positive direction is the direction in which the distance of T to the celestial pole is < 180®. The z — axis is perpendicular to the y — axis, and is counted positive in the direction of increasing right ascension as shown in Figure 2.3.2 Data. Acquisition 2 0 §2.3 Dec S

RA

Figure 2.3.2. Tangential or ftandard coordinate Bystem, as seen from inside of the celestial sphere. As opposed to the usual Cartesian convention, the direction o f increasing R A (i.e., -x) is considered positive.

A point So on the celestial sphere, or its image on a photographic plate, corre­ sponds, therefore, to the plane rectangular coordinates X and F of a point 5, that point being the central projection of So on the tangential plane or on its image, the photographic plate, which is assumed to be parallel to the tangential plane. The linear distance

c — tan p. (2.3.1)

It follows that the rectangular components are related to the equatorial coordinates l>y r = tanpsind, (2.3.2)

y = tan p cos 6 (2.3.3) where 6 is the position angle of the segment p (or

In our case, a maximum of 25 SAO stars were identified in a field 2 x 2 degrees and their locations digitized. Positions of these standard stars in X and Y Cartesian coordinates were calculated with reference to the published nominal plate center and the measured geometric center correcting these positions by allowing for to the epoch of the plate. Then the X and Y positions as measured by the digitizer were fitted to these positions by least squares and the resulting Right D ata Acquisition 21 §2.3

Ascensions and Declinations of these same stars calculated from the fit. While the above procedure can give some estimate of the errors of measurement it should also be emphasized that the images of the SA O stars are so large, some 400 to 600 microns in diameter, and often show considerable diffraction ”spikes” and "rings” and sometimes even a blaze, that the determination of the coordinates of the center of the image is very much less accurate than that for the smaller star images in the

1 0 0 micron range.

The positions of the SAO standard stars were then transformed into a plate- centered zenith-azimuth system, p and 6 :

cos p = cos So cos St cos(a* — Oq ) + sin sin (2.3.4)

^i^^^cosg.sm(a.-ao) (2.3.5) amp

(2.3.6) COS Oo s m p

where and ao. So are, respectively, the right ascension and declination of the star and the nominal plate center and p is expressed in degrees and decimal fractions of a degree.

We next scale and translate the corresponding measured plate coordinates of the SAO stars by X = F{xm-xo), Y = F(ym-yo)- (2.3.7)

Here F is the plate scale - 67.2 arcseconds per millimeter - expressed in degrees and Xm and y ^ are the measured coordinates of the standard stars. Data Acquisition 22 §2.3

Now if:

a.) the plate centers (ao,5o) and (ïoi Î/o ) coincided exactly;

b.) the plate ordinate as defined by the digitizer ran exactly North-South;

c.) the scale factor were exact;

d.) and the plate relaxed precisely along radial lines with no stretch as it was released from the telescope plate holder,

then, if ( = tan p sin d and tj = tan p cos 0 are the measured coordinates on the plate, ( = g(X, Y), and r/ = h(X , Y) would be identically the same as X and Y.

However, this is not usually the case, so we fit by least squares:

e = g{X, Y ) = A o + A iX + A 2 Y-i- A ^X ^ + A ^ X Y ^ (2.3.8)

q = h{X, y) = Bo + B iX + B 2 Y + BiXY^ + B^Y^ (2.3.9)

where A q and Bo represent the celestial:pbysical plate center translation alignment, A i and primarily represent scale factor corrections, Aa and B% primarily rep­

resent ordinate:Nortb-Soutb rotation alignment; and A 3 — B 4 represent corrections for elastic distortions introduced between the Schmidt plate holder and the relaxed planar plate. An estimate of the quality of the reduction can be seen in Figure 2.3.3 which shows the dispersion of the standard stars used to determine the posi­ tion of cluster members. Here we have plotted the O — G residuals of the standard stars along the East-West absissa and the North-South ordinate. We note that tTx = 0.24mm and Cy = 0.29mm which gives rise to a distribution somewhat elon­ gated along the North-South direction. We attribute this to internal bias in the digitizer. D ata Acquisition 23 §2.3 STANDARD STAR RESIDUALS 0-C 1.00

0 . 6 0

0 . 5 0

MK •L* 0.20

0.00

0.20

0 . 4 0

•0.50

- 0 . 8 0

- 3 . 0 0 CD O o o o CDCD O CD CD CD 00 CO f \ l o (NJ CD CD CD ^ CD O CD ~ I I I Figure 2.8.3 0-C Diagram for Standard Star Reductions.

The plate constants Ai and B,-, so determined, were used to obtain the co­ ordinates of the galaxies from their measured positions and constitute the major positional information in the cluster catalogue. The transformation from standard to equatorial coordinates for the measured objects is straightforward.

We apply the sine, cosine and extended cosine rules to the spherical triangle GTP, formed by a galaxy’s position G, the tangent point T, and the North Celestial Pole, P as in Figure 2.3.4 This gives us several important relationships between the measured and known positions on the plate. Data Acquisition 24 §2.3

Thus we have;

cos p = sin Sff sin So + cos 6g cos Sq cos A a (2.3.10)

BinpsinG = cos 6g sin A a (2.3.11)

sin p cos 6 = sin cos — cosSg sin So cos A a (2.3.12) where A a = Qg — tto, Af = fg — So.

Ao

G

T

F ig u re 2.SA.Spherieal Triangle GTP formed by the galaxy G, tangential point T, and North Pole P.

The above equations are identical to (2.3.4), (2.3.5) and (2.3.6). Now, if we set the measured position of a galaxy to be

Xg = tan p sin 0 (2.3.13)

Pg = tan p cos 6 (2.3.14) Data Acquisition 25 §2.3 and divide (2.3.11) and (2.3.12) by (2.3.10), respectively, and substituting in (2.3.13) and (2.3.14) we obtain

------( 2 .3 .1 5 ) s in 0 s m Ô0 + c o s 5 c o s Oq c o s A a and sin 5 cos 5o ~ cos 5 sin ^ 0 cos A a % = : J-----r ------(2.3.16) sin 0 sin Oo + cos 0 cos Oo cos Aa

We can now express Aa and 6g for a measured galaxy in terms of the measured positions Xg and jjg and the celestial coordinates of the nominal plate center (ao, ^o).

Equation ( 2 .3 .1 6 ) can be written

yg (sin Sg sin So + cos 5g cos S q c o s A a) = sin 5g cos S q — cos Sg sin S q cos A a o r

s in Sg(cosSo - yg s in 5o ) = cos6g{yg cos^o + sin 5o) cos A a, from which we find . c I fsin fisn ^o -i-+ «Jî/oCOs5q' I tân Oÿ — I , c o s A a. (2 .3 .1 7 ) [cos So - t/g sm So,

The quantity Aa may be found by writing ( 2 .3 .1 5 ) as

sin A a = (sin Sg sin + cos Sg cos So cos A a)

= Xg{iasiSg sin^o + c o s 5q co s A a).

Since from ( 2 .3 .1 7 ) we have

(2.3.18) |_sinoo + yg cos Sol we can write , c . r c ^ cosfo - % sin go] sin A a = Xg [tan Sn sin do + tan Sg cos do -i—: ------t" " " smdo + î/y cosdoj

- r sin^ do + Vo sin do cos do + cos* do - yg sin do cos do — Xg t& D S g I : % J- ^ BUlSo + ygCOsSo Data Acquisition 26 §2.3 from which sin Aa = . . (2.3.19) sm So + Vg cos So Also, by dividing (2.3.19) by (2.3.18), we finally obtain:

tan A a = ----- . (2.3.20) cosSo - VgSmSo

The catalogued positions of both cluster centers and positions of galaxies are determined by applying the plate constants A,- and Bi to the measured galaxy positions and substituting the resulting quantities in equations (2.3.17) and (2.3.20). This yields the equatorial coordinates and Sg which are reduced to the epoch 1950. We assume the errors in position are similar to those of the standard star positions.

It is also of interest to transform the equatorial coordinates of the cluster centers to new galactic coordinates. This is useful to give estimates of galactic extinction which effects the determination of mio and hence, the cluster .

The conversion formulae to galactic latitude, 6 , and galactic longitude, I, are given by:

b = sin” ^ {cos Sg cos Sq cos(a^ — og) + sin Sg sin gg}, (2.3.21) and

( cos Sg sin(ag - ag) cos Sg J where the epoch 1950 coordinates of the North Galactic Pole are given by a g = 192® 15' and Sa = +27® 24' with the ascending node of the on the equator as Ig = 33®. Data Acquisition 27 §2.4

2.4 Determination of Cluster Centers

Once we obtain a set of coordinate values for the position of galaxies in a cluster, an important parameter to be derived is the center of the cluster. We have determined the center of each cluster by various means. Here we accept the fact that we are merely displaying our ignorance of just what constitutes a cluster and our inability to determine other than operationally the nature of such an ensemble of objects. Up to this point the term cluster has been used in an intuitive sense without attempting any formal definition, such as a group of contiguous elements in a statistical population.

A discription of what constitutes a cluster which probably agrees with our intuitive understanding of the term is given by considering our galaxies as points in Euclidean space. Clusters may now be described as continuous regions of this space containing a relatively high density of points, separated from other such regions by regions contmning a relatively low density of points. Care must be taken, however, not to restrict the definition. For example, there is no a priori reason for believing that any clusters present in the data are of one particular shape and we must guard against imposing a particular structure on the data, rather than finding the actual structure present.

So to determine the center of a clusters depends on just what we think a cluster is. In the case of clusters of galaxies, the notion of cluster center at its simplest refers to the geometric centre of a bivariate distribution of points projected onto the plane; the notion can be further compounded by the realization that in actuality we are dealing with a multivariate population of objects of different morphological classes or sub-populations, effected by selection and possible mass segregations. For the sake of simplicity' and homogeneity, we choose a geometric approach. Data Acquisition 28 §2.4

Initially, a center was constructed by considering the cluster members as merely points projected to a plane tangent to the celestial sphere and whose positions and coordinates were accurately known. Then the standard bivariate analysis of their positions performed to yield the geometric center of the population, and a bivariate ellipse within which a known fraction of the population resides.

The analysis proceeds as follows: we assume that the positions of galaxies in a cluster pven by their measured coordinates (z»,*/») are a random sample from a bivariate population. We can say that the two quantities, r and j/ are jointly distribated since, in general, x and y depend on each other. However, we also assume that different pairs and (zy, are independent of each other.

We concentrate on the data reduction by means of purely descriptive statistical tools. Whereas the mean, x, and the standard deviation, usually suffice to represent a univariate sample, our case demands five statistics, two means, two standard deviations, and a correlation coefficient. It is not only important to what extent the member galaxies are dispersed in a cluster, but also to see how their positional scatter is oriented on the plane tangent to the celestial sphere. These requirements can be satisfied graphically by the so-called dispersion ellipse.

After amassing the coordinates of the position of cluster members, we calculate the arithmetic means

(2.4.2) and define the variances Data Acquisition 29 §2.4

- e f (2.4.4) so that by taking the square root of these, we define the standard deviations, Oi and

We also construct the familiar measures of the joint behavior of x and y, the covariance Cov[x, y) = %](zi - ï)(y, - s) (2.4.5) and the cor reaction coefficient

r = ooTrx.y= ^^ai^ (2.4,6)

provided that Oi and 0 2 do not vanish.

From these quantities we construct a dispersion ellipse such that

1 (z - _ „^(g-g)(y-p) (y-g) = 1 (2.4.7) 1 - r* [ <7-i

f 2 (z - - 2 ro-i(r 2 {x - i){y - g) +o"i^(y-g)^ = (l - r*)o’i^o’2 ^

We can rewrite this equation in the quadratic form

A{x - i f + 2B{x - x){y - g) + C{y - ÿ f = D (2.4.8)

where the coefficients are given by

A = (rl, B = —TOitTz = —Cov{z, y]

C = (Ti, D = {l-r'^)a\(T\. Data Acquisition 30 §2.4

Given the above quadratic form where we assume that D > 0 we let

f f = A C - B^.

Then the graph of our quadratic equation is an ellipse if, and only if, all three inequalities A >0, G>0, H > 0 hold. The midpoint of the ellipse is then located at î, ÿ.

Two special cases can be treated separately:

(1) A = C7,B = 0. The ellipse is a circle with radius r = (D/a)a.

(2) A > = 0. The major axis is parallel to the Y axis. The semi-axes are a = (D/C)3 and b — [DJA)^.

Excluding these special cases, we calculate the following quantities for each cluster: R = [{A-CŸ

2B G = arctan A — C — R

Here, a and b are the semi-axes (a > 6 ), and 0 is the angle by which the major axis is inclined with respect to the X axis with (—90° < 0 < 90°).

For the plots of Cluster Membership and Morphology, we have used the para­ metric form of the ellipse to plot several important contour lines:

a: = 3c-I-a cos 0 cos ^ — 6 sin 0 sin 4P (2.4.10) Data Acquisition 31 §2.4

1 /= Ç + osin0cosÿ5 + 6cos6sin4 5 (2.4.11) with p a variable angle increasing from 0 to

It is of some interest to inquire what fraction of the cluster population de­ termined by their positions z,, y, fall inside of the dispersion ellipse. We have designated these as the core population. Following Trumpler and Weaver (1953) we note that if /ix is the expectation and a i the standard deviation of the random positional variable, X, then the probability density is given by:

fi(x) = (2ir)~^f^

Correspondingly, if is the expectation and the standard deviation of the random positional variable Y, the probability density is

/2(y) = {2n)~^^'^(T2^exp [ - ( y - ^2 ^ ■ (2.4.13)

If we assume that x and y are independent of each other we can multiply fi{x) and

/ 2 (y) hi order to obtain the probability of the joint distribution:

/ ( z , y) = fi{x) • / 2 (y) = (2;r

Here, the auxiliary function g{x, y) is

= , 2 .,.15) a l

To study the density function f{x, y) we consider the contour lines or isolines with equations f{x,y) = constant.

Since the variables x and y only occur in g{x,y), it suffices to study the lines g(x, y) = COT + = (2.4.ie) D ata Acquisition 32 §2.4 where each isollne is associated with a particular constant e.

A comparison of equation (2.4.16) with

= (2.4.17)

reveals that the isoline represents an ellipse with its center at the point (pi, P2 ) and with semi-axes a = c^CTx,b = caffj.

In general, o : 6 =

Hence, given

Now the area of an ellipse defined by the above parameters is ro-jo-gc^. The element of area dA corresponding to the change of c from c — d | to c -h d | is

2 Ta‘iO’2 cdc the frequency along such an infinitesimal ring is constant and equals 1 2ff

The fraction of the population du contained within the ring is thus ce % do and the fraction u of the galaxy population contained within the dispersion ellipse is therefore 1 - e-2 = 0.39347. (2.4.18) - j : a The dispersion ellipse thus encloses some 39 percent of the total galaxy population and can be used to estimate cluster density and richness. Data Acquisition 33 §2.4

r

Figure 2.4.1 Itolinet representing a bivariate normal distribution of independent random variables. The shaded ellipse is the dispersion ellipse with standard devia­

tions, Cl and 0 2 , as semi-axes.

To serve a a check on the center determined by bivariate methods, the galaxy positions were also analysed using the traditional strip counting method. Here we have determined the center of each cluster by performing galaxy strip counts as a function of distance for mutually orthogonal directions on the plate as is shown in Figure 2.4.2. The orientation was chosen to coincide with the axes on the ESO/SERC plates determined by the intersection of lines drawn by connecting opposite fiducial marks on the plate edges. The initial width of the strips was chosen to be one arcminute on the plate, but this was varied somewhat from cluster to cluster depending mainly on distance (that is, from the apparent size of the cluster as determined by mio) and the projected density. The range of the strip width was from about 0.5’ for z < 0.1 to about 5.0’ for z ~ 0.02. The length of the strips was determined individually for each cluster and was found by constructing that rectangle whose extent completely enclosed the counting circle. Recall that the counting diameter corresponds to that determined by Abell (1958). Data AcquisitioD 34 §2.4

CflLRXY CLUSTER 50 23 58 48 -44 12 GfiLBXY CLUSTER 50 23 58 43 -44 12

NZRTH-SBUTH s t r ip C 2U M S______WEST-EAST STRIP ceuMS

I l i S i l f '

f.*. m m I « ■ » • » *■»

"''I:,!"''!'']'!"

Figure 2.4.2 N-S and E-W Strip Gounte for Galaxy Clusters.

All galaxies were counted down to a limiting magnitude of 19.0 even though some clusters had fainter members. The strip densities were then plotted as his­ tograms as a function of distance in the different directions and a normal probability' curve drawn for the each distibution. The center of the cluster was determined for each direction from the high density peak in the histogram and the correspond­ ing peak in the normal distribution. In the more irregular clusters, or those with density concentrations, the most highly concentrated and symmetrical peak served to locate the center of the cluster. The positions of the center determined in this way was then converted to the 1950 epoch coordinates relative to the astrometric standard SAO stars and plate constants calculated for each cluster region. D ata Acquisition 35 §2.5

2.5 The Classification of Galaxy Clusters

Having measured the cluster members within an Abell radius we attempt to discover a basis for comparisons from cluster to cluster. Over the years numerous classification schemes for clusters of galaxies have been designed and continue to be developed based on the morphological, physical and optical properties of the cluster members. As Hubble (1936) remarked: “In a certain sense each cluster may be characterized by a most frequent type, although the dispersion around that type is considerable. ”

To categorize clusters in his catalogue, Abell (1957) sorted his rich clusters in groups of increasing population. He defines the richness, R, of a cluster as the number of galaxies intermediate in brightness between the third brightest galaxy in the cluster and two magnitudes fainter counted within a projected radius r from the apparent cluster center. This distance, known as the A b ell radius, is an oper­ ationally defined boundary scaled inversely as the mean cluster recession velocity and therefor subtends an approximately constant metric length at the distance of the cluster. For the Palomar Sky Survey plates with a scale of 67^.2 we have r = 4.6 X 10*/cdA/A mm and in terms of the galaxies counted within r, the richness subdivisions are shown in Table 2.5.1

ABELL RICHNESS GR0UP INTERVALS

RICHNESS C0UNTS RICHNESS C0UNTS RICHNESS C0LINTS

GR0UP GR0UP GR0UP 0...... 30-49 2 ...... 80-129 4 ...... 200-299 1 50-79 3 130-199 5 ...... 300

Table 2.5.1 Abell Richness subdivisions for galazy clusters. Data Acquisition 36 §2.5

Abell’s richness estimates are still widely used to complement other cluster descriptions which do not incorporate such a population parameter.

Zwicky et al. (1961-1968) provide the other main source of data on clustering and use the criterion of classifîying galaxy clusters according to the distribution of their bright members. The classification scheme proceeds as follows:

Com pact clusters show a single outstanding concentration among the bright member galaxies. Within this concentration, ten or more galaxies appear in actual contact. Many of these clusters display a high degree of spherical symmetry.

M edium -Com pact clusters are characterized by either a single concentration where, however, the ten brightest galaxies are not in contact but are separated by several of their own diameters, or by several distinct condensations, some of which may be quite compact.

O pen clusters contain no very obvious condensations, but in various locations, the number of galaxies per square degree is at least five times as great as in the surrounding field, so that the cluster appears to be as a cloud superposed on the background.

Hubble’s early ideas were enhanced by de Vaucouleurs (1961) who recognized three distinct classes of galaxy clusters, each divided by size and form: clusters of spiral and irregular galaxies, comprised of small, low-density groups and large elliptical clouds of diameter 2 — 3 Mpc; clusters of mainly elliptical and lenticular galaxies, either small and dense or large and globular; and clouds of mixed types, including large elliptical clouds or cloud complexes like the multiple , and vast supersystems, the latter exemplified by the Local Supercluster. Data Acquisition 37 §2.5

After examining the 20 nearest clusters in Abell’s (1957) catalogue, Morgan (1961, 1962) suggested that the Coma and Virgo (and Ursa Major) clusters could be considered as prototypes for a cluster morphology that paralleled that of open star clusters in the Galaxy. In Virgo-type clusters, appreciable numbers of galaxies of low central light concentration (in eflFect, spirals and irregulars) appear 1/2”* to 1”* fainter than the brightest members, whereas Coma-type clusters are popu­ lated in the range of the brightest two magnitudes exclusively by galaxies of high light concentration. Incidental mention was afforded Ursa Major-type clouds which represent ill-defined physical groups of exceedingly low volume density.

The de Vaucouleures and Morgan systems, based as they are on the morphol­ ogy of the brighter galaxies of a cluster, suffer from the disadvantage that only the nearby clusters of galaxies can be so classified. However on a first order approach, there are marked correlations between these systems and the system of Zwicky. Their main features are preserved in the two-part classification scheme of Abell (1965, 1966);

R egular clusters show strong central concentration and tend to be spherically symétrie. All are rich, containing > 10* galaxies in the range of the brightest seven magnitudes, the first S'" — 4'" of which are populated entirely or almost entirely by E and SO galaxies. One or two giant elliptical galaxies are often centrally located, and there is no strong evidence of subclustering. Most of Zwicky’s compact clusters and Morgan’s si Coma-type clusters are regular; examples are the [Abell 1656) and the cluster ().

Irregular clusters exhibit little or no spherical symmetry and no marked cen­ tral condensation; often multiple nuclei exist indicating some substructuring. Clus­ ter populations vary widely and galaxies of all types are normally present, although poor groups may not contain giant elliptical galaxies. To this classification belong Data Acquisition 38 §2.5

M organ’s Virgo-type clusters and Zwicky’s Medium compact and Open clusters. Examples are the Local and MSI groups, the Virgo cluster, and Abell 2151, the Hercules cluster.

The particular advantage of Abell’s classification is that it can be applied to clusters over a great range of distances.

A five-part classification scheme depending on the relative optical contrast of the brightest galaxy in a cluster to other cluster members was devised by Bautz and Morgan (1970). To the initial list of types for 76 rich clusters were added the classification for a further 111 by Bautz (1972). Their scheme is shown in Table 2 . 5 . 2 . ______BAUTZ-M0RGAN CLRS5IFICATI0N SYSTEM

TYPE ! THE aUSTER JS DBMINfiTED BY A SINGEE. CENTRALLY LBGATED, CD GA.AXY.

TYPE II THE BRIGHTEST MEMBERS ARE INTERMEDIATE IN APPEARANCE BETWEEN CO

GALAXIES (WHICH HAVE EXTENDED ENVEL0PES) AND NORMAL GIANT l ELIPTICA.S

TYPE III THE CLUSTER C0NTAINS N0 DOMINANT GALAXIES

AND TH0 INTERMEDIATE TYPES. TYPE I- II AND TYPE II- III.

Table 3.5.2 The Bautz-Morgan Classification.

There are three main diflBculties encountered with the practical use of Bautz and Morgan’s brightest galaxy morphology (van den Bergh, 1977). Initially, the classification scheme is extremely vulnerable— to contamination by foreground field galaxies; for example, missassigning cluster membership to a forground galaxy can change a cluster’s classification from HI to I. Conversely, a dominant cD galaxy in a distant cluster might be regarded as a member of a sparse clustering of brighter foreground objects. Secondly, the K-dimming effect will reduce the surface bright­ ness of the faint outer envelopes of distance cD galaxies and hence systematically reduce the contrast between the cD and normal giant elliptical galaxies in the clus­ Data Acquisition 39 §2.5

ter. Finally, clusters in which three or more bright galaxies obviously dominate the remaining members do not fit naturally into the Bautz-Morgan classification system.

Rood and Sastry (1971) introduced a scheme strongly reminiscent of Hubble’s early aingle-galaxy classification system which is based on the distribution of the ten brightest cluster members:

cD (super giant): These clusters contain an outstandingly bright member, a cD galaxy. As an operational definition, the size of the cD galaxy (i.e. semimajor axis plus semiminor axis) is > 3 times that of any other member. If the main body is multiple or shows any peculiarity, a subscript p is added to the type designation. Prototypical examples include Abell 0401 (cD) and (cDp).

B(binary): Here, two supergiant galaxies are separated by < 10 diameters of the larger galaxy, with combined size > 3 times that of any other cluster member. A subscript b indicates a connecting bridge between the subergiant binary or the components of one or both of its members. Examples include Abell 1656 (b) and AbeU 0154 (Bb).

L(line): In this case, > 3 brightest galaxies among the top ten members are arreanged with comparable separations in a line, with numerous fainter members distibuted around them. A typical example includes Abell 0426 (L).

C(coTe-balo): Here, > 4 of the ten brightest members are located near the center of the cluster with comparable separations as well as being surrounded by fainter galaxies. An example is Abell 2065 (G).

F (Bat): In this case, several of the ten brightest members and a large fraction Data Acquisition 40 §2.5 of the fainter galaxies are distributed in a flattened conflguration, for example, as in Abell 0297 (F).

l(iiT€gvlar): In this last description, the galaxies in the cluster are distributed irregularly and the center is not well-defined. Examples include Abell 0400 (I) and AbeU 2151 (L).

The classification system can be represented by a tuning fork diagram as shown in Table 2.5.3.

------F / > ■ cD — ^ C ------I

Table 2.5.8 The Rood-Sastry Cluster Classification Scheme.

Here the size and luminosity of the first-ranked galaxy declines systematically from left to right while, Rood and Sastry suggest, the angular momentum per unit mass simultaneously increases.

After photometrically studying some 15 rich clusters of varying populations, Oemler (1974) has suggested a further classification scheme with three categories of clusters:

cD clusters are dominated by central supergiant galaxies. They are deficient in spirals (which are completely absent in their cores) and contain the greatest proportion of ellipticals of the three cluster types, with (E:SO:Sp) ratios of about (3:4:2). Physically, they are dense, centrally concentrated, and apparently Data Acquisition 41 §2.5 spherical. They also exhibit segregation by mass and morphological type of galaxy, although the observational evidence for the former is marginal. Examples are Abell 1656, AbeU 2199 and AbeU 2670.

Spiral-poor clusters are intermediate in type and are dominated by SO galax­ ies, with (E:SO:Sp) ratios of about (1:2: l). These, too according to Oemler, are segregated clusters, but they are less regular, compact, and centrally condensed than the cD clusters. Examples include AbeU 0400 and AbeU 1214.

Spiral-rich clusters are irregular in appearance, possess a low mean density and have no tendency toward central condensation. Their composition is fairly homogeneous, without perceptible segregation by morphological type, and they show no evidence of dynamical relaxation or mass segregation. Spiral galaxies predominate and the (E:SO:Sp) ratios are typically (1:2: 3). Examples include AbeU 1367, AbeU 2151 and AbeU 2197.

Oemler finds his system to relate most closely to that of Morgan, although the dividing lines between the types do not precisely coincide.

The most recent proposals regarding classification have been advanced by Mel- nick and Sargent (1977). From a study of six X-ray clusters they suggest subdivi­ sion according to the relative radial distributions of different morphological types of member galaxies in each cluster:

Spiral or Sp clusters have a flat integral distribution of ellipticals but steep cumulative distributions of spirals and lenticulars; the SO ’s dominate in the cluster cores and the spirals in the outer regions, so that the integral radial frequency distributions cross. Examples are the Hydra I (AbeU 1060) and Virgo clusters. Data Acquisition 42 §2.5

SO clusters have less flat E distributions, although the cumulative radial SO and Sp profiles are again steep. Here, however, the lenticulars dominate the galaxy populations throughout the clusters, and the integral distributions of SO and Sp galaxies do not cross. To this class belong the clusters Abell 0376 and Abell 0576.

A bell 0426 (the ] appears to be unique in Melnick and Sargent’s sample. Here it is the few spirals which exhibit a flat integral distribution, whereas the SO’s and the E’s show steep parallel distributions at all radii. The number of ellipticals remains larger than the number of SO’s throughout the cluster.

Comparison with the system of Oemler suggests similarities between SO and Sp clusters described above and Oemler’s spiral-rieh ani tpiral-poor chisteis. Moreover the distribution for the Perseus cluster resembles that of Oemler’s cD clusters, with almost no spiral galaxies and with a somewhat larger number of ellipticals.

An important and desirable attribute for any cluster clasification system is that it should be applicable to aggregates at large distances, as is Abell’s simple two-part scheme. Ultimately, however, the usefuUness of any system must depend on how well it elucidates the nature of clusters by correlating their many varying traits.

For our purposes, however, we shall conform to the Abell Two-Part Clas- tification and the Bautz-Morgan Classification schemes. We do this primarily to be consistent with the of galaxy clusters made for the North­ ern Hemisphere, and the forthcoming catalogue of galaxy clusters of the Southern Hemisphere. C H A PTER III

THE CLUSTER CATALOGUE

But by measure and number and weight, Thou didst order all things. - Solomon

A catalogue of the positions of the galaxy clusters is given in Table 8.1.1. The initial tabular data consists of a galaxy cluster identification number. Next the rectangular coordinates of the cluster center as determined by the dispersion ellipse analysis and measured from the geometric center of the plate; we note the use of the standard astrometric conventions with z directed positively in the Eastward direction, contrary to the Cartesian sense. The next two entries are the celestial and new-galactic coordinates of the cluster center for the epoch 1950. These coordinates are determined by applying the plate constants derived from the least-squares fitting of the standard SAO stars to the cluster center rectangular position. Appropriate transformations (see Section 2.3) convert the rectangular coordinates to Right Ascension and Declination and these to new-galactic longitude and latitude. Finally, an estimate of the cluster distance derived from mio is given to complete the table.

43 The Cluster Catalogue 44 §3.0

The measured positions of cluster members, magnitude estimates, and position angle measurements are collected in the following descriptive sections. In Section 8.1 we present the cluster catalogue. The catalogue is in tabular form and gives the locations of the cluster centers for the epoch 1950 as well as their locations on the ESO/SERC J plates. In addition, an estimate of redshift by virtue of mio is pven as a distance indicator.

In S ection S.2 we pve in both graphical form and narrative the following information:

1. Cluster Field. We present an enlargement of the field of every galaxy cluster taken from film copies of the ESO/SERC survey plates. The print scale is typically 10 arcsec/mm and shows the galaxy cluster and its environs.

2. Cluster Membership and Morphology. Here, the measured positions of the cluster members are plotted as they occur on the ESO/SERC Fields alligned with the standard convention of orientation. The plotting grid is based on locations determined from the plate center derived from extending and intersecting the four fiducial marks found on the plate edges. Following this convention. East is located in the Cartesian —x direction. The grids have been prepared in uniform size so as to facilitate intercluster comparisons. The member galaxies have been plotted with various symbols to indicate their morphological type as specified by the legend on the plot.

S. Surface Density Distribution. In this plot, the cluster surface density is plotted as increasingly dense tones and isopleths corresponding to the number of galaxies counted per unit area. The extent of the plots is determined by the actual extreme positions of the member galaxies and so the scale of the plot will vary from cluster to cluster. The central portions of the cluster are emphasized in this case Tie Cluster Catalane 45 §3.0

and thus the plot gives an intuitive, albeit qualitative, impression of the projected surface density of the cluster.

4. Cluster Magnitude Distribution. Here, the estimated magnitudes of the cluster members has been plotted as a histogram in bins corresponding to a change in magnitude of 0.5 as determined by step-scale readings which were converted to visual magnitudes by the appropriate transformations. The data has been smoothed and a “smoothed version” of the data is plotted as a curve over the binned data. This information extends to the limiting magnitude m„ = 19.0 uniformly for all clusters and is useful in determining the Luminosity Function of the cluster.

5. Position Angle Distribution. As an attempt was made to measure the physical extent of galaxies that were larger than 10 microns, a body of data was acquired for each cluster that included an estimate of the major and minor axes of the appropriate galaxy images as well as their position angles. We use the standard convention for the sense of orientation with angles measured in degrees positive Eastward of North. The data is then tabulated in ten degree bins and plotted in histogram form with a smoothed curve of the same data over the histogram. We also present a sector plot which shows by means of a radial vector whose magnitude is directly proportional to the number of galaxies in a given ten degree sector, the position angle distribution of the cluster members.

6. Cluster Membership by Morphological Type. In similar fashion to the initial figure, we plot a to-scale version of the cluster members but sorted by morphological type. The original dispersion ellipse is maintained to assist comparative studies by virtue of location while the cluster members have been separated into elliptical, SO and spiral galaxies and plotted. The center of the cluster is marked and refers to the center of the dispersion ellipse as determined by bivariate methods described elsewhere. The Cluster Catalogue 46 §3.0

7. Cluster Data Table. The data table consolidates the general body of infor­ mation about the cluster. We indicate the cluster number designated by increasing Right Ascension as weU as the position of the cluster center as determined by the dispersion analysis in coordinates of Right Ascension and Declination of epoch 1950. These coordinates are derived from least-squares fitting to the set of standard SAO stars used in the measuring analysis. For each cluster we give the appropriate ESO/SERC Plate and Field number to assist in locating the given cluster. In ad­ dition, the table lists the x and y coordinates of the cluster center in the usual convention as measured from the derived plate center, the epoch 1950 ecliptic and new galactic coordinates, and the cluster redshift as determined by the visual mag­ nitude of the tenth brightest cluster member. Several subtables show the cluster morphology separated and counted to give the number of Elliptical, SO, normal and barred Spiral and Peculiar galaxies; parameters of the calculated dispersion ellipse to include major and minor axes measures in millimeters on the plate and position angle, this time referred to the E-W absissa, with angles measured West to North as positive in the Cartesian convention; and finally some population statistics to include the number of galaxies in the sample, the core population, or the number of galaxies found in the primary dispersion ellipse, and the limiting magnitude of the sample.

8. Cluster Discriptiou. Here, we note individual discriptions of the galaxy clus­ ters. General features of the cluster and its environs are noted along with estimates of cluster Richness and Type. Special attention is paid to unique properties of the cluster, peculiarities discovered and items of special interest. T ie Cluster Catalogue 47 §3.1

8.1 Catalogue of Southern Galaxy Clusters

In this section we present a uniform catalogue of the clusters of galaxies in our sample. For each of the clusters, we present the position of the cluster center as determined by the dispersion ellipse analysis. In this case we give the Cartesian coordinates of the cluster center as found on the ESO/SERC J plates, measured from the plate center found by orthogonal extension of the plate fiducial marks; the Right Ascension and Declination for the epoch 1950 found by the plate transforma­ tion equations developed in Section 2.3; and the galactic latitude and longitude of the cluster center for the epoch 1950. In addition, we give a value of the cluster redshift as determined by mio. Finally, we present the ESO/SERC J plate location of the clusters for quick identification of observation fields. T ie Cluster Catalogue 48 §3.1

CRTRL0GUE 0F BRIGHT SOUTHERN GRLRXY CLUSTERS

NX Y RA DEC L B Z FIELD PLATE

(1950) (1950) (1950) 11950)

01 005.543 -070.735 00 00 45.6 -36 19 39.4 348 51 23.1 -76 26 01.2 0.042 349 J6145

02 035.621 -003.767 00 03 13.9 -35 04 01.6 352 02 54.5 -77 35 08.1 0.072 349 J6145

03 071.702 -039.543 00 06 49.1 -35 43 49.9 347 29 52.6 -77 45 43.8 0.057 349 J5146

04 051.069 -119.610 00 07 28.7 -57 14 52.8 313 59 38.0 -59 15 32.8 0.044 149 JS501

05 -107.031 024.617 00 18 08.3 -49 32 34.3 315 55 27.3 -67 04 38.6 0.050 194 J1861

OS -015.272 094.597 00 22 49.7 -33 17 33.7 345 09 53.8 -81 50 34.0 0.038 350 J4601

07 -005.774 -082.259 01 29 33.8 -51 32 55.7 288 10 19.5 -64 40 13.3 0.040 196 J5467

08 -043.427 -127.677 01 39 50.0 -42 23 49.0 271 41 23.9 -71 46 58.0 0.050 297 J3593

09 087.306 109.659 02 55 44.0 -52 56 09.1 269 10 28.4 -55 20 33.5 0.049 154 J4715

10 -103.679 -070.538 03 44 04.7 -41 21 11.8 245 59 33.1 -51 44 56.9 0.050 302 J3580 11 101.219 054.375 04 04 04.0 -39 00 28.8 241 56 20.8 -48 06 22.5 0.042 302 J35S0

12 -115.824 -001.271 05 24 00.3 -45 01 46.1 250 45 41.6 -33 34 17.9 0.061 253 J6743

13 -083.921 004.016 06 21 39.4 -64 56 34.9 274 42 10.3 -27 29 35.5 0.038 087 J8249

14 -088.653 070.926 06 25 02.5 -53 39 26.8 262 21 36.2 -25 11 15.9 0.049 161 J5538

15 -076.713 032.793 06 26 25.1 -54 22 29.4 263 10 56.4 -25 08 49.3 0.048 161 J5538

16 146.553 065.348 12 51 41.2 -28 44 33.4 303 42 32.9 33 51 13.3 0.048 442 J5750

17 -095.233 -121.728 13 03 25.3 -37 17 59.6 306 10 10.3 25 12 41.6 0.049 382 JI530

18 005.223 069.735 14 00 40.6 -33 44 13.9 319 37 09.5 26 32 41.9 0.020 384 J485!

19 102.148 117.241 14 09 17.9 -32 50 02.6 321 51 15.5 26 48 60.0 0.044 384 J4551

20 102.819 053.059 14 09 28.3 -34 01 36.5 321 26 22.7 25 40 56.0 0.038 384 J455I

21 -043.965 -081.811 14 30 26.3 -31 32 40.5 327 01 28.9 26 17 33.7 0.054 447 J1472

22 003.581 080.348 19 56 35.4 -38 32 47.9 002 03 26.0 -29 14 54.4 0.025 339 J2378

23 -105.191 -022.456 20 38 34.4 -35 23 58.1 007 43 35.8 -36 50 15. 1 0.055 401 J6I09

24 -095.831 -115.415 20 48 40.7 -52 08 45.6 346 31 00.9 -39 25 40.1 0.037 235 J3389

25 -131.705 018.574 21 13 10.0 -59 36 24.2 336 02 49.4 -41 23 39.8 0.042 145 J1759

Table 3.1.1 (a.) Catalogue of Southern Galaxy Clutters T ie Cluster Catalogue 49 §3.1

CATALOGUE OF BRIGHT SOUTHERN GALAXY CLUSTERS

N }( f RA DEC L 8 z FIELD PLATE

(19501 (19501 ( 19501 (19501

26 -144..719 -001,.784 21 22 58,.0 -35 00 38.8 009 47 57,.8 -45 46 32.8 0.,052 403 J5290

27 -033,.381 -057,.179 21 26 09,.6 -51 04 18.4 346 46 32,.5 -45 20 18.5 0.,048 236 J2391

28 -075, .807 -019,.961 21 29 13, .5 -35 22 50.6 009 24 15,.7 -47 04 43.0 0..044 403 J5290

29 -008, .471 - lie ..667 21 31 14,.2 -62 15 40.3 331 40 36,.2 -42 31 56.4 0..048 145 J1759

30 028,.755 064..519 21 31 05,.9 -53 50 08.2 342 41 57, .2 -45 23 37.9 0. .050 188 J1592

31 039,.266 123..490 21 32 18, .2 -52 44 02.1 344 08 48,.2 -45 51 52.5 0.,044 188 J1592

32 096, .553 -093. .917 21 41 46,.5 -51 43 57.4 344 58 17,.5 -47 32 00.7 0.,043 236 J2391

33 074,.215 134.,600 21 42 50,.8 -57 29 48.5 336 58 51,.8 -45 44 51.4 0..042 145 J1759

34 -119,.635 051.,550 21 43 46, .1 -44 05 15.9 356 06 55,.3 -49 31 23.7 0.,048 288 J4594

35 -107.,000 -061.,752 21 44 40,.6 -46 13 32.3 352 51 36,.7 -49 19 04.4 0. .043 288 J4594

36 127.,534 102.,014 21 50 32,.0 -58 03 48.4 335 38 09,.9 -46 27 19.6 0.,050 145 JI753

37 -098.,536 -032.,630 21 55 17,.4 -60 35 13.4 331 59 31,.8 -45 51 03.0 0.,048 145 J6201

38 -080.,549 -010.,760 21 58 08, .7 -60 11 45.0 332 14 19,.1 -46 20 56.5 0. 065 145 J62D1

39 -053.,530 090. ,895 22 01 11. .1 -58 18 35.8 334 23 10,.0 -47 35 52.6 0. 043 146 J5201

40 008.,125 -014..404 22 01 6..9 -50 18 11.9 345 35 47..8 -50 52 6.4 0. 042 237 J3658

41 -101..125 -022. 117 22 19 59..2 -50 23 8.1 343 35 50..1 -53 37 12.6 0. 040 190 J5332

42 -087. .461 -088.,514 22 21 25..9 -56 38 22.8 334 28 44..6 -50 47 22.1 0. 043 190 J5332

43 -079. ,768 -059..435 22 22 36.,0 -56 05 57.1 335 3 58.,2 -51 12 57.0 0. 043 190 J5332

44 -143.,511 -045.,125 22 24 46.,3 -30 51 42.7 017 55 41.,2 -58 26 58.1 0. 038 468 J5435

45 -075..547 -126.,152 23 16 35..3 -42 22 36.6 348 24 55..0 -65 59 02.5 0. 030 347 J2413

46 038..794 021. ,784 23 27 57..5 -39 37 6.8 351 47 36. .1 -69 14 01.1 0. 049 347 J2413

47 038..221 025.,705 23 34 24.,3 -69 34 43.5 312 19 10,,5 -46 27 04.8 0. 057 077 J3664

48 -066..526 -028.,689 23 38 44..8 -30 30 4.2 017 24 7..9 -74 20 20.9 0. 044 471 J6138

49 -015,,479 085. ,995 23 44 55..4 -28 24 42.6 025 10 13,,4 -75 49 04.7 0. 023 471 J5I38

50 104..794 047.,058 23 59 05. .8 -44 06 46.5 330 42 13.,2 -70 30 40.1 0. 038 292 J45C4

Table 8.1.1 (b.) Catalogue of Southern Galaxy Clusters The Cluster Catalogue 50 §3.2

8.2 Descriptions of Southern Galaxy Clusters

In this section we present a uniform description of the clusters of galaxies in our sample. Rather than publish the data in numerical form, we choose a graphical and tabular format for ease of comparison between cluster and cluster. Although nearly 21,000 individual galaxies have been measured the final sample is magnitude-limited and uniform to = 19.0. T ie Cluster Catalogue 51 §3.2

GALAXY CLUSTER 001 00 00 46 - 3 6 19

Figure 8.2.01 faj Field of G A LA X Y CLUSTER 001: 00 00 46 -S6 19 The Cluster Catalogue 52 §3.2

GALAXY CLUSTER 001 00 00 46 - 3 6 19

CLUSTER MEMBERSHIP AND H0RPH0L0GY SURFACE DENSITY OISTRIBUTI0N

£ -49. I

-B.

- 70. Ï 3

legend ; E -.1 # O so= -

£BST t * l£ S T # ? ? Ç = = s r s

CLUSTER MAGNITUDE DISTRIBUTI0N P 0 5 IT I0 N ANGLE D IS T R IB U T I0N 25. -T— I— I— I— I— I— I— I— T -r-l— I— I 1— I— I— I— r- 24. 23. 0 0 . 22. 21. 80. 20. £- 19. 16. TO. 17. 16. 60. 15. 10e«4SO 2466 10 14. H. MÜNT5 POl 8ECTIR 13. 50. 12. 11. 40. 10. 6 . 6. SO. 7. 6. 2 0 . 5. 4. 3. 10. 2. U I. 0. I < 1 I -I I » I I ‘ ' o u, o u, o u, o 5.^^^ o T ïC T fl (OECREESj or ri m fO fO

Figure S.2.01 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 53 §3.2

CRJXY CLUSTER 001 00 00 46 -36 19 GR-RXY [LUSTER 00 1 00 00 46 -36 19 CM. A XT CLUSTER 001 00 00 46 -36 19

i

ELLIPTICAL GALAXIES S0 GALAXIES SPIRAL GALAXIES i £ * * t

GALAXY CLUSTER 001 00 00 46 -36 19

F IE L D 3 4 9 ES0/SERC PLATE J6145

X Y RA DEC L B z (tasoi U9S0I (I9S0I (19S0I 005.543 -070.735 0 0 45.6 -36 19 39.4 348 51 23.1 -76 26 1.2 0.042

MORPHOLOGY DISPERSION ELLIPSE CLUSTER MEMBERS

E 180 MAJOR A XIS 14. 15 SAMPLE POPULATION 330

80 3 3 MINOR A X IS 1 3 .1 0 CORE POPULATION 119

S 9 9 ECCENTRICITY 0.38 LIMITING MAGNITUDE 19.0

SB 13 P0SN. ANGLE - 3 0 . 2 0

P 5

Figure 8.2.01 (J,g,h) Cluster Morphological Population Distributions. Table 8.2.01 Cluster Population Description.

GALAXY CLUSTER 001; 00 00 46 -86 19 : The cluster is located in the South-East quadrant of ESO/SERC Field 349. Within a diameter of 60mm as determined by mio we count 863 galaxies in this cluster and 330 to a limiting magnitude of mnm = 19.0. The cluster is classihed as Abell type R but displays a somewhat elongated N — S concentration of galaxies within the primary dispersion ellipse. The Cluster Catalogue 54 §3.2

We count over 50 galaxies brighter than m 3 + 2 and thus classify the cluster as having an Abell richness of 1 . The brightest galaxy in the cluster has a corona and is highly centrally condensed suggesting a B —M type I-II classification for the cluster. For mi, m3 , and mio we ^ v e 13.5, 14.6 and 15.1, respectively. The value of mio implies a redshift of 0.042.

We have counted the galaxies in this cluster to a limiting magnitude of mnm = 19.0 and see a smooth distribution of magnitudes from the brightest to faintest galaxies. The measured position angles of the appear to show no preferred orien­ tation and we find the population mix of elliptical and spiral galaxies to be about evenly scattered throughout the cluster. The number of elliptical galaxies, how­ ever, is about a factor of two higher than that of the spirals with an apparently poor number of SO galaxies. There seem to be several concentrations of ellipti­ cal galaxies; one, in particular, lies to the West near the periphery of the cluster; another concentration is seen near the center of the cluster, to the North. There appears to be a slight enhancement of spirals in the South-West quadrant of the cluster and a relative paucity in the South-East.

The dispersion ellipse measures 14.15 mm for the major axis and 13.10 mm for the minor axis on the plate. We calculate an eccentricity of 0.38 for the dispersion ellipse which is oriented -30.0 degrees South of West. The core population of the cluster is 119, or some 36% of the galaxies counted and is contained in an area of some 0.2 square degrees. This yields a surface density of 583 galaxies per square degree. The Cluster Catalogue 55 §3.2

GALAXY CLUSTER 002 00 03 14 - 3 5 04

Figure 3.2.02 (a) Field of GALAXY CLUSTER DOS: 00 OS U -S5 04 T ie Cluster Catalogue 56 §3.2

GALAXY CLUSTER 002 00 03 14 - 3 5 04

SURFACE DENSITY DI5TR1BÜTÎ0N CLUSTER MEMBERSHIP AND M0RPH0L0GY I "I......

E a . I n.

9.

•9. i

•IS.

•17. LEGEND^ C = • SO-* i S " * S B = «

CRsr iC S T Ç ? *

CLUSTER MAGNITUDE DISTRIBUTI0N P05ITI0N ANGLE DISTRIBUTI0N loo,

fio. 22. eo. TO. |i 15.

13. "

10.

90.

20.

10. 0 o rsNiTug o oooeeoeoeooeooeooooE TÆTP (DECREES) W iÎ8ëSSStiS5°SSS!SSS^SS

Figure 3.2.02 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 57 §3.2

CnLflXT CLUSTER 002 00 03 H -35 M CRLRXT CLUSTER 002 00 03 14 -35 04 CRLRXT CLUSTER 002 00 03 H -25 04

ELLIPTICAL GALAXIES 50 CRLPXIES SPIRAL GALAXIES M r * l e r BBT m BBT IB i ^ * é < t f * 4 * 1 ^ " * 4 * 4 * 1 * 4 i f - * 4 4 4 4 4 4 *

GALAXY CLUSTER 002 00 03 14 -35 04

FIEJLD 3*9 Csa/SERC PLRTE JB145

X Y RA DEC L B Z C19SQI nasoi IlS S Q I (1 9 5 0 1 0 3 5 . 621 -003.767 0 3 13.9 -35 4 1.6 352 2 54 .5 -77 35 8.1 0 .0 7 2

M0RPHBL0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 159 HRJ0R AXIS 9.50 SAMPLE P0PULATI0N 265

50 20 MIN0R A XIS 7 . 9 6 C0RE POPULATION 85

S 4 6 ECCENTRICITY 0.55 LIMITING MAGNITUDE 1 9 .0

SB 2 P0SN. ANGLE - 3 4 . 2 6

P 30

Figure 3.2.02 (f,g,h) Cluster Morphological Population Distributions. Table 3.2.02 Cluster Population Description.

GALAXY CLUSTER 002: 00 03 14 -35 04 : The cluster is located in South-East quadrant of ESO/SERC Field 349. Within a diameter of 36mm as determined by mio we count 608 galaxies in this cluster and 265 to a limiting magnitude of mjim = 19.0 that are predominantly elliptical. The cluster is classified as Abell type R but seems to have several concentrations of elliptical galaxies in the North-East and North-West quadrants. T ie Cluster Catalogue 58 §3.2

We count over 80 galaxies brighter than ms + 2 and thus classify the cluster as having an Abell richness of 2. The brightest galaxy in the cluster has a corona and is intermediate in appearance between the class cD and normal giant elliptical galaxies suggesting a B — M type II classification for the cluster. For mi, m 3 , and mio we give 15.6, 15.8 and 16.3, respectively. The value of mio implies a redshift of 0.072.

The surface density distribution of this cluster shows several concentrations, one running almost lineeirly East-West across the cluster, two East of center, and another to the South-Southwest. The magnitude distribution is somewhat steep from mv = 15 to m„ = 19 albeit smooth. There appear to be no unusual irregulari­ ties in the position angle distribution with perhaps a very slightly higher of galaxies measured with a position angle near —30°.

The dispersion ellipse holds nearly a third of the cluster population located in an area of some 0.08 square degrees. With a core membership of 8 6 galaxies this repersents a surface density of 1033 galaxies per square degree. The dispersion ellipse is inclined 34 degrees South of West and is somewhat eccentric.

The cluster is rich in elliptical galaxies with nearly four times as many ellipticals as spirals. The few SO galaxies identified appear to be loosely scattered throughout the Western portion of the cluster. The spirals in the cluster appear somewhat evenly divided East and West, but there appears to be a region perpendicular to the dispersion ellipse major axis that is devoid of this type of galaxy. There are several superposed faint pairs of galaxies, often pairs with an early and late type elliptical. In addition, there are several subgroups dominated by a bright elliptical with fainter elliptical attendants as, for example, one located at x = 52.39, y = 2.87. We also note the appearance of severed faint "chains” of galaxies, comprised of four or more galaxies in what looks like a line, such as those found at z = 31.15,^ = —7.02. T ie Cluster Catalogue 59 §3.2

GALAXY CLUSTER 003 00 06 49 - 3 5 44

“l j M t i I 1 I M j I 1 1 . 1 1 I 1 I j . : I I 1 I I ; I I I I I I I I I I I N «

vt *

-i B .

- r-

4 ' :" L ;

Figure 8.2.03 /'oj F*eW 0/ GALAXY CLUSTER OOS: 00 06 49 -S5 44 T ie Cluster Catalogue 60 §3.2

GALAXY CLUSTER 003 00 06 49 - 3 5 43

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTI0N T-TT-r-r-r-rr-r-

i 1

GENE

CLUSTER MAGNITUDE DISTRIBUTI0N P05ITI0N ANGLE DI5TRIBUTI0N 100. 25. 24.

mo. 22. eo. TO. li 15. 13. «g“I

90. 6. a 20.

10. 0. E THETR (DEGREES) k

ei CD CDw r»* r>* ^ CO ifi u) w in w cn cn ; : ; ; : ^ ^ : : : : ; : : : : : :

Figure 3.2.03 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 61 §3.2

CflLflXT CLUSTER 003 DO 06 49 -3S « GflLflXT CLUSTER 003 00 06 43 -35 43 GALAXY CLUSTER 003 DO 06 *9 -35 43

I

3 i

ELLIPTICBL CflLflXIES t f 4 f * ^ 1 * * * * # ; ; * 4 f f f

GALAXY CLUSTER 003 00 06 49 -3 5 43

FIELD 349 ESB/SERC PLBTE J514S

X Y R B DEC L B z (ISSni 119501 119501 119501 071.702 -039.543 0 6 49.1 -35 43 49.9 347 29 52.6 -77 45 43.5 0.057

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 2 9 5 MBJ0R A XIS 1 3 .4 8 SAMPLE POPULATION 463

80 24 MINOR A XIS 1 3 .0 0 C0RE P0PULATI0N 153

S 14 9 ECCENTRICITY 0.26 L IM IT IN G MAGNITUDE 19.0

SB 7 P0SN. ANGLE - 1 5 . 7 3

P 6

Figure 8.2.03 f/,ff,hj Giddier Morphological Population Distributions. Table 8.2.03 Cluster Population Description.

GALAXY CLUSTER 003: 00 06 49 -35 44 : The cluster is located in South-East quadrant of ESO/SERC Field 349. Within a diameter of 60mm as determined by mio we count 868 galaxies in this cluster and 265 to a limiting magnitude of miim = 19.0 that are predominantly elliptical. The cluster is classified as Abell type IR and there are several concentrations of galaxies of all types in the South-East and North-West quadrants. These dense concentrations suggest the possibility of two clusters superposed. The Cluster Catalogue 62 §3.2

We count over 1 0 0 galaxies brighter than m 3 + 2 and thus classify the cluster as having an Abell richness of 2. Since the brightest galaxy in the cluster has a corona and is intermediate in appearance between the class cD and normal giant elliptical galaxies, it suggests perhaps a B — M type Iim classification for the cluster. For m i, m s, and mio we give 13.9,15.6 and 16.3, respectively. The value of mio implies a redshift of 0.057.

The brightest galaxy in the cluster has a halo, whilst the third brightest appears to be a spindle. The Northern portion of the cluster is more densly populated than the Southern, yet there appears to be a relatively high concentration of galaxies in a small region Southeast of the cluster center. This concentration is located at z = 77.87, y = —52.15, is dominated by a bright elliptical (m„ = 15.8), and appears to be populated equally with both ellipticals and spirals, although the main cluster has nearly twice the number of ellipticals as spirals. There are a few obvious barred-spirals, several displaying rings around a dense nucleus, as the one located at * = 89.46, y = —27.24. A small faint group predominately composed of spirals is located at z = 57.35, y = —35.85 and there are several elliptical galaxies apparently surrounded by a constellation of very faint attendants. Several galaxies are termed peculiar because of possible superposition or irregularities and there are a number of very low surface brightness galaxies with very f ^ t but distinguishable nucleii.

The dispersion ellipse has a core population of 163, or some 34% of the sample with a limiting magnitude of = 19.0. With an eccentricity of 0.26 and a position angle of 15.73° South of West, the dispersion ellipse spans 0.19 square degrees and gives a core surface density of 845 galaxies per square degree on the sky. T ie Cluster Catalogue 63 §3.2

GALAXY CLUSTER 004 00 07 29 - 5 7 15

Figure 3.2.04 fa) Field of GALAXY CLUSTER OO4: 00 07 29 -57 15 T ie Cluster Catalogue 64 §3.2

GALAXY CLUSTER 004 00 07 29 - 5 7 15

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBÜTI0N

I •I DO. S

o Oo •1 9 0 . £ i o- .:iO

LEGEND •Its. z

-170.

•1 1 0 . EAST

? 4 4 T « • « mm

CLUSTER MAGNITUDE D IS T R IB U T I0N P05ITI0N ANGLE DÎ5TRIBUTI0N 100. 25. -T — I— :— I— r— T- 23.24. 90. 2 2 . 2 1 . 80. 20. 19 . 16. 70 . 17. 16. 15. 10 e 6 4 2 0 2466 10 14. C6UNT3 fCR SECrm 13. 50: 12. II. 4 0 , 10. 9. 6. 30. 6.7. 2 0 . 5. 4 . 3. 10. 2. i. 0 0. eeaooeE o o eo o oeeo TÆTA oo (DECREES) R8PSSSRS2®2gR5ase

Figure 3.2.04 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 65 §3.2

GBLfIXY CLUSTER OtM 00 07 25 -57 15 CRLBXT CLUSTER 001 00 07 29 -57 15 CRLfiXT CLUSTER 001 00 07 29 -57 15

i i

ELLIPTICAL g a l a x ie s SPIRAL GALAXIES ICST BBT 4 -* < * # f ^ f ^

GALAXY CLUSTER 004 00 07 29 -5 7 15 FIELD 119 ESB/SERC PLATE J6S0I

X Y RA DEC L B Z (lesoi 119501 119501 (19501 0 5 1 . 06 9 - 1 1 9 .6 1 0 0 7 2 8 .7 - 5 7 14 5 2 . 8 313 59 38.0 -59 15 32.8 0. 044

M0RPH0L0GY DISPERSIONELLIPSE CLUSTER MEMBERS

E VI MAJOR AXIS 1 3 .2 4 SAMPLE POPULATION 153

50 27 MINOR AXIS 1 0 .8 9 CORE POPULATION 63

5 50 ECCENTRICITY 0.57 L IM IT IN G MAGNITUDE 1 9 .0

SB 3 P0SN. ANGLE 5 8 .2 0

P 2

Figure 3.2.04 (f,g,h) Cluster Morphological Population Distributions. Table 8.2.04 Cluster Population Description.

GALAXY CLUSTER 004: 00 07 29 -57 15 : The cluster is located in South-West quadrant of ESO/SERC Field 149. Within a diameter of 60mm as determined by mjo we count 157 galaxies in this cluster and 153 to a limiting magnitude of miim = 19.0. The cluster is classified as Abell type IR mainly because of the concentrations of galaxies being non-uniform.

We count over 50 galaxies brighter than mj + 2 and thus classify the cluster The Cluster Catalogue 66 §3.2 as having an Abell richness of 1. We suggest a B —M type HI classification for the cluster which has several normal giant ellipticals, the brightest of which appears to be superposition of an early and a late elliptical. For mj, mj, and mio we give 13.2, 14.3 and 15.1, respectively. The value of mio implies a redshift of 0.044.

The cluster magnitude distribution is depressed near m„ = 16.5 and tapers off after m„ = 18.5 suggesting several populations making up the cluster. We also note a very slight excess of galaxies with orientation of 75 — 80° but do not deem it significant.

We find a slight concentration of predominately elliptical galaxies just South of the cluster center and there is a large region, comprising nearly half of the Southern portion of the dispersion ellipse that is practically devoid of spirals. The third brightest galaxy appears to be a spindle. The morphological distribution {E : SO : 5) goes as (3:1:2) while the core population represents 41% of the total magnitude limited sample. The dispersion ellipse spans some 0.16 of a square degree which implies a surface density of some 397 galaxies per square degree. The position angle of the dispersion ellipse is inclined some 58 degrees North of West. The Cluster Catalogue 67 §3.2

GALAXY CLUSTER 005 00 18 08 - 4 9 32

Figure S.2.05 faj Field of GALAXY CLUSTER 005: 00 18 08 -49 S2 The Cluster Catalogue 68 §3.2

GALAXY CLUSTER 005 00 18 06 - 4 9 32

sunrncc dcn 3 I tt Disrr^iDUTiBN CLUSTER MEMBERSHIP AND M0RPH0L0GY •0.

I !

i

LEGEND. E = ' : B 0 = » : I •II. S V « 1 Sfis • i

s e

CLUSTER MAGNITUDE DISTRIBUTION POSITION ANGLE) D ISTRIBU TIO N

K.

BQ.

TO.

FI I s n m

3 0 .

20. 4

1 0 .

„ o u> o T « T P (DECREES) r: œ m ui ui «" V

Figure S.2.05 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 69 §3.2

CRLBla aUSTER 005 00 18 08 -M 32 CRLBXT CLUSTER 005 00 18 08 -49 32 CRLBXT CLUSTER 005 00 18 OS -49 32 ..... I III I li ^

3 m:

. *• i : ELLIPTICAL GALAXIES 50 GR.AXIE5 SPIRAL WLRXIES m K31 BBT IB *■ BBT IB * * * * t i i t t t i ******** t * i ******* « * * (

GALAXY CLUSTER 005 00 18 08 -49 32

F IELD 1 9 4 ES0/SERC PLATE JIBBl

X Y RR DEC L B z 119501 119501 19501 119501 -1 0 7 . 031 024.617 0 18 8.3 -49 32 34.3 315 55 2 7 . 3 - 6 7 4 3 8 .8 0 .0 5 0

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 115 MAJOR AXIS 8 .1 8 s a m p l e POPULATION 214

S0 23 MINOR AXIS 7.37 CORE POPULATION 84

s 7 0 ECCENTRICITY 0.43 L IM IT IN G MAGNITUDE 1 9 .0

SB 6 P0SN. ANGLE 4 2 .0 9

P 0

Figure S.2.05 (f,g,h) Cluster Morphological Population Distributions. Table 8.2.05 Cluster Population Description.

GALAXY CLUSTER 005: 00 18 08 -49 32 : The cluster is located in North-West quadrant of ESO/SERC Field 149. Within a diameter of 36mm as determined by mio we count 281 galaxies in this cluster and 214 to a limiting magnitude of rnjim = 19.0. The cluster is classified as Abell type R because of its compact center and relatively smooth distribution of galaxies.

We count 67 galaxies brighter than ma+2 and thus classify the cluster as having The Cluster Catalogue 70 §3.2

an Abell richness of 1. We suggest a B —M type II classification for the cluster which has several giant ellipticals, intermediate between cD and normal giant ellipticals. The brightest cluster member appears to be a superposition between an early and a late elliptical. For m i, m j, and mio we give 14.2, 15.0 and 15.4, respectively. The value of mio implies a redshift of 0.050.

Two concentrations seem to be evident in this cluster. The largest is evident just North of the cluster center spanning some 20 minutes of arc from East to West and the second, a much smaller concentration South-West of the cluster center. The magnitude range spans five magnitudes, shows a gentle rise of population with increasing magnitude, a plateau region near m„ = 17.0, and then a sharper rise to the limiting magnitude. The position angle distribution shows a marked increase of galaxies oriented with position angles West of North with a large fraction oriented nearly North-South. The former concentration most likely refiects the higher density of galaxies in the first and fourth quadrants rather than an intrinsically preferred orientation.

The number of elliptical galaxies in the cluster exceeds that of any other popu­ lation group being nearly one-and-one-half times as numerous as spirals, with spirals being nearly three times as numerous as SO’s. The core population represents 39% of the population and with the dispersion ellipse spanning 0.066 square degrees, it suggests a surface density of galaxies of 1265 galaxies per square degree.

We note that the cluster contains several close pairs of elliptical galaxies of early and late type, as for example, those located at z = —101.90, y = 15.60. T ie Cluster Catalogue 71 §3.2

(:luij 5)TE:];t c ) o e ; ()C) 5>() -- 3 c ) I ' z

#

Figure 3.2.06 (a) Field of GALAXY CLUSTER 006: 00 22 50 -SS 17 Tie Cluster C atalane 72 §3.2

GALAXY CLUSTER 006 00 22 50 - 3 3 17

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTION tn.

140.

IM.

no.

110.

too.

«0.

to.

to. liU ERST I£ S T ? ? P

CLUSTER MAGNITUDE DISTRIBUTION POSITION ANGLE DISTRIBUTION 100.

90.

TO.

50: «I

90. 6. S 2 0 .

10. 0. o

Figure 3.2.06 (b) Ghsier Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 73 §3.2

CRLflXY CLUSTER 006 00 22 SO -33 17 GALAXY CLUSTER 006 00 22 50 33 17 GALAXY CLUSTER 006 00 22 50 -33 17

ELLIPTICAL GALAXIES SPIRAL GALAXIES BBT BBT f < ? a W R ^

GALAXY CLUSTER 006 0 0 22 50 -33 17

FIELD 350 ESO/SERC PLATE J 5531

X Y RR DEC L BZ (19501 (19501 (19501 (19501 - 0 1 5 . 272 094.597 0 22 49.7 -33 17 33.7 345 9 53.8 -81 50 34.0 0 .0 3 8

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 150 MRJ0R A X IS 14 .5 1 s a m p l e POPULATION 335

50 34 MINOR A X IS 1 3 .7 0 CORE POPULATION 114

S 144 ECCENTRICITY 0 .3 3 L IM IT IN G MAGNITUDE 1 9 .0

SB 5 P0SN. ANGLE 3 6 .7 7

P 2

Figure 3.2.06 (f,g,h) Cluster Morphological Population Distributions. Table S.2.06 Cluster Population Description.

GALAXY CLUSTER 006; 00 22 50 -33 17 : The cluster is located in North-West quadrant of ESO/SERC Field 350. Within a diameter of 60mm as determined by mio we count 347 galaxies in this cluster and 335 to a limiting magnitude of mum = 19 0. The cluster is classified Abell type RI because of it being somewhat regular but with some concentrations.

We count 97 galaxies brighter than mj +2 and thus classify the cluster as having The Cluster Catalogue 74 §3.2 an Abell richness of 2. We suggest a. B — M type II classification for the cluster which has a mild core-halo configuration with the brightest galaxies intermediate between the class cD and normal giant ellipticals. For and mio we give 13.9,14.3 and 14.9,respectively. The value of mio implies a redshift of 0.038.

As mentioned above the cluster displays a mile core halo configuration with a somewhat diagonal concentration of cluster members running South- West to North- East about 20mm long on the plate located just South-East of the cluster center. There appears to be a small concentration of galaxies slightly more South-East of this structure.

The brightest galaxy in the cluster appears to have a corona; likewise, othe bright members are seen to possess extended envelopes and halos. The cluster magnitude distribution displays a gentle rise from thirteenth to about sixteenth magnitude where it appears to flatten off somewhat. An enhancement of the number of faint galaxies appears to occur in the eighteenth magnitude range.

The position angle distribution for the brighter galaxies seems dominated by inclinations West of North with two other noticable peaks occurring near 0.0 degrees and 50.0 degrees East of North.

We notice a heavier concentration of elliptical galaxies near the center of the cluster and within the dispersion ellipse, whereas the spirals appear to be more uniformly distributed. The elliptical-spiral ratio appears to be nearly 1 : 1 with a relative paucity of SO galaxies, which may be due to selection.

The core population of the cluster represents nearly 34% of the sample in an area of nearly 0.22 square degrees yielding a surface density of 521 galaxies per square degree in the dispersion ellipse. T ie Cluster Catalogue 75 §3.2

GALAXY CLUSTER 007 01 29 34 - 5 1 33

. . .. -1.

I ft

■J^.• ...' '-'r -V fw.'. /-"mf../ ' ^ JsSs^SiiS '% •^- • ^f 4 •■''■'•V.-.’'-^sjr-■’ ’ ■ ■„

m "..?• V0K . .,• -j

;5 &#%

%'r.' H jsSt.''" . 3 #% 2CsK)*^.

Figure 3.2.07 faJ Field of G A LA X Y CLUSTER 007: 01 SO S4 -51 SS T ie Cluster Catalogue 76 §3.2

GALAXY CLUSTER 007 01 29 34 - 5 1 33

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUT10N •B. 1- x' i i T nr"4 4 "I I 4 I 4 I V 4 I 1 I' '% r - r r t i r-

-a.

3 Ï

•uo.

•iifi.

so=

•148 . j < I I ' ' I i i \ I : ) EAST

f ? ? C t v «.MB

CLUSTER MAGNITUDE D IST R IB U T I0N POSITION ANGLE DISTRIBUTION IX.

X. 22 . N.

70.

X 15.

SO. «0, s . za. 1:1

10.

0 , E TtETA IÜECREES1 o u. o u, «'ÏFo u> . eeoeoeoeeocs iliiPsasRS2®s S g g E S

Figure 8.2.07 (b) Cluster Morphology, (e) Surface Density Distribution, (dj Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 77 §3.2

CALAn CLUSTER 007 01 29 31 -51 33 CALRXT CLUSTER 007 01 29 31 -51 33 GALA XT CLUSTER 007 01 29 31 -SI 33

i

SPIRAL GALAXIES

GALAXY CLUSTER 007 01 29 34 -51 33

F IE L D ID E CSa/SERC PLATE J 54 S7

X Y RA DEC L B Z (19501 (19S0I (195DJ (I9S0I 005.774 -082.259 1 29 33.8 -51 32 55.7 288 10 19.5 -64 40 13.3 0.040

MORPHOLOGY DISPERSION ELLIPSE CLUSTER MEMBERS

E 118 MAJOR AXIS 12.91 SAMPLE POPULATION 289

S0 2 5 MINOR AXIS 12.56 CORE POPULATION 96

S 140 ECCENTRICITY 0.23 L IM ITIN G MAGNITUDE 19.0

SB 5 P0SN. ANGLE -57.00

P 1

Figure 8.2.07 (f,g,h) Cluster Morphological Population Distributions. Table 8.2.07 Cluster Population Description.

GALAXY CLUSTER 007: 01 29 84 -51 88 : The cluster is located in South-West quadrant of ESO/SERC Field 196. Within a diameter of 60mm as determined by mio we count 300 galaxies in this cluster and 289 to a limiting magnitude of mum = 19.0. The cluster is cleissified Abell type RI because of its somewhat linear concentration of galaxies near the center of the cluster surrounded by a somewhat uniform scatter of cluster members. The Cluster Catalogue 78 §3.2

We count 37 galaxies brighter than m 3 +2 and thus classify the cluster as having an Abell richness of 0. We suggest a B — M type IH classification for the cluster which has no really dominant galaxies other than what appears to be a superposed field spiral. For m i,m 3 , and mio we give 14.0,14.7 and 15.1,respectively. The value of mio implies a redshift of 0.040.

We note a concentration of galaxies South-East of the cluster center with a few small very dense concentrations such as the one at z = 10.0, y = -93.0. There is a slow increase in fainter populations with increasing magnitude reaching a plateau near m^ = 17.0 and then a dramatic increase of members in the next magnitude range. Position angles show a slight concentration of brighter galaxies with inclinations West of North with an apparent enhancement near zero degrees.

The cluster population appears somewhat spiral enhanced with a E : S ratio of 1:1.2 with apparently fewer SO galaxies noted in the population. We notice a con­ centration of elliptical galaxies South-East of the cluster center and a concentration of spiral galaxies North-West of center.

The core population comprises slightly over a third of the galaxies in the sample and resides in an area of nearly 0.18 square degrees, giving a core surface density of 538 galaxies per square degree.

We find several superposed galaxies in this cluster such as the centrally con­ densed diffuse ovoid superposed at its pole with a faint elliptical galaxy at z =

—2 2 .2 , 1 / = —79.41. In addition, we discover another elliptical spiral combina­ tion apparently superposed with (or possibly connected by) a luminous bridge at z = —6.52, y = -95.01. Another luminous bridge combination is found at X — —18.26, y = —88.56. Finally, several superposed pairs are seen such as the set at z = —22.03, y = —91.31. T ie Cluster Catalogue 79 §3.2

GALAXY CLUSTER 008 01 39 50 - 4 2 24

Figure 3.2.08 (a) Field of GALAXY CLUSTER 008: 01 SO 50 -42 24 The Cluster Catalogue 80 §3.2

GALAXY CLUSTER 008 01 39 50 -42 23

SURFACE DENSITY DISTRIEUTI0N CLUSTER MEMBERSHIP AND M0RPH0L0GY

i I

•190. 1 i i

•ISO. LEGEND

-170.

•IK.

8 8 S 3 8 3 8

CLUSTER MAGNITUDE DISTRIBUTION PO SITIO N ANGLE D ISTRIBUTION 100. 25. 24. •0 . 80.

70.

15. 13. "

90. l:s 2 0 .

10.

^ MflGNITOGI R»g€ ^ ^ r- t*. ID to m to 5 3 3 2 S S

Figure 3.2.08 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 81 §3.2

cn.nxr aiSTER oos oi 39 so -12 23 0 cn.nxr CLUSTER oœ 01 39 so -42 23 0 cfuixT ausiER ooe o: as so -42 23 0

i 9

I ELLIPTICBL cajW IES 30 GALAXIES SP IR A L GALAXIES

GALAXY CLUSTER 008 01 39 50 -42 23$

f ie l d 2 9 7 ES0/SERC PLATE J3SS3

X Y RR DEC L B 2 US5DI I19S0I (1950J [195QJ 043.427 -127.677 1 39 50.0 -42 23 49.0 271 41 23.9 -71 46 58.0 0.050

M0RPHBLBGY DISPERSION ELLIPSE CLUSTER MEMBERS

E 103 MRJ0R A X IS 1 1 .1 6 SAMPLE P0PULRTI0N 214

SB 24 MIN0R AXIS 9.20 C0RE P0PULRTI0N 76

S 7 5 ECCENTRICITY 0.57 LIMITING MAGNITUDE 19.0

SB 10 P0SN. ANGLE 3 4 .7 5

P 2

Figure 8.2.08 (f,g,h) Cluster Morphological Population Distributions. Table 8.2.08 Cluster Population Description.

GALAXY CLUSTER 008: 01 89 50 -42 24 : The cluster is located in South-West quadrant of ESO/SERC Field 297. Within a diameter of 45mm as determined by mio we count 265 galaxies in this cluster and 214 to a limiting magnitude of rrium = 19.0. The cluster is classified Abell type RI and shows a slight somewhat linear enhancement of galaxies near the core of the cluster.

We count 62 galaxies brighter than + 2 and thus classify the cluster as T ie Cluster Catalogue 82 §3.2

having an Abell richness of 1 . We suggest a B — M type III classification for the cluster which lies somewhat intermediate between those clusters domimated by a single cD galaxy and those with several giant ellipticals. For m i,m 3 , and mio we give 14.5,14.8 and 15.4,respectively. The value of mio implies a redshift of 0.050.

We notice a nearly North-South linear concentration of galaxies near the clus­ ter center as well as several regions of slight enhancement of numbers. This cluster is found to be somewhat centrally condensed as shown in the surface density dis­ tribution plot.

The cluster magnitude distribution shows a ramp-like increase in the population form m„ = 14.5 to m„ = 18.5 with two enhancements in the range 16.5 — 17.0 and 18.0 — 18.5. For the brighter members of the cluster, we find position angles more positive in the sense East of North and slightly more inclined at zero and near fifty degrees than average.

The population is dominated by elliptical galaxies with a [E : SO : S) ratio of (4:1:3). The ellipticals are scattered throughout the dispersion ellipses, but somewhat concentrated in the core. SO galaxies seem to be concentrated in the Northerly portions of the clusters whereas the spirals show little concentration at all, but a more uniform scatter. The core population represents nearly thirty-five percent of the sample in an area of 0 . 1 1 square degees giving a cluster core surface density of 672 galaxies per square degree.

We note several superposed or very close pairs of galaxies (of which we find seven ) which seem consistently to be composed of an early elliptical and a later one which is usually fainter. Examples can be found at the following locations: * = —51.76, y = —115.22; x = —38.19, y — —145.40 and x = —29.41, y = —145.09. T ie Cluster Catalogue 83 §3.2

GALAXY CLUSTER 009 02 55 44 - 5 2 53

• ♦

Figure 3.2.09 faj Field of GALAXY CLUSTER 009: OS 55 44 -52 56 T ie Cluster Catalogue 84 §3.2

GALAXY CLUSTER 009 02 55 44 - 5 2 56

SURFACE DENSITY DISTRIBUTI0N CLUSTER MEMBERSHIP AND H0RPH0L0GY

I !

i i

1

CLUSTER MAGNITUDE D I5T R IB U T I0N P 0 5 IT I0 N ANGLE! D I5 T R IB U T Î0 N 100. 2 5 . 2 4 . 2 3 . n. 22. 21. eo.

70. Ii16. 1,: I 10 # e oiMT^rn4 2 0 3Ecrm2460 10 1 3 . ' :: I 10. ! 9 . j 8. ! 90. 7. : 6 . i ZO. 5. ; r 4. ' : r- 3. 10 . 2. 1. 0. THETfl lOEGREES) o in o in in o ui o oimmrJ^inminin^^

Figure 3.2.09 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalane 85 §3.2

CRLflXT CLUSTER 009 02 SS -52 56 CHLflXT CLUSTER 009 02 55 45 -52 58 CALRXT CLUSTER 009 02 55 44 -52 56

I

i

EU-IPTICn. GALAXIES SPIRAL GALAXIES B B T m IC 9 I t t f f t * t * * * f f # f ^ # f » f f

GALAXY CLUSTER 009 02 55 44 -52 56 FIELD154 ESB/SERC PLATE J4716

X Y RR DEC L B Z (19501 (lasoi (18501 I1S50I 0 8 7 . 305 1 0 9 .5 6 9 2 55 49.0 - 5 2 55 9 . I 259 10 28.4 -55 20 33.5 0 .0 4 9

■M0RPHBL0GY DISPERSION ELLIPSE CLUSTER MEMBERS

EISO MAJOR AXIS 1 0 .2 5 SAMPLE P0PULRTI0N 355

S0 33 MIN0R AXIS 9 .5 8 C0RE P0PÜLATI0N 125

s 129 ECCENTRICITY 0 .3 6 L IM IT IN G MAGNITUDE 19 .0

SB 4 P0SN. ANGLE - 3 8 . 1 4

P 0

Figure 8.2.09 f/,g,hj Cluster Morphological Population Distributions. Table 8.2.09 Cluster Population Description.

GALAXY CLUSTER 009; 02 55 44 -52 56 : The cluster is located in North-East quadrant of ESO/SERC Field 154. Within a diameter of 45mm as deter­ mined by mio we count 438 galaxies in this cluster and 356 to a limiting magnitude of mutn = 19.0. The cluster is classified Abell type I due to the several concen­ trations of galaxies found and the general lack of smoothness in the distribution of cluster members. T ie Cluster Catalogue 86 §3.2

We count 8 6 galaxies brighter than m 3 + 2 and thus classify the cluster as having an Abell richness of 2. We suggest a B — M type II classification for the cluster which has as its first brightest member an elliptical galaxy with a corona.

The third brightest object in the cluster is a spiral. For m i,m 3 , and mio we give 14 4,14.8 and 15.4,respectively. The value of mio implies a redshift of 0.049.

The distribution of cluster membership shows several small concentrations of galaxies within the cluster. The main subgroup consists of a knotty chain of galaxies running North-East to South-West, South-East of the cluster center. A relatively dense region is located at z = —82, y = 1 0 1 where several galaxies form a subgroup dominated by a bright pair.

The magnitude distribution exhibits a somewhat uniform increase in brightness at all magnitudes although a slight change of slope occurs near m„ = 16.5. We find that the position angle distribution of the brighter galaxies shows a preference for those galaxies aligned in projection to the direction of the major axis of the dispersion ellipse, that is. East of North.

We note an [E : SO : 5) ratio of ( 1 : 0.17 : 0.68) with the ellipticals occuring scattered throughout the cluster as well as being in present in several clumps. The spirals are located predominantly in the Southern quadrants of the cluster, with a relative paucity in the Northern quadrants. We find similar behavior with the SO galaxies but are aware of possible misidentifications that might arise with confusion of this class with that of the ellipticals at large distances.

The core population contains some 35% of the galaxies in the sample within an area of nearly 0.11 square degrees. This provides some 1164 galaxies per square de­ gree for the core population, which resides in a somewhat eccentric (0.36) dispersion ellipse aligned nearly forty degrees South of West. T ie Cluster Catalogue 87 §3.2

GALAXY CLUSTER 010 03 44 05 - 4 1 21

Ii

Figure 3.2.10 (a) Field of GALAXY CLUSTER 010: OS U 05 - 4I 21 The Cluster Catalogue 88 §3.2

GALAXY CLUSTER 010 03 44 05 -4 1 21

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTION

g I

O s

so=

86 - $

ERST WEST fi P 8 ^ s R R S 8

CLUSTER MAGNITUDE DISTRIBUTI0N soo. ZS. -I—I—I—I—I—1—I—i—j—I—I—I—I—I—I—I—r-P05ITI0N ANGLE DISTRIBUTION 24. 23. ea. 2 2 . 21. 60. 20. K- 19. 16. 70. 17. 16. 15. *0 # e 4 2 D 24 6 6 10 14. CMTB W SEnm 13. 12. 11. 40, 10. 6. 90. 8. 6.7. 5. 4. 10. 2.3. 1. 0, 0. 1 - 1—' I I _i_ LM 11 Mill I [t_ j_ THETfl (DECREES) o in o u, in o • oeeoeeeeoooeoooooo 88P88^RR2«2ER88SRS8

Figure 3.2.10 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catahgue 89 §3.2

C r i M T f CLUSTER 010 03 44 05 <41 21 5 CRJ4XY CLUSTER 010 03 44 05 -41 21 5 GtAXT CLUSTER 010 03 44 05 -41 21 5

I

i

E L L IP T IC A L GALAXIES SPIRAL GALAXIES ■■r m lot i i i i t

GALAXY CLUSTER 010 03 44 05 -41 21:

FIEUn 3C2 ESB/SERC PLATE J3SB0

X Y RR DEC L B 2 IIBSOI 119501 I18S0I (19501 103.679 -070.536 3 44 4.7 -41 21 11.8 245 59 33.1 -51 44 55.9 0.050

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 78 HRJ0R AXIS 14.66 SAMPLE P0PULATI0N 224

50 40 MIN0R AXIS 13.15 C0RE P0PULATI0N 90

5 96 ECCENTRICITY 0.44 L IM IT IN G MAGNITUDE 1 9 .0

SB 8 P0SN. ANCLE -14.11

P 2

Figure 3.2.10 (f,g,h) Clutter Morphological Population Distributions. Table 8.2.10 Cluster Population Description.

GALAXY CLUSTER 010: 08 44 05 -41 21 : The cluster is located in South-West quadrant of ESO/SERC Field 302. Within a diameter of 60mm as determined by mio we count 227 galaxies in this cluster and 224 to a limiting magnitude of mum - 19.0. The cluster is classified Abell type R due to its inherent regularity and central condensation.

We count 93 galaxies brighter than mj + 2 and thus classify the cluster as The Cluster Catalogue 90 §3.2 having an Abell richness of 2. We suggest a B — M type I classification for the cluster which has a dominant cD galaxy near the cluster center. We notice also, that the third brightest galaxy has a corona For mi,ms, and mio we give 13.5, 15.1 and 15.4,respectively. The value of mio implies a redshift of 0.050.

The central cD galaxy is surrounded by faint attendants and dominates the cluster. This central condensation provides the highest surface density in the cluster. We find a rapid rise of population with magnitude to a plateau near m„ = 16.5 a quick jump to m» = 18.0 and then a sudden fall at fainter magnitudes. The distribution of bright galaxy position angles is practically uniform and appears to ■how no preferential position angle.

In this cluster we find the spiral galaxies more numerous with an (E:SO:S) ratio of (l.0:0.5:1.2). The ellipticals seem to be concentrated near the center of the cluster with an obvious enrichment near the central cD. SO galaxies are scattered throughout the cluster as are the spirals, which have a slight preference for the Eastern portions of the cluster.

The core population represents some 40% of the sample in an area of 0.21 square degrees. This represents a core surface density of 424 galaxies per square degree.

We notice the occurence of several close pairs and groups of galaxies in the cluster. For instance a pair of superposed and somewhat peculiar dense ovoid galaxies with extended envelopes is located at x = —130.26, y = —88.78. In addition there are many low surface brightness galaxies with bright nucleii and a few concentrations of galaxies above the general field, notably that located at X = —91.06, y = -68.77. The latter is composed primarily of spiral-type galaxies. The Cluster Catalogue 91 §3.2

GALAXY CLUSTER O il 04 04 04 - 3 9 00

Figure S.2.H (a) Field of GALAXY CLUSTER Oil: Of Of 04 -SO 00 T ie Cluster Catalogue 92 §3.2

GALAXY CLUSTER O il 04 04 04 - 3 9 00

SURFACE DENSITY DISTRIBUTION CLUSTER MEMBERSHIP AND M0RPH0L0GY 110. I .* I I...I .1. I 4 ^ 1 t I. i t ! f . 1.1 yrri r-v f r

H. I I ? TÎ.

s i 1 f :

m.

IfGENDC = • : 80= * : II. B ■ * i EB= • : I * * ') ' ' EAST m WEST S 9 S £ 8 8 ? P S8 ■ aw "'4455?=-=

CLUSTER MAGNITUDE D IST R IB U T I0N POSITION ANGLE DISTRIBUTION too. 2 5 . T—I—1—I—I—I—r- M. 23. •0. 22. 21. ■ Q . 2 0 . 19. 16. 70. n . IE. IS. n.eitozieeio 1 1 . Mwm PEx snv 13. 50, 12. 11. 40| 10. 6. 90. а. б.7. 2 0 . 1.5 . è: to. 2.3. I. a. 0. ^«NITUg ^ „ oe E «eaooe eoot i c toaoe b i d e ceoeo r e e s i w 88£8898S£»S£8S8S£S8

Figure 3.2.11 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 93 §3.2

CHLHXT aUSTK on M CM O'! -39 OQ OR.flXT CLUSTER O il CM CM 04 -39 00 Cn.B)(T CLUSTER Oil 04 0-5 04-39 00

3 3 «I

# f $ ( f ^ $ * f < # # # f f ; $ $ f f f f * * ( f f ^ f f f

GALAXY CLUSTER O il 04 04 04 -3 9 00

FIELD 302 ES0/SERC PLATE J3560

X Y RR DEC L B H II9 S 0 I 119501 (ISSOI 119501 1 0 1 .2 1 9 0 5 4 .3 7 5 4 4 4 . 0 - 3 9 0 2 8 .8 241 56 20.8 -48 6 22.5 0 .0 4 2

M0RPH0L0GY O ISPERSI0N ELLIPSE CLUSTER MEMBERS

E 36 MRJ0R AXIS 1 3 .4 9 SAMPLE POPULATION 107

S0 16 MIN0R AXIS 1 1 .2 9 C0RE POPULATION 55

S 5 0 ECCENTRICITY 0.55 LIMITING MAGNITUDE 19.0

SB 4 P0SN. ANGLE - 2 9 . 5 8

P 1

Figure 8.2.11 f/,ff,hj Cluster Morphological Population Distributions. Table 8.2.11 Cluster Population Description.

GALAXY CLUSTER Oil: 04 04 04 -89 00 : The cluster is located in North-East quadrant of ESO/SERC Field 302 . Within a diameter of 60mm as determined by mio we count 112 galaxies in this cluster and 107 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type IR because of its somewhat irregular surface density, although it is centrally condensed.

We count 53 galaxies brighter than m 3 + 2 and thus classify the cluster as The Cluster Catalogue 94 §3.2 having an Abell richness of 1. We suggest a possible B — M type II classification for the cluster which displays a number of bright elliptical galaxies of intermediate appearance. For m ijtnj, and mxo we give 13.4, 14.7 and 15.1,respectively. The value of mio implies a redshift of 0.042.

The cluster membership is widely scattered save for the central portions of the dispersion ellipse. We note a high concentration of galaxies just South of the cluster center and a more dispersed collection of members distributed Northward of the cluster center.

The total cluster membership is somewhat small, and the magnitude distribu­ tion shows a gentle rise to a plateau at m„ = 16.0. There apears to be an isolated group of faint galaxies from seventeenth to nineteenth magnitude. The position angle distribution appears to be concentrated in the positive sense, that is. East of North with a zone of avoidance of large angles of the opposite sense.

We find an [E : SO : 5) ratio of (1.0 : 0.44 : 1.39) and thus a relatively spiral-rich cluster. Both the ellipticals and spirals are somewhat uniform in their distribution with a higher concentration of spirals in the core population than el­ lipticals. The cluster core contains over 51% of the sample population within an area of nearly 0.17 square degrees. This yields a surface density of 328 galaxies per square degree. The Cluster Catalogue 95 §3.2

GALAXY CLUSTER 012 05 24 00 - 4 5 01

rrp iji I I'r 111 ! 11 n 1 ii i 11M11 ! j 11111111 ■ 11 W l

■ . I

-m.

-A .t-

.- v-«-- «

■•• • ■ ..

. 1 - • V',»., ••V'^'vyi•.

Figure 8.2.12 (a) Field of GALAXY CLUSTER 012: 05 24 00 -45 01 The Cluster Catalogue 96 §3.2

GALAXY CLUSTER 012 05 24 GO - 4 5 01

SURFACE DENSITY DISTRIBUTI0N CLUSTER MEMBERSHIP AND M0RPH0L0GY 8. • I' iV JW 4 I I I I i -l \ p r ' . r I V ‘----1“ E a.

n.

0* - 4>

EAST MM S g s R 8 S P

CLUSTER MAGNITUDE DISTRIBUTI0N P0SITI0N ANGLE DISTRIBUTI0N

22.

6. a

S S

Figure 3.2.12 fbj Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 97 §3.2

CflLflXT CLUSTER 012 05 24 00 -45 01 5 CRLflXT CLUSTER 012 05 24 00 -45 01 6 GALAXY CLUSTER 012 05 24 00 -45 01 6

i i

I EU-IPTICn. CSLflKIES SPIRAL GALAXIES t * * t â i i t t t t

GALAXY CLUSTER 012 05 24 00 -4 5 01!

F IE L D Z S 3 ESe/SERC PLATE J674S

X Y RR DEC L B Z IlS S O J 119501 IIBSOI 119501 115.824 -001.271 5 24 0.3 -45 1 46.1 250 45 41.6 -33 34 17.9 0.051

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 45 HRJBR A XIS 1 0 .3 0 SAMPLE POPULATION 115

SB 12 MINOR AXIS 9 .6 5 CORE POPULATION 52

S 55 ECCENTRICITY 0.35 LIMITING MAGNITUDE 19.0

SB 2 P0SN. ANGLE - 7 1 ,6 2

P 0

Figure 3.2.12 (J,g,h) Cluster Morphological Population Distributions. Table 8.2.12 Cluster Population Description.

GALAXY CLUSTER 012; 05 24 00 -45 01 : The cluster is located IB South-West quadrant of ESO/SERC Field 253. Within a diameter of 45mm as determined by mio we count 168 galaxies in this cluster and 115 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type I due to its in­ herent irregularity; we note a general scatter of the member galaxies with a single concentration South of the cluster center. The Cluster Catalogue 98 §3.2

We count 38 galaxies brighter than + 2 and thus classify the cluster as having an Abell richness of 0. We suggest a B — M type HI classification for the cluster which has no dominant galaxies in the field, but just an enhancement of the number of galaxies over and above the nominal field density. For mi,mg, and fWio we give 14.1, 15.1 and 15.2,respectively. The value of mio implies a redshift of 0.061.

The cluster member galaxies are scattered throughout the measured region with a concentration South of the cluster center and an enhancement in the third quadrant. The cluster density distribution suggests a ’’U-shaped” grouping in the region of highest galaxy surface density.

The cluster magnitude distribution is practically flat, with a few bright galaxies in the tail of the range rising in number to a plateau after m^ = 16.5 and continuing to the faint limit. The position angles of the brighter galaxies appears to be con­ centrated in the negative sense with the majority of the population having position angles West of North. We note two peaks in the distribution, one at zero degrees, that is, running North-South, and another at fifty degrees, or to the North-West.

We find the cluster to be somewhat spiral rich with an {E : SO : S) ratio of (l.O : 0.3 :1.2). Whereas the elliptical galaxies appear to be concentrated in an area South and East of the cluster center, the spirals appear in greater numbers South of center with relatively few North of center. The core population, where 45% of the galaxies reside, is located in an area of some 0.11 square degrees. This yields a surface density of 475 galaxies per square degree within the dispersion ellipse.

We notice several pairs of elliptical galaxies composed of an early and late member such as found at z == —99.4, y = —3.9 and x = —109.4, y = —2.9. The Cluster Catalogue 99 §3.3

GALAXY CLUSTER 013 06 21 39 - 6 4 56

/ *

Figure 8.2.18 (a) Field of GALAXY CLUSTER OIS: 06 21 SQ -64 56 T ie Cluster Catalogue 100 §3.2

GALAXY CLUSTER 013 06 21 39 - 6 4 56

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY OISTR1BUTI0N •0.

41. o m. I

It. , E £

-4.

IBGENVic = ■ ; 80= • 6 — * i SB= • ; •4X1. EAST EASTMM WEST 8 e p e g 8 2 L # # mikm. i.ssa^s

CLUSTER MAGNITUDE DISTRIBUTION POSITION ANGLE DISTRIBUTION 100.

•0. 22. eo. 19. ■w. 18.

IS. t CfUNT9 PER irrm 13. ^

40,

30. 6. a 2 0 .

10. 0, o m o u, o o u, o TÆTA (DECREES) S 8 i S S @822 2 2 8 2 22? 2

Figure 3.2.IS (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 101 §3.2

CnuHXT CLU5TQI D13 06 21 S3 -M 56 CBLBXÏ CLUSTER 013 06 21 39 -69 56 CFlflXT CLUSTER 013 05 21 39 -69 55

i i

ELLIRTICRL GSLBXIES 9B CPLPXIES

GALAXY CLUSTER 013 06 21 39 -64 56

FIELD 0B7 ESB/SERC PLATE J9299

X Y RA DEC L B z lia s o i (IB5DI IIBSOI iia s o i 083.921 009.016 6 21 39.4 -64 56 34.9 274 42 10.3 -27 29 35.5 0.038

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 52 MAJ0R AXIS 17.95 SAMPLE P0PULATI0N 163

80 28 MINOR AXIS 15.73 CORE P0PULATI0N 65

S 66 ECCENTRICITY 0.48 LIMITING MAGNITUDE 19.0

SB 12 P0SN. ANGLE 8 1 .11

P 5

Figure 3.2.13 Cluster Morphological Population Distributions. Table 8.2.13 Cluster Population Description.

GALAXY CLUSTER 018: 06 21 39 -64 56 : The cluster is located in North-West quadrant of ESO/SERC Field 087. Within a diameter of 90mm as determined by mio we count 163 galaxies in this cluster, all of which are measured to a limiting magnitude of mum = 19.0. The cluster is classified Abell type R because of its uniform distribution of surface density which appears to smoothly diminish radially from the cluster center. The Cluster Catalogue 102 §3.2

We count only 25 galaxies brighter than ms + 2 and thus classify the cluster as having an Abell richness of 0. We suggest a B — M type Ü-III classification for the cluster which has an intermediate population with only a single dominant galaxy which appears to be a normal giant elliptical. For mi,m 3 , and mio we give 12.9, 13.2 and 14.7,respectively. The value of mio implies a redshift of 0.038.

The cluster appears to be relatively smooth in its distribution with few con­ centrations, the density gradually decreasing radially form the cluster center. The ■urface density has a few spots where galaxies congregate in shghtly higher num­ bers, but this is due in part to what appears to be, for example, an elliptical galaxy lurrounded by faint attendants as we find at z = -103.6, y = 3.8.

We find a somewhat symmetrical distribution of magnitudes in the cluster reminiscent of a “bell-shaped” spread rising from the brightest cluster members to a peak near m„ = 16.0 and tapering off to m„ = 18.5 with very few measured faint galaxies near the magnitude limit. The position angle distribution shows a preference for the brighter galaxies to lie inclined to the North-East whereas there is a relative sparsity found to be inclined to the West of North. The positions of elliptical galaxies are scattered throughout the cluster but with a preference for the second and third quadrants. The spirals, on the other hand appear to have a slightly larger population in the third and fourth quadrants. The cluster is spiral rich with an {E : SO : S) ratio of (1.0 : 0.5 : 1.5). We find a core population representing nearly 40% of the membership within an area of 0.31 square degrees. On the sky, this represents a surface density of 209 galaxies per square degree.

Several pairs of superposed galaxies are noted with an early and a late elliptical as that found at z = —65.5, y = 23.9. Some of the spirals appear distressed and/or superposed and we note a at z = —81.7, y = —25.4 which displays a thin diffuse bar with concentrations at its poles. The Cluster Catalogue 103 §3.2

GALAXY CLUSTER 014 06 25 02 - 5 3 39

M I : : 1 t I 1 I , I 1 j 1 I I I 1 1 M 1 j I 11 1 I I I 1 I I I I I 1^! I I 1 'M l 1 I I ! I N] i * I 1 I i JT'r['l 1 I IJ j I I y 1 11 I 1 I

•

♦ : ' . W . . • . * » » .

♦ •» - *• * , - . ♦ . • m -tik: ; •• * ■'..' , , . - w

T» . : . .

54 !L • ' fc * /

. T- • r . .0 • * * :>■ i J . :

Figure S.2.14 (a) Field of GALAXY CLUSTER 014: 06 25 02 -5S S9 T ie Cluster Catalogue 104 §3.2

GALAXY CLUSTER 014 06 25 02 - 5 3 39

SURFACE DENSITY DISTRIBUTION CLUSTER MEMBERSHIP AND H0RPH0L0GY t».

110. m.

#0. LEGEND

S 0 = • i 4C. m. MM &EST g e 8 S I = S R S

CLUSTER MAGNITUDE DISTRIBUTION POSITION ANGLE DISTRIBUTION 25. 24. •0. eo.

TO.

15. dUMrS f t? 3ECT#R 13.

90. 20.

10.

TÆTfi (DECREES) ; ^ : 3 :

Figure 8.2.14 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. Tie CJuster Catalogue 105 §3.2

GALAXY aUSTER OH 06 25 02 -53 39 6 GALAXY CLUSTER OH 06 25 02 -53 39 6 GALAXY CLUSTER OH 06 25 02 -S3 39 B

ii

% • •

SPIRAL GALAXIES

t t < < < < < < I i i i

GALAXY CLUSTER 014 06 25 02 -5 3 39$

FIELD 161 ESB/SERC PLATE JES3B

X Y RA DEC L B z (19S0I tISSOI (taSOI [195DI 088.653 070.926 6 25 2.5 -53 39 26.8 252 21 36.2 -25 11 15.9 0.099

MORPHOLOGY DISPERSI0N ELLIPSE CLUSTER MEMBERS

E 109 MAJOR AXIS 1 0 .3 0 SAMPLE POPULATION 232

50 20 MINOR A XIS 9 .1 3 CORE POPULATION 79

5 98 ECCENTRICITY 0.46 LIMITING MAGNITUDE 19.0

SB 4 P0SN. ANGLE - 8 6 . 7 2

P 1

Figure 3.2.14 (f,g,h) Cluster Morphological Population Distributions. Table 8.2.14 Cluster Population Description.

GALAXY CLUSTER 014; 06 25 02 -53 39 : The cluster is located in North-West quadrant of ESO/SERC Field 161. Within a diameter of 45mm as determined by mxo we count 239 galaxies in this cluster and 232 to a limiting magnitude of miim = 19.0. The cluster is classified Abell type R because of its fairly uniform distribution of galaxies.

We count over 100 galaxies brighter than m 3 + 2 and thus classify the cluster The Cluster Catalogue 106 §3.2 as having an Abell richness of 2. We suggest a, B — M type I classification for the cluster which has a dominant centrally located cD galaxy with an apparent double nucleus and a corona. Form i,m s, and mio we give 12.9,15.0 and 15.4, respectively. The value of mio implies a redshift of 0.049.

The cluster appears centrally condensed with a smooth distribution decreasing radially from the center. There is, however, a slight concentration North-East of center where we find a slightly enhanced group of elliptical galaxies.

The magnitude distribution rises gradually from about m„ = 14.5 to m„ = 17.0 where it tapers off to a nearly flat plateau. For the position angle distribution, we find no aparent preference for orientation and have nearly the same number of galaxies oriented North-East as we have oriented North-West.

We find the positional distribution of elliptical and spiral galaxies to be similar and somewhat oriented North-South. The {E : SO : S) ratio is (1.0 ; 0.2 ; 0.9) giving a somewhat similar population of ellipticals and spirals. The core population holds 34% of the cluster membership in an area of some 0.10 square degrees. This yields a surface density of 763 galaxies per square degree. We note that the dis­ persion ellipse is nearly oriented North-South which agrees well with the apparent distribution of elliptical and spiral galaxies.

Aside from the remarkable cD galaxy with an apparent double nucleus and corona, we note several complicated spiral galaxies that are centrally condensed and have ring-like structures as, for example, one found at z == —79.3, y = 66.9. The Cluster Catalogue 107 §3.2

GALAXY CLUSTER 015 06 26 25 - 5 4 22

I I t I i I 1 1 I 1 1 I I

: ...

, r - ^ : V - - - . V . ..

% # " ' * ' " - - ^ %

: * . - ¥ .■ I*: ♦ . ' » . If . # * * . v

% . •• # ♦ « • * •

♦. s - ■ Ï ; T '

Figure 8.2.15 (a) Field of GALAXY CLUSTER 015: 06 86 85 -54 88 Tie Cluster Catalogue 108 §3.2

GALAXY CLUSTER 015 06 26 25 - 5 4 22

SURFACE DENSITY DISIRIBUTI0N CLUSTER MEMBERSHIP AND M0RPH0L0GY •0. . tl. .1 r. m. = E M.

(f.

X. L£GEND- I = • "I S 0 = ♦ -e. B * * 8B= »

EAST m NEST '"Ifcc'-"

CLUSTER MAGNITUDE DISTRIBUTION PO SITIO N ANGLE D ISTRIBU TIO N 100. Z5. eo. 22.

80. 70. !S: % : 16. g - 15. S - 11. =- 13. 12. E - I I . E .

90. 6. a ZD.

10.

o w . = ^ „

Figure 8.2.15 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 109 §3.2

ca.nrr ausTER dis os zs zs -54 zz Cn.RTT CLUSTER 015 06 Z6 Z5 -54 ZZ GBLRXT CLUSTER 015 OS Z6 25 -54 22

I

i i

I ELLIPTIC». CR.BXIES t

GALAXY CLUSTER 015 06 26 25 -54 22

PIELO 161 ESe/SERC PLB7E JSS3S

X RA DEC L B ZY tlBSai (19501 (19501 (19501 076.713 032.793 6 26 25.1 -54 22 29.4 263 10 56.4 -25 8 49.3 0.048

MORPHOLOGY DISPERSION ELLIPSE CLUSTER MEMBERS

E 8 9 MAJOR AXIS 1 0 .5 5 SAMPLE POPULATION 235

SO 14 MINOR AXIS 8 .6 7 CORE POPULATION 90

S 127 ECCENTRICITY 0.57 LIMITING MAGNITUDE 19.0

SB 4 P0SN. ANGLE 2 1 .0 6

P 1

Figure 8.2.15 (f,g,h) Cluster Morphological Population Distributions. Table 8.2.15 Cluster Population Description.

GALAXY CLUSTER 015; 06 26 25 -54 22 : The cluster is located in North-West quadrant of ESO/SERC Field 161. Within a diameter of 45mm as determined by mio we count 247 galaxies in this cluster and 235 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type R because of its regular appearance and smooth radial distribution of galaxies outward from a rather dense core. The CJuster Catalogue 110 §3.2

We count 85 galaxies brighter than m 3 + 2 and thus classify the cluster as having an Abell richness of 2. We suggest a B — M type II classification for the cluster which has a dominant elliptical galaxy somewhat intermediate between a cD class galaxy and a normal giant elliptical. For mi,m 3 , and mio we give 14.3, 14.7 and 15.3, respectively. The value of mio implies a redshift of 0.048.

The cluster membership form a dense, rich and diverse cluster. There is an obvious central condensation to the cluster with several concentrations South-East of the cluster center. The core of the cluster appears somewhat elongated and "dumbeir shaped.

The magnitude distribution rises rapidly from the relatively few very bright galaxies to a plateau near m„ = 16.0 then rises to another peak near m„ = 18.0 after which it falls off.

Position angles for the brighter galaxies are distributed about equally in both the positive and negative sense, with a slight peak near +30°, that is to the North North-East.

We find the cluster center dominated by elliptical galaxies, with the spirals, on the other hand, scattered throughout the cluster-at-large. The [E : SO : 5) ratio is (1.0 : 0.2 :1.5) making this a spiral-rich cluster. The core population represents some 38% of the sample population and is located in an area of 0.10 square degrees. This yields a core surface density of 894 galaxies per square degree.

We note that the mi, m 3, and miO brightest galaxies are elliptical galaxies, all possessing a corona. Other ellipticals are seen with coronae as well. Several superpositions occur, for example at z = —84.1, y = 45.6, where we find a spiral- elliptical combination. Tie Cluster Catalogue 111 §3.2

GALAXY CLUSTER 016 12 51 41 -2 8 44

lL‘J ^mmmMm

1 I ! I ! - ! ± - ‘ ! , t t

Figure 3.2.16 faj Field of GALAXY CLUSTER 016: IS 51 41 -28 44 T ie Cluster Catalogue 112 §3.2

GALAXY CLUSTER 016 12 51 41 - 2 8 44

SURFACE DENSITY DI5TRIBUTI0N CLUSTER MEMBERSHIP AND M0RPH0L0GY

CLUSTER MAGNITUDE DISTRIBUTION POSITION ANGLE DISTRIBUTION 2 S . 2 9 .

BO. 2 2 .

8 0 . 1 9 . 1 6 . 7 0 . 1 7 .

1 5 . cwira ftp SECin

10.

TtETfi I DEGREES] o in o in a ÜP'W'% o in o in o {5:5:5

Figure 8.2.16 (b) Cluster Morphology, (e) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 113 §3.2

COLHXY CLUSTER 016 12 51 41 -28 « GfUXY CLUSTER 016 12 51 41 -28 44 (SLBXY CLUSTER 016 12 51 41 -26 44

3

SPIRflL GALAXIES

< ♦ * ? f < < M ? » < ♦ ♦ Ç < ? » ? ? I I .

GALAXY CLUSTER 016 12 51 41 -28 44

FIELD 442 ESe/SERC PLBTE J5 7 6 0

X Y RH DEC L B Z I1S53I (I9SQI CIBSDI (ISSCl IQG.553 055.348 12 51 41.2 -28 44 33.4 303 42 32.9 33 51 13.3 0.048

MORPHOLOGY DISPERSION ELLIPSE CLUSTER MEMBERS

E 175 MAJOR A X IS 1 0 .2 9 SAMPLE POPULATION 34 8

S0 45 MINOR AXIS 6.26 CORE POPULATION 145

5 121 ECCENTRICITY 0.60 L IM IT IN G MAGNITUDE 1 9 .0

SB 7 P0SN. ANGLE 8 2 .4 4

P 0

Figure 3.2.16 (f,g,h) Cluster Morphological Population Distributions. Table 3.2.16 Cluster Population Description.

GALAXY CLUSTER 016: 12 51 41 -28 44 : The cluster is located in North-East quadrant of ESO/SERC Field 422. Within a diameter of 45mm as determined by mio we count 420 galaxies in this cluster and 348 to a limiting magnitude of mum = 19 0. The cluster is classified Abell type RI because of its linear core with fairly large extended scatter. There is a suggestion of the superposition of two clusters. The Cluster Catalogue 114 §3.2

We count 8 6 galaxies brighter than m 3 + 2 and thus classify the cluster as having an Abell richness of 2. We suggest a possible B — M type II: classification for the cluster which appears to have several bright elliptical galaxies intermediate in appearance between the class cD and normal giant ellipticals. For m i,m 3 , and Wio we give 12.9, 14.5 and 15.2, respectively. The value of mio implies a redshift of 0.048.

The cluster membership appears to be aligned preferentially North-South, giv­ ing the core of the cluster an almost linear appearance. We note a strong concen­ tration just South of center and a smaller one, somewhat isolated, North of the cluster center.

The cluster magnitude distribution rises rapidly with increasing magnitude range till about = 17.0 where there is a change in slope, rising once more, but not as steeply. The position angles of the brighter galaxies seem to concentrate in the negative sense, that is, to the North-West with a dominant peak at approximately —45 degrees.

The cluster is dominated by a somewhat linear distribution of elliptical galaxies. We find the [E : SO : S) ratio to be (1.0 : 0.3 : 0.7) with the ellipticals densly occupying the cluster core. The spirals are more evenly distributed, but have their concentrations as well, the major one being quite near the cluster center. The dense core of the cluster contains some 42% of the population within an area of 0.09 square degrees. This yields a core surface density of 1549 galaxies per square degree.

The cluster contains an obvious subgroup centered on a elliptical galaxy at

X = 146.5, p = 61.6. This subgroup appears to be composed primarily of elliptical galaxies. We also notice several pairs of galaxies, the pairs formed by an early and a late elliptical as found at z = 147.0, y = 60.3. T ie Cluster Catalogue 115 §3.2

GALAXY CLUSTER 017 13 03 25 -3 7 18

Figure 8.2.17 (a) Field of GALAXY CLUSTER 017: IS OS 25 -57 18 T ie Cluster Catalogue 116 §3.2

GALAXY CLUSTER 017 13 03 25 - 3 7 18

SURFACE DENSITY DI5TRIBUT10N CLUSTER MEMBERSHIP AND M0RPH0L0GY

-1 9 0 . E

èinr! 6 0 =

EAST ICST 68 8 8 8 8 S

CLUSTER MAGNITUDE D IST R IB U T I0N P 0 5 I T I 0 N ANGLE D I5T R IB U T I0N 100. so.

80 .

TO.

!Q # # 4 2 0 2 4 6 0 10 CfUNTS fO 9 C W

80 .

2 0 .

10.

HCNITUDE RANGE E TtCTfl fOECREESl W o I/) O 1/1 o • eeooeeoooeooooooeo o iC D o r» r“ {ci£ii/iin«*«*cncn 8 SRS 98882^588888^8 8

Figure 3.2.17 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 117 §3.2

CHJXY ausTER on 13 03 2S - 3 7 10 ghlrxy ausTER on 13 03 2s -3 7 is CBLRXY CLUSTER 017 13 03 25 -37 18

i i

SB GALAXIES SPIRBL CfiLRXlES ear « I

GALAXY CLUSTER 017 13 03 25 -37 18

riE L O 362 ESB/SERC PLATE J1 5 3 3

X Y RH DEC L B z (tssai IlSSOI (19501 (19S0I □95.233 -121.728 13 3 25.3 -37 17 59.G 306 10 10.3 25 12 41.6 0.049

MORPHOLOGY DISPERSION ELLIPSE CLUSTER MEMBERS

E 6 9 MAJOR AXIS 1 0 .4 8 SAMPLE PBPULRTIBN 181

S0 IB MINOR AXIS 8 .2 6 C0RE P0PULOTI0N 65

S 81 ECCENTRICITY 0.61 LIMITING MAGNITUDE 19.0

SB 12 P0SN. ANGLE - 1 9 . 0 1

P 1

Figure 3.2.17 (f,g,h) Cluster Morphological Population Distributions. Table 3.2.17 Cluster Population Description.

GALAXY CLUSTER 017: 13 03 25 -37 18 : The cluster is located in South-West quadrant of ESO/SERC Field 382. Within a diameter of 45mm as determined by mio we count 255 galaxies in this cluster and 181 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type i? because of its somewhat smooth distribution of galaxies and high central condensation.

We count 28 galaxies brighter than m 3 + 2 and thus classify the cluster as The Cluster Catalogue 118 §3.2 having an Abell richness of 0. We suggest & B - M type II classification for the cluster which has several bright elliptical galaxies with coronae that are intermediate between the class cD and normal giant elliptical galaxies. For and mio we give 13.2, 14.2 and 15.4, respectively. The value of mio implies a redshift of 0.049.

The cluster members form a distribution with several surface density concen­ trations. The highest concentration exists at the cluster center with less dense regions located South-West of center and North of center.

The magnitude distribution gently rises to an initial maximum at m„ = 17.0 then falls some thirty percent to a plateau near m„ = 18.5 and then rises once more to the limiting magnitude. The position angle distribution shows an enhance­ ment towards the North-East with peaks to the North-East, North and North-West respectively.

In the core of the cluster we find the elliptical galaxies somewhat aligned along the major axis of the dispersion ellipse and then scattered about the cluster with a diminished number towards the Western end of the cluster. Similar behavoir is found with the spiral galaxies which have a tendency to congregate in their greatest numbers South of the cluster center. We find an (E ; SO : 5) ratio of (1.0:0.3:1.3) making this a slightly spiral enriched cluster. The core population amounts to some 36% of the sample located in an area of 0.09 square degrees. This represents a surface density of 682 galaxies per square degree on the sky.

We note that the brightest five galaxies are classed as ellipticals having a corona. At least two of these brightest galaxies appear superposed. Also found in this cluster are several pairs of galaxies composed of an early and a late elliptical such as the one located at z = —Q8 .8 ,y = —126.9. The Cluster Catalogue 119 §3.2

GALAXY CLUSTER 018 14 GO 41 -3 3 44

Figure 3.2.18 (a) Field of GALAXY CLUSTER 018: I 4 00 4I -SS U T ie Cluster Catalogue 120 §3.2

GALAXY CLUSTER 018 14 00 41 - 3 3 44

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTI0N m t . . .

m . •9

110.

m.

00. E ; 0 n.

m. ♦ <5>- ? SO; «0 . .o* o' lUiltiliM.Hi.i.H 111 £ R S j EPST WEST

CLUSTER MAGNITUDE D IS T R IB U T I0 N P05ITI0N ANGLE DISTRIBÜT10N 100. 25. M. 23. 22. 21. I! IE. 10 « « 1 2 0 2 4 « « to II; i t«JNT3 KK m iR 13. ‘ so.! IÎ;! 10. I g;i l:\ l;i a. 2. 1. 0. 7>£TR I DECREES: W o in o lA o in o m o ui o > o o o o e eooeoo SBBSBgRBS E R S S g g g

Figure 3.2.18 (b) Clurter Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. Tie Ciuster Catalogue 121 §3.2

Ca.flXY CLUSTER 018 H 00 41 -33 44 CFlflXY CLUSTER 018 14 00 41 -33 44 CflflXY CLUSTER 018 14 00 41 -33 44

i # f #* V-

aH P T lC nt GALAXIES S0 GALAXIES

GALAXY CLUSTER 018 14 00 41 -33 44

FIELD 384 ESO/SERC PLATE J4BSI

X Y RR DEC L B Z i t e s o i ii9sai 119501 (18501 0 0 5 .2 2 3 069.735 14 0 40.6 -33 44 13.9 319 37 9.5 26 32 41.9 0. 020

M0RPH0L0GV DISPERSION ELLIPSE CLUSTER MEMBERS

E 165 HRJ0R A X IS 2 7 .6 5 SAMPLE POPULATION 444

S0 63 MIN0R AXIS 2 5 .6 3 C0RE P0PULATI0N 155

S 172 ECCENTRICITY 0 .3 8 L IM IT IN G MAGNITUDE 1 9 .0

SB SB P0SN. ANGLE - 8 . 0 7

P 8

Figure 3.2.18 (f,gjh) Cluster Morphological Population Distributions. Table 8.2.18 Cluster Population Description.

GALAXY CLUSTER 018: 14 00 41 -S3 44 : The cluster is located in the North-East quadrant of ESO/SERC Field 384. Within a diameter of 120mm as determined by mio we count 479 galaxies in this cluster and 444 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type RI due to the presence of several concentrations within the body of the cluster.

We count 24 galaxies brighter than ms +2 and thus classify the cluster as having T ie Cluster Catalogue 122 §3.2 an Abell richness of 0. We suggest a B —M type I classification for the cluster which has a dominant cD galaxy in its core. We note that the cD is rather elliptical and has a corona. For mi,ms, and mio we give 11.2, 12.6 and 13.3, respectively. The value of mio implies a redshift of 0 .0 2 0 .

The cluster membership is sparsely distributed over some 1000 mm^ and is has a relatively high central density. We note that the surface density is generally quite low except for the core where there is an elongated group of galaxies forming the highest concentration of galaxies in the cluster.

The magnitude distribution shows two peaks suggesting a bright population of galaxies that cuts off beyond m„ = 17.0 and perhaps a background population of many very faint galaxies near = 18.5. The position angle distribution shows a preference of the brighter galaxies to be oriented West of North with peaks in the

distribution near - 1 0 and -60 degrees.

We find the {E : SO : S) ratio to be (1 . 0 ; 0.4 : 1.3) showing an excess of spirals. The core population represents nearly SSoccupies an area of 0.78 square degrees. This yields a cluster surface density of 199 galaxies per square degree.

Several elliptical galaxies are seen in groups reminiscent of "chains” such as the set found at a: = —23.8, y = 112.9. Other groups of spirals or SO galaxies with faint elliptical companions are seen at, for example, x = 4.5, y = 104.1 or X = 38.3, y = 90.5. We find a large proportion of barred-spiral galaxies in the cluster, several with ring-like structures about the nucleus such as the object located at x = —18.5, y = 62.1. T ie Cluster Catalogue 123 §3.2

GALAXY CLUSTER 019 14 09 18 -3 2 50

Figure 8.2.19 (a) Field of G A LA X Y CLUSTER 019: U 09 18 -SS 50 Tie Cluster Catalogue 124 §3.2

GALAXY CLUSTER 019 14 09 18 - 3 2 50

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DI5TRIBUTI0N IW. m. 5 IK. I

MO.

no.

no. E £

n o . K ^ -.o 000. é«!!l •• t r LEGEND o #0. E - • 8 0 = • «0. I

EAST MH C 9 R 5 2 8 8 : P i«3Ti— ■ -

CLUSTER MAGNITUDE DISTRIBUTI0N P 0 S IT I0 N ANGLE D I5T R IB U T I0N 100.

■0. 2 2 .

80.

1 5 . d u n j r a s n m 13.

«I

90.

20.

10.

0. E THETfl (OeCREES) H „ WglTUDE ROtgE ooooceoeoeeeoooooo 882888822 = 28838822 8

Figure 8.2.19 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. r i e Cluster Catalogue 125 §3.2

CHLflXT CLUSTER 019 H 09 18 -32 SO CRLRXY CLUSTER 019 H 09 18 -32 50 CBLfiXT CLUSTER 019 11 09 10 -32 SO

i i

GALAXIES SPIRBL GALAXIES WST

GALAXY CLUSTER 019 14 09 18 -32 50

FIELD 3B4 ES0/5EHC PLATE J4B51

X Y RA DEC L B Z ItgSDI (19SDI HS50I (ISSOI 1 0 2 .1 4 8 117.241 14 9 17.9 -32 50 2.6 321 51 15.5 26 48 60.0 0.044

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 7 7 MAJOR AXIS 1 4 .3 6 SAMPLE POPULATION 238

S0 31 MINER AXIS 12.43 C0RE POPULATION 91

S 118 ECCENTRICITY 0.50 LIMITING MAGNITUDE 19.0

SB g P0SN. ANGLE - 4 6 . 5 1

P 3

Figure 8.2.19 (f,g,h) Cluster Morphological Population Distributions. Table 8.2.19 Cluster Population Description.

GALAXY CLUSTER 019; 14 09 18 -82 50 : The cluster is located in the North-East quadrant of ESO/SERC Field 384. Within a diameter of 60mm as determined by mxo we count 265 galaxies in this cluster and 238 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type I because of the high degree of scatter.

We count 64 galaxies brighter than m 3 + 2 and thus classify the cluster as The Cluster Catalogue 126 §3.2

having an Abell richness of 1 . We suggest a B — M type III classification for the cluster which has no significantly dominant galaxies. For mi,m 3 , and mio we give 14.3,14.8 and 15.2, respectively. The value of mio implies a redshift of 0.044.

The cluster appears to have several concentrations not located near the cluster center: the most dense lies East of center while another lies North-East of center. There are other smaller condensations scattered throughout the cluster.

The magnitude distribution rises slowly from the brightest galaxies to those at m„ = 17.5 after which the slope changes, rapidly rising to fainter magnitudes. Position angles seem to be concentrated East of North, in the positive sense, with peaks in the distribution near zero and forty-five degrees.

The elliptical galaxies appear to be scattered throughout the cluster with a slight concentration in the core, especially in the second quadrant. Likewise, the spirals concentrate in the core with a similar enhancement towards the North-East.

We find the {E : SO : S) ratio to be (1.0 : 0.4 : 1 .6 ) suggesting a spiral-rich cluster.

We note that the core population comprises some 38% of the sample within an area of 0.19 square degrees. This yields a core surface density of 463 galaxies per square degree.

The great diversity of spiral galaxies in the cluster gives rise to the discovery of several peculiar members. What appears to be a barred- spiral with concentrations at the poles of the bar can be found at z = 84.7, y = 122.1. Another peculiar object lies at z = 79.3, y = 104.9, and appears as an “exclamation point” with a fine whisp. T ie Cluster Catalogue 127 §3.2

GALAXY CLUSTER 020 14 09 28 -3 4 01

J I I I I ! I M I I i I I I I i I I I n I I I I I I I I i I I I I I I I I I I I I I I i I I I I 1 I I I I 1 I I I I I I I I I I I I I I I I I I I M W I I ( I M I I ; n —

E ^ ^ • • • : • _

#

m m m L W . : 1 -1.1:

i

Figure 3.2.20 faJ Field of GALAXY CLUSTER 020: U 09 28 -S4 01 T ie Cluster Catalogue 128 §3.2

GALAXY CLUSTER 020 14 09 28 - 3 4 01

SURFACE DENSITY DISTRIBUTI0N CLUSTER MEMBERSHIP AND M0RPH0L0GY lie .

M. 5 M. I

V.

0« i o o «4.

e .

ERST ÆST S 8 S. g ? # P ?

CLUSTER MAGNITUDE DISTRIBUTI0N P 0 5 I T I 0 N ANGLE D IS T R IB U T I0N 100. 25. 2 4 .

n . 22. so. 20. 1 9 . 10. TO. 1 7 .

1 5 . CWdS rtn SCTB 'I 13. " -

40,

90. 7. ».

20 .

10 .

0. {JRGN^nœ RgCE^ THE TP lOECREES) oimDt.^r.'iotouiin.' in iri cO rO

Figure 3.2.20 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 129 §3.2

Cn.RXT CLUSTER 020 H 09 28 -34 01 CRLflXY CLUSTER 020 14 09 28 -34 01 CRLflXT CLUSTER 020 14 09 29 -34 01

3

a i

I

# # $ # f ; I f * f # $ f f ^ I f f f f f 4 ( i 1 f ^ f *

GALAXY CLUSTER 020 1 4 0 9 2 8 ■34 0 1

FIELD 364 tS e/S E K C PLATE J4SS1

X Y RR DEC L B Z (ISSOI 119561 IIBSO! 119501 102.819 053.059 14 9 28.3 -34 1 38.5 321 26 22.7 25 40 56.0 0.038

M0RPH0L0GY d : s p e r s ] 0 n e l l i p s e CLUSTER MEMBERS

E 53 MBJ0R AXIS 14.68 SAMPLE P0PU LA TI0N 219

30 17 MIN0R AXIS 12.21 C0RE P0PULATI0N 75

S 140 eccentricity 0 .5 5 LIMITING MAGNITUDE 19.0

SB 7 P0SN. ANGLE - 1 2 . 1 6

P 2

Figure 3.2.20 (f,g,h) Cluster Morpkological Population Distributions. Table 3.2.20 Cluster Population Description.

GALAXY CLUSTER 020: 14 09 28 -34 01 : The cluster is located in the North-East quadrant of ESO/SERC Field 384. Within a diameter of 60mm as determined by mio we count 238 galaxies in this cluster and 219 to a limiting magnitude of miim = 19.0. The cluster is classified Abell type RI because of its scattered, somewhat irregular appearance.

We count 61 galaxies brighter than ms+2 and thus classify the cluster as The Cluster Catalane 130 §3.2

having an Abell richness of 1 . We suggest a B — M type II classification for the cluster which has a number of bright galaxies intermediate between the type cD and normal giant elliptical galaxies. For and mio we give 12.7, 14.5 and 14.8, respectively. The value of mio implies a redshift of 0.038.

The cluster shows a slight central condensation of the core with several small concentrations, somewhat less dense than that found West of center. We find the magnitude distribution to be ramp-like from brightest to faintest in a practically uniform rise. Position angles tend to lean East of North with a few concentrations a t 0, 30 and 50 degrees, respectively.

The elliptical galaxies appear more frequently in the Southern portions of the cluster with a slight enchancement in the core. On the other hand, the spirals are fairly uniformly scattered throughout the cluster. We find an (E : SO : S) ratio of (l.O : 0.3 : 2.8) giving a spiral-rich cluster.

The core population comprises some 34% of the sample in an area of 0 . 2 square degrees. This gives a surface density of 380 galaxies per square degree on the sky.

We call attention to a peculiar triplet of galaxies located at z = 98.7, y = 53.6 that appear to be superposed. Another superposition reminiscent of an "exclama­ tion point”, of a lenticular and an elliptical, is found at x = 108.4,y = 46.3. Also noted are pairs of galaxies consisting of an early and a late elliptical, such as the set residing at z = 82.0, y = 46.1. The Cluster Catalogue 131 §3.2

GALAXY CLUSTER 021 14 30 26 -31 33

TTTTTT

Figure S.2.21 (aj Field of GALAXY CLUSTER 021: U SO 26 -SI SS Tie Ciuster Catalogue 132 §3.2

GALAXY CLUSTER 021 14 30 26 -3 1 32

SURFACE DENSITY DISTRIBUTI0N CLUSTER MEMBERSHIP AND M0RPH0L0GY

@ 2 •uo. tëï£ e s •ÎK. -O tml?.

£RST «CST e 8 8 S 8Ê 8 S 8

CLUSTER MAGNITUDE OISTRIBUTI0N P05ITI0N ANGLE DISTRIBUTI0N 100.

M. 2 2 .

8 0 .

TO. 15.2 ■ n. = ■ o m rr? h k s u m 13. 5 0. 12, S

IQ.

9 0 . B. S *

2 0 .

1 0 .

0 . •«GNITUE RfMGC T « T fl !0ECR££SJ 0«90(/>oinoi^oinouioi/)omomo e 8

Figure 8.2.21 (b) CluBter Morphology, (e) Surface D entity Distribution, (i) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalane 133 §3.2

C T .R « [LUSTER 021 » 30 26 -31 32 CB.BXT OUSTER 021 11 30 26 -31 32 CRLflXT OUSTER 021 11 30 26 -31 32

3

i

GALAXY CLUSTER 021 14 30 26 -31 32

riELO ♦ 47 ES0/SERC PLBTE J H 7 Z

X Y RA DEC L B Z ItCSOJ iiesQi (iBsai 119501 - 0 4 3 . 9SS -081.811 14 30 26.3 - 31 32 4 0 .5 32 7 1 2 8 . 9 26 17 3 3 .7 0. 054

M0RPH0L0GY DISPERSI0N ELLIPSE CLUSTER MEMBERS

E 6 3 HAJ0R AXIS 10.96 SAMPLE P0PULATI0N 150

S0 20 MIN0R AXIS 8 . 14 CBRE P0PULATI0N 58

s 61 ECCENTRICITY 0 .5 5 L IM IT IN G MAGNITUDE 1 9 .0

SB 6 P0SN. ANGLE 2 8 .2 4

P 0

Figure 8.2.21 f/,ff,hj Clutter Morphological Population Dittributions. Tkble 8.3.31 Clutter Population Deteription.

GALAXY CLUSTER 021; 14 80 26 -81 8 8 : The cluster is located in the South-West quadrant of ESO/SERC Field 447. Within a diameter of 45mm as determined by fn%o we count 193 galaxies in this cluster and 150 to a limiting magnitude of muni = 19.0. The cluster is classified Abell type RI due to its reg­ ular appearance, and fairly smooth distribution of galaxies radially from the core. Whatever irregularities occur can probably be traced to a large concentration South of center. The Cluster C&tsJogue 134 §3.2

We count 13 galaxies brighter than ms + 2 and thus classify the cluster as having an Abell richness of 0. We suggest & B — M type E-in classification for the cluster which has no really dominant galaxies albeit several bright ellipticals which could not be considered giant. For mi,m 3 , and mio we give 12.1, 12.6 and 13.9, respectively. The value of mio implies a redshift of 0.054.

We find the cluster smooth with the exception of the fourth quadrant which has a paucity of galaxies. There is a strong concentration of cluster members just South of center, and a smaller group North of this. At the South-East extremity of the cluster we find another small concentration.

The cluster magnitude distribution rises somewhat linearly from brightest to faintest galaxies, with a noticable drop in population in the range m„ = 17.0 to niv = 17.5. The position angle distribution shows no preference for sense other than perhaps the peak at zero degrees indicating a North-South orientation.

We note the concentration of elliptical galaxies in the core, their scatter else­ where and their avoidance of the fourth quadrant. The spirals, on the other hand, Are more uniform in their distribution, are somewhat concentrated towards the cen­ ter of the cluster, and are also found at its periphery. The {E : SO : S) ratio is (1.0 : 0.3 : 1.0) suggesting a nearly evenly divided population of ellipticals and spirals. The core population comprises nearly 89% of the sample and is found in an area of 0.11 square degrees. The core surface density is thus some 526 galaxies per square degree on the sky.

We notice five pairs of elliptical galaxies comprised of an early and late member, the brightest of which is located at z = —42.3, y = —67.9. The dense galaxy concentration South of center has an unusual elliptical galaxy, centrally condensed and supporting a halo, that is surrounded by a very faint population of attendants. The Cluster Catalogue 135 §3.2

GALAXY CLUSTER 022 19 56 35 -3 8 33 1,, 1 U'li I nj 111 mu 111 n u 11 ui^rrrr^i : ; V J N T , : . • . » » ij ■ • ' ‘ ^ ® . .* ' j# . . • . .% - a

, ......

î s m ï f

F ig u re 3.2.22 FieW of G A L A X Y CLUSTER 022: 19 56 S5 -S8 SS T ie Cluster Catalogue 136 §3.2

GALAXY CLUSTER 022 19 56 35 - 3 8 32

CLUSTER MEMBERSHIP AND M0RPH0L0GY

tao. E I2B. I <3® *XL" n- -=s_^. - ^ MO. 0 ”o ■■ft mui is3

Ot 0 Kkii &!«. * . hr::: to. }■*:..

m. .1 lU tN i ltU U m u i< iiii« H .n l^in l«tti m i i M 111 II EnST W NEST

CLUSTER MAGNITUDE DISTRIBUTI0N P 0 5 I T I 0 N ANGLE D IS T R IB U T I0N 100

90. 22.

20. e

15.

13. “>

o in o « o e> m o u> o

Figure 3.2.22 (b) Clutter Morphology, (c) Surface Dentity Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster CaWogTie 137 §3.2

omn ausTER ozz 19 ss 35 -as 3z CHJXY aUSTER 022 19 56 35 -38 32 CBLBxr CLUSTER 022 19 56 35 -3 9 32

m*

*EmPïicw..g3Li«its» SPIRRL GALAXIES

*

GALAXY CLUSTER 022 3 9 56 35 -38 32

FIELD 339 ESa/SERC PLATE J2 3 7 6

X Y RP DEC L B H (tSSOl (19501 I105DI (19SDI 003.581 080.398 19 56 35.4 -38 32 47.9 002 3 26.0 -29 14 54.4 0.025

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 2 2 0 MPJ0R AXIS 28.60 s a m p l e POPULATION 458

S 0 5 8 MIN0R AXIS 25.89 C0RE POPULATION 157

S 137 ECCENTRICITY 0.43 LIMITING MAGNITUDE 19.0

SB 31 P0SN. ANGLE 4.55

P 12

Figure S.2.22 (f,g,h) Cl%tter MorpkologieaJ Population Diftrihutions. Table 8.3.32 Cluater Population Detcription.

GALAXY CLUSTER 022; 19 56 85 - 8 8 8 8 : The cluster is located in the North-East quadrant of ESO/SERC Field 339. Within a diameter of 90mm as determined by mio we count 493 galaxies in this cluster and 458 to a limiting magnitude of m y.m = 19.0. The cluster is classified Abell type I due to the paucity of galaxies found South of center, giving a nonuniform radial distribution.

We count 80 galaxies brighter than ms +2 and thus classify the cluster as having T ie Cluster Catalogue 138 §3.2 en Abell richness of 2. We suggest a B — M type I-II classification for the cluster which has a dominant cD type galaxy as well as a number of giant ellipticals. For and mjo we give 15.4,15.8 and 16.1,respectively. The value of mxo implies a redshift of 0.026.

This cluster is spread out over a region in excess of lOOOmm^ and is sparsely populated. We note a slight concentration of galaxies South of the cluster center as well as several small concentrations North-West of center. The magnitude dis­ tribution is somewhat bifurcated showing a fairly rapid increase of population from the brightest to = 16.5 then dropping rapidly only to rise quickly to near the limiting magnitude. Given the size of the cluster, one might assume that the second peak represents a background population of galaxies.

We find most of the elliptical galaxies scattered throughout the cluster, save for a virtually empty zone South of center. There appears to be a slight concentration of these in the region South of the cluster center. The spiral galaxies appear to be more uniformly distributed, save for the zone of avoidance. The {E : SO : S) ratio fives (1.0 : 0.3 : 0.8) implying a cluster marginally rich in elliptical galaxies.

The core population comprises nearly 34% of the sample contained in a area of 0.81 square degrees. This implies a surface density of 193 galaxies per square degree on the sky.

We note several groups composed of a spiral with what appears to be a number of faint attendant galaxies, for example, as that located at z = —40.4, y = 85.3. In addition there are several pairs of ellipticals consisting of an early and late member as is found, for example, at x = —1.9, y = 28.6. The Cluster Catalogue 139 §3.2

GALAXY CLUSTER 0 2 3 20 38 34 - 3 5 24

Figure 3.2.28 (a) Field of GALAXY CLUSTER OSS: SO S8 S4 -S5 Sf T ie Cluster Cataiogue 140 §3.2

GALAXY CLUSTER 023 20 38 34 -35 24

o u r r r n c c ocn^xtt oxotrxoutjbn CLUSTER MEMBERSHIP AND M0RPH0L0GY

I

3

LEGEND

""iScV"

CLUSTER MAGNITUDE DISTRIBUTI0N PBSITI0N ANGLE DISTRIBUTION 100. flO. eo.

TO.

cniTs rex s a »

90.

20.

10. V, •ÇNITl^ RRN% ^ E THETB IDEOREES) H

; 2 ; d ; ; ; : : : H H ; H : ;

Figure 8.2.23 fbj Clutter Morphology, (c) Surface Dentity Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 141 §3.2

CanXT aUSTER 0Z3 ZD S8 M 24 CUXI auSTER tea 20 38 M -3 5 24 capxt aUSlER 0Z3 20 38 34 -35 24 I A

i * 1 ELLlPTJCa. CflLRXm SPIRAL GALAXIES •BT ## mv mmr m OBT m * t i < i t i t i t i » t t * * * » i Î t i t t i

GALAXY CLUSTER 023 2 0 38 34 -35 24

FIELD 401 Cse/SERC PLATE J61D9

X Y RR DEC L B z I1D 50I (lasoi IIBSOJ (ISSOI -IDS. 191 -022.45B 20 38 34.4 -35 23 58.1 007 43 35.8 -36 50 15.1 0 .0 6 5

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 2 3 5 MRJ0R A X IS 8 .1 2 SAMPLE POPULATION 334

80 32 MIN0R AXIS 7.43 CORE p o p u l a t io n 109

S 64 ECCENTRICITY 0.40 LIMITING MAGNITUDE 1 9 .0

SB 2 P0SN. ANGLE - 2 1 . 5 2

P 1

Figure 8.2.38 (f,g,h) Clatter Morphologicd Population Dittrihutiont. Table 8.2.28 Cluster Population Description.

GALAXY CLUSTER 028: 20 8 8 84 -85 24 : The cluster is located ia the South-West quadrant of ESO/SERC Field 401. Within a diameter of 36mm as determined by rtiio we count 651 galaxies in this cluster and 334 to a limiting magnitude of rniim = 19.0. The cluster is classified Abell type R due to its inherent regularity.

We count 65 galaxies brighter than m, + 2 and thus classify the cluster as T ie Cluster Catalane 142 §3.2 having an Abell richness of 1. We suggest a B — M type HI classification for the cluster which has no dominant galaxies in the field. For and nj^o we give 15.3,15.8 and 16.1, respectively. The value of mio implies a redshift of 0.065.

This rich cluster shows a dense concentration of galaxies with a radial popula­ tion fall-off and several dense subgroups. The main subgroup is located somewhat East of the cluster center with another concentration lying South of it. A similar group is found just South of center. We note also the presence of another very dense nbgroup to the East North-East at the periphery of the cluster.

The magnitude distribution rises nearly exponentially from the brightest galax­ ies to the magnitude limit with the majority of the cluster members being fainter than = 17.5. We note that the position angle distribution displays a greater number of bright galaxies oriented W^est of North in the negative sense, with a not- icable excess at zero degrees. We note the heavy concentration of elliptical galaxies distributed throughout the cluster, whereas the spirals are fewer in number and riiow no obvious grouping. The (E : SO : S) ratio favors the elliptical galaxies and fives (1.0 : 0.1: 0.3).

The core population represents some 33% of the sample population but since this cluster is so rich with faint galaxies, we must view this number with caution. The dispersion ellipse spans 0.07 square degrees on the sky giving a core density of 1641 galaxies per square degree.

The rich core density may be further enhanced if we count the faint galaxies th at comprise the population fainter than = 19.0. We note 16 pairs of galaxies in very close proximity or superposed, the brightest of which is located at z = —99.7, y = —13.2. These are generally pairs of elliptical galaxies with an early and a late member. T ie Cluster Catalane 143 §3.2

GALAXY CLUSTER 024 20 48 41 - 5 2 08 j i iiu ix i4 _ 4 i 11II1 lyi 1 iTi 1 rjTjT

••

• ••

Figure 3.2.24 {aj Field of GALAXY CLUSTER 0S4: SO 48 4I -58 08 The Cluster Catalogue 144 §3.2

GALAXY CLUSTER 024 20 48 41 - 5 2 08

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTI0N -TO,

410. 0 o f Î Ï

E PST WEST m 8 8 8 8 S 9 s

CLUSTER MAGNITUDE O IS T R 1B U T I0N P05ITI0N ANGLE DISTRIBUTION lOO, 25. 23.24. 22. 21. 2 0 . g|-

70.

1 5 . L I to « 4 4 2 0 2 4 6 0 10 H. = COUNT? fOt XCTV 13. ' l?;i 10. I 8 . ; 8. : i;S a. 2. I. ± i— ^ 1 I I I- 1 ] THETA (DECREES) W OV)O V>O iPOffCNITUOE inO iAO RANGE O toooooeoeooo 8 8 P 8 S 8 RB ‘ 2 SRSSSP2

Figure 8.2.24 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalane 145 §3.2

COflXT CLUSTER 024 20 48 41 -52 08 CPLRXT CLUSTER 024 20 48 41 -5 2 08 C n L R IT CLUSTER 024 20 48 41 -52 08

i 1

ELLIPTICAL GALAXIES GALAXIES SPIRAL GALAXIES B B T m K 3 I t tététisiiit

GALAXY CLUSTER 024 20 48 41 ■52 08

FIELD 235 ESB/SERC PLATE J33B5

X Y RR DEC L B Z CIOSOI 119501 IIB 5 D I I19SQI - 0 9 5 .8 3 1 -115.415 20 48 40.7 -52 8 45.6 346 31 0.9 -39 25 40.1 0.037

MORPHOLOGY DISPERSION ELLIPSE CLUSTER MEMBERS

E 71 MAJOR AXIS 1 4 .2 1 SAMPLE POPULATION 179

SO 13 MINOR AXIS 1 2 .5 7 CORE POPULATION 65

S 7 9 ECCENTRICITY 0.47 LIMITING MAGNITUDE 19.0

SB 12 P0SN. ANGLE 6 . 4 7

P 4

Figure 8.2.24 Clutter Morphological Population Dittrihutions. Table 8.2.24 Cluster Population Description.

GALAXY CLUSTER 024: 20 48 41 -52 08 ; The cluster is located in the South-West quadrant of ESO/SERC Field 235. Within a diameter of 60mm as determined by mio we count 183 galaxies in this cluster and 179 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type I because of the level of inherent scatter of the cluster members.

We count 64 galaxies brighter than + 2 and thus claissify the cluster as OcO

T ie Cluster Cataiogue 146 §3.2 having an Abell richness of 1. We suggest a B — M type III classification for the cluster which has no dominant galaxies in the field. For mi,ms, and mio we give 13.2, 13.7 and 14.9, respectively. The value of mio implies a redshift of 0.037.

We find the general characteristics of the cluster to be somewhat irregular with a slight concentration of galaxies immediately South-East of the cluster center, an­ other loose aggregate North of center and a sparse scattering of galaxies throughout the rest of the cluster. The cluster magnitude distribution rises rapidly from the brightest galaxies to a slight excess at m„ = 15.5 then drops to a plateau termi­ nating at TTiv = 18.5 with a sudden drop of membership to the limiting magnitude. We find little preferred orientation of the brightest cluster members with respect to position angle save for the slight excess at orientations almost directly West of North which appears to lie zilong the major axis of the dispersion ellipse.

The cluster appear to be divided almost equally between ellipticals and spi­ rals with a slight enhancement of the spirals the (JE : 50 : 5) ratio being (1.0 : 0.2 : 1.3). We note a relative enrichment of barred spirals in the sample and ■everal peculiar galaxies. The elliptical galaxies appear to be scattered throughout the cluster without apparent concentrations with perhaps the exception of their paucity in the Western portions of the cluster. Likewise, the spirals show no ob­ vious concentrations save for a small group North of the cluster center. The core population houses some 36% of the population in an area discribed by the disper­ sion ellipse of 0.2 square degrees. This yields a cluster core surface density of 330 galaxies per square degree.

We note several distressed spiral galaxies, perhaps superposed, such as the ob­ ject located at X = —95.4, y = —129.4 and another found at x = —78.9, y = —107.6. At least seven of the spirals in the sample appear to have ring-like structures, the brightest of which lies at z = —116.4, y = —117.6. The Cluster Catalogue 147 §3.2

GALAXY CLUSTER 025 21 13 10 - 5 9 36

I J — ; jÿT,

Figure 3.2.25 (a) Field of GALAXY CLUSTER 025: 21 IS 10 -59 SO The Cluster Catalogue 148 §3.2

GALAXY CLUSTER 025 21 13 10 - 5 9 36

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTI0N

E I

O i •o

I£GEND-i E = » B0 = « ! S * • i S B = • :

EAST « g E ? S 8 8

CLUSTER MAGNITUDE D IST R IB U T I0N P0SITI0N ANGLE DISTRIBUTION 100. 24. 80. 22.

80.

e a | 15. ttüMT9 fCP SETT*) 13. ^ «g“ i so.

2 0 .

10.

0 . „ ...... eooooeooooooooeooo coiflu^tnvvtncn

Figure 8.2.25 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Ca.talogue 149 §3.2

CHLBXT CLUSTER 02S 21 13 10 -53 36 CnjX T CLUSTER 025 21 13 10 - S 3 36 CfLBXT CLUSTER 025 21 13 10 -53 36

i i

GALAXY CLUSTER 025 21 13 10 -59 36 FIELD 14S ESa/SERD PLATE J17S9

X Y RA DEC L B Z CIOSDI IIBSDJ I1S50I 119501 - 1 3 1 .7 0 5 0 1 8 .5 7 4 21 13 1 0 .0 --59 36 24.2 336 2 49.4 -41 23 39.8 0 . 042

M0RPH0L0CY DISPERSION ELLIPS E CLUSTER MEMBERS

E 113 MAJOR AXIS 15. 11 SAMPLE POPULATION 271

80 19 MINOR AXIS 13. 10 CORE POPULATION 106

S 135 ECCENTRICITY 0.50 LIMITING MAGNITUDE 1 9 .0

SB 4 P0SN. ANGLE 8 8 .0 9

P 0

Figure 8.2.25 (J,g,h) Clutter Morphological Population Distributiont. Table 8.2.25 Cluster Population Description.

GALAXY CLUSTER 025: 21 IS 10 -59 8 6 : The cluster is located in the North-West quadrant of ESO/SERC Field 145. Within a diameter of 45mm as determined by mjo we count 296 galaxies in this cluster and 271 to a limiting magnitude of mijm = 19.0. The cluster is classified Abell type I because of its large nonuniform scatter and clumpy appearance.

We count 80 galaxies brighter than mj + 2 and thus classify the cluster as r i e Cluster Catalogue 150 §3.2 having an Abell richness of 2. We suggest a B — M type II classification for the cluster which has several very bright galaxies intermediate in appearance between the cD class and normal giant ellipticals. For and mio we give 13.9, 14.6 and 15.1, respectively. The value of mio implies a redshift of 0.042.

We find the general appearance of the cluster to be irregular and somewhat clumpy. The cluster has several density concentrations located North and South of the cluster center as well as another found to the East. There are regions apparently devoid of galaxies, such as that found to the North-West at the periphery of the cluster.

The magnitude distribution rises slowly from the brightest members to about = 16.5 after which we find the bulk of the sample population under a large plateau ranging from m„ = 16.5 to nty = 18.5 after which the numbers decrease rapidly to the magnitude limit. We find the position angle distribution skewed to the North-East with a disproportionate number of bright galaxies oriented between forty and sixty degrees in the positive sense.

The cluster appear somewhat spiral rich with the (E : SO : S) ratio of (1.0 : 0.2 ; 1.2). The elliptical galaxies display several concentrations, especially North and South of center whereas the spirals appear to show a single concentration South-West of center. We note a slight single group of SO galaxies at the cluster periphery. The core population represents some 39% of the sample in an area of nearly 0.22 square degrees. This yields a core density of 486 galaxies per square degree.

We note several pairs of superposed galaxies that appear to be spirals such as those located at z = —138.0, y = 29.4 and x = —130.4, y = 2.8. We also note a peculiar group of galaxies whose brightest member is located at z = —135.5, y = 5.2. Tie Cluster Catalogue 151 §3.2

GALAXY CLUSTER 026 21 22 58 - 3 5 00

li 1 i.q L U iu in ju 111xu 11 iiiiij111 ij i ‘ jTrnrnrn,'! 1111,,,.,...... _ % /.-v V/'v’' '.• ■ ~ : .-'..-••■v’.v» V.- - ■• • . : - : : ^ ■/... ■ ; V.. -* ■. V -•' • ■ ■ ■ -

‘ ■ ■■• ■ 0 > 1 f . i- • .-r ' *■ ' .. . . t m - :... .* ..' .# . •--^-ii'.

• V # .%

. . • fb . •

. 0 '. ' V -# ' •

1-J# O f : y # r . " ' -i- **- ** . E . • ^ • . . • .

S ’* ' ' É I I I I I I ! ■ ; : 1 I I : ■ I I I I I ! ' ! I I I I rirrrrnTii;

Figure 3.2.26 F»eW of G A LA X Y CLUSTER 086: 81 88 58 -S5 00 T ie Cluster Catalogue 152 §3.2

GALAXY CLUSTER 026 21 22 58 - 3 5 00

SURFACE DENSITY DISTRIBUTI0N CLUSTER MEMBERSHIP AND M0RPH0L0GY

E \

t

lEGEKD S0 =: •

CLUSTER MAGNITUDE D IS T R IB U T I0N P05ITI0N ANGLE DI5TRIBUTI0N 100. ». ». #0. 22. 21. eo. 2 0 . g «.h

15. iiwra MX

». ».

10.

TlCTfl (DECREES) c „ o „ o o .n o u . o H : : : ;

Figure 3.2.26 (b) Cluster Morphology, (c) Surface Density Distribution, (i) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 153 §3.2

CRLAXY CLUSTER 026 21 22 58 -35 00 CfiLRXT CLUSTER 025 21 22 58 -3 5 00 CFLflXY CLUSTER 026 21 22 58 -3 5 00

ELLIPTIC^. CflLPXIES SPIRPL GALAXIES m ten * BBT m “ B c r w t i t i i t * t i i i tiiitttt i t t t i i t i t t t i i t

GALAXY CLUSTER 026 21 22 68 -35 00

FIELD 4 D 3 ESa/SERC Pl BTE JS293

X Y RP DEC L B z C1950I (18501 (ISSOI (ISSOI -M 9. 719 -001.784 21 22 58.0 -35 0 38.8 009 47 57.8 -45 46 32.8 0. 052

MBRPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 2 0 9 MPJ0R RXIS 1 0 .6 1 s a m p l e PBPULATIBN 323

SB 48 MINER AXIS 8.66 C0RE P0PÜLRTI0N 103

S 6 5 ECCENTRICITY 0.58 L IM IT IN G MAGNITUDE 1 9 .0

SB 0 P0SN. ANGLE 3 2 .2 1

P 1

Figure 8.2.26 Cluster Morphological Population Distributions. Table 3.2.26 Cluster Population Description.

GALAXY CLUSTER 026: 21 22 58 -85 00 : The cluster is located in the South-West quadrant of ESO/SERC Field 403. Within a diameter of 45mm as determined by mio we count 547 galaxies in this cluster and 323 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type RI because of its somewhat regular appearance, but we note several clumps of galaxies throughout the sample. The Cluster Catalogue 154 §3.2

We count 81 galaxies brighter than ms + 2 and thus classify the cluster as having an Abell richness of 2. We suggest a B - M type HI classification for the cluster which has no really dominant galaxies save for a few bright members near the cluster center. For m i,m s, and mio we give 15,1, 15,3 and 15,5, respectively. The value of mio implies a redshift of 0,052,

We find the cluster somewhat elongated with several concentrations, the main ones located North-West of center and South-East of center. The cluster appears to reside in a sea of faint galaxies below the sample magnitude limit. We find the magnitude distribution gently rising from the brightest members to a plateau terminating at m„ = 18,0 after which there is an extremely rapid rise to the mag­ nitude limit. This may suggest the cluster is a cloud of galaxies superposed on a fmnt background. We find the position angle distribution somewhat skewed with a preference of the brighter galaxies to be oriented West of North with an obvious peak located at 45 degrees in the negative sense.

The elliptical galaxies in the sample are scattered throughout the cluster with m, major concentration to the North-West of cluster center along the major axis of the dispersion ellipse. The spirals appear to be located more to the periphery of the cluster with some avoidance of the Western portions. The [E : SO : S) ratio greatly favors the elliptical galaxies with divisions distributed as (1,0 : 0,2 : 0,3),

We find nearly 32% of the galaxies in the core of the dispersion ellipse which spans an area of 0,1 square degrees. This yields a core surface density of 1018 galaxies per square degree.

We note nine pairs of elliptical galaxies in very close proximity that consist of an early and a late member, the brightest of which is located at x = —158,2, y = 10,3, The Cluster Catalogue 155 §3.2

GALAXY CLUSTER 027 21 26 10 - 5 1 04

Figure 3.2.27 faj Field of GALAXY CLUSTER 027: 21 26 1 0 -51 04 The Cluster CataJo^e 156 §3.2

GALAXY CLUSTER 027 21 26 10 - 5 1 04

SURFACE DENSITY DI SIRIBUT10N CLUSTER MEMBERSHIP AND M0RPH0L0GY

•11.

i :

«T7. Kuni

i I

S 5 S

CLUSTER MAGNITUDE DISTRIBÜTI0N P05ITI0N ANGLE DI5TRIBUTJ0N K». 25. I I I I I I I I A , I I I— :— !— I— 1 24. 0 23. • . 22. 21. eo. 2 0 . 19. 16. 7 0 . 17. 16. 15. 14. K. C M T S rot 9ECTP 13. 12. 11. 40j 10. 9. 6 . 80. 7. 6 . 20. S. 4 Ï- j W l f f If 10. 3 . 2 , I. tfV; 0 . 0 . j I I » I qPC N ing RfiNK E THETA (DECREES) W o m o b n o «•eoooeoeeeooooaooo V) CD CD f ' r*>' ui i/i » m m

Figure 8.2.27 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 157 §3.2

CflLRXr CLUSTER C?7 21 2S JO -51 M GFLflXT CLUSTER 027 21 26 30 -51 M GALAX7 CLUSTER 027 21 25 10 -51 04 I

GALAXY CLUSTER 027 21 26 10 -51 04

FIELD 2 3 6 ESO/SEBC PLR7E J2 3 3 I

X Y RA DEC L B z IiaSOI (19501 (19501 [[9501 033.381 -057.179 21 26 9.6 -51 4 18.4 346 48 32.5 -45 20 16.5 0.048

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 92 MAJ0R A X IS 1 0 .4 4 SAMPLE POPULATION 221

50 14 MIN0R AXIS 9.24 C0RE POPULATION 80

S 107 eccentricity 0 .4 6 LIMITING MAGNITUDE 19.0

SB 7 P0SN. ANGLE - 7 9 . 1 5

P 1

Figure 8.2.27 (f,g,h) Clutter Morphological Population Distributions. Table 8.2.27 Clutter Population Description.

GALAXY CLUSTER 027: 21 26 10 -51 04 : The cluster is located in the South-West quadrant of ESO/SERC Field 236. Within a diameter of 45mm as determined by mio we count 263 galaxies in this cluster and 221 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type I because of its irregular appearance.

We count 43 galaxies brighter than mj + 2 and thus classify the cluster as The Cluster Catalogue 158 §3.2

having an Abell richness of 0 . We suggest a B — M type IH classification for the cluster which lacks any dominant galaxy. For and mio we give 13.5, 14.5 and 15.3, respectively. The value of mio implies a redshift of 0.048.

We find that the cluster contains several major concentrations, in particular, those located near the cluster center, North of center and South-East of center. These appear to be other smaller groups scattered throughout the sample.

The magnitude distribution is far from smooth, with a gentle rise from the brightest galaxies to about rriy = 16.5 where a sharp rise in membership occurs. The distribution then drops rapidly and rises again to the magnitude limit. Position angles are irratic as well with the suggestion of a larger number of bright galaxies oriented West of North, with a greater population having position angles less than forty-five degrees.

We find a high concentration of elliptical galaxies near the center of the cluster with the spirals somewhat less concentrated and away from center. The {E : SO : S) ratio suggests a slighly spriral enriched cluster with a distribution of (l.O : 0.2 : 1.2). Those galaxies identified as SO appear to be located in the Southern portion of the cluster.

We note that the core population comprises some 36% of the sample within an area of 0.11 square degrees giving a core surface density of 753 galaxies per square degree.

We find four pairs of elliptical galaxies in the cluster which appear to be com­ prised of two early type ellipticals, the brightest of which is located at z = —32.3, y = —55.5. The majority of the spirals are noticed to be lens-like in appearance with central condensations. The Cluster Catalogue 159 §3.2

GALAXY CLUSTER 028 21 29 13 - 3 5 23

'"#Y'

Figure 3.2.28 faJ Field of GALAXY CLUSTER 028: 21 29 IS -S5 2S Tie Cluster Catalogue 160 §3.2

GALAXY CLUSTER 028 21 29 13 - 3 5 23

SURFACE DENSITY DISTRIBUTION CLUSTER MEMBERSHIP AND M0RPH0L0GY

-».î

CLUSTER MAGNITUDE DISTRIBUTION too. P 0 5 IT I0 N ANGLE D IST R IB U T IO N

•0 .

BO,

70.

15. 13. ^ 50.

40j

2 0 .

10.

0 . E TJCTR (DECREES) ;

Figure 3.2.28 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 161 §3.2

CaHXT CLUSTER 028 21 29 13 -3S 23 GALAXY CLUSTER 028 21 29 13 35 23 GALAXY CLUSTER 028 21 29 13 -3 5 23

I a 1 J

.* ■ *

i . a E i

*

* 1

____ ELLIPTICAL DA.AX1C5. 30 GALAXIES SPIRAL GALAXIES I â g < i i i « ttëitttitii

GALAXY CLUSTER 028 21 29 13 -35 23

FIELD 4D3 ESO/SERC PLATE JS230

X Y RA DEC L B Z I195DI CI950J I185DI (19501 - 0 7 5 . 80 7 - 019.961 21 29 13.5 -35 22 50.6 009 24 15.7 -47 4 43.0 0 .0 4 4

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 3S1 MAJOR AXIS 10. 39 SAMPLE p o p u l a t io n 27 0

50 40 MIN0R AXIS 9.2B CORE POPULATION 102

5 73 ECCENTRICITY 0 .4 5 L IM IT IN G MAGNITUDE 19 0

SB 5 P0SN. ANGLE - 4 . 3 6

P 1

Figure 8.2.29 (f,g,h) Cluster Morphological Population Distributions. Table 8.2.29 Cluster Population Description.

GALAXY CLUSTER 028; 21 29 18 -85 23 : The cluster is located in the South-West quadrant of ESO/SERC Field 403. Within a diameter of 45mm as determined by mio we count 430 galaxies in this cluster and 270 to a limiting magnitude of miim = 19.0. The cluster is classified Abell type I because of its scattered appearance and several condensations.

We count 55 galaxies brighter than mj + 2 and thus classify the cluster as The Cluster Catalogue 162 §3.2 having an Abell richness of 1. We suggest a B — M type 00 classification for the cluster which has... For mi,m 3 , and rriio we give 13.8, 15.0 and 15.5, respectively. The value of mio implies a redshift of 0.044.

The cluster membership appears somewhat concentrated towards the core of the dispersion ellipse with several density enhancements noticed directly South and East of the cluster center. There appear to be several smaller concentrations dis­ tributed throughtout the cluster giving it a somewhat irregular shape.

The magnitude distribution of the cluster shows a general rise from the bright­ est galaxies to the magnitude limit of the sample with an obvious plateau centered at m„ = 17.0. The position angle distribution shows an excess of bright galaxies oriented West of North, in the negative sense, with a significantly larger peak almost directly North, along the minor axis of the dispersion ellipse.

We find the elliptical galaxies somewhat concentrated towards the center of the cluster with the spirals more scattered about. The (E : SO : S) ratio is (1.0 : 0.3 : 0.5) suggesting an elliptical-rich cluster.

The core population comprises some 38% of the sample contained in an area of 0.11 square degrees on the sky. This yields a core surface density of 961 galaxies per square degree for this cluster.

We notice some fifteen pairs of elliptical galaxies, some superposed, and most comprised of an early and a late elliptical galaxy, the brightest of which is located at X = —94.8, y = —23.4. In addition, we point out several interesting spiral galaxies with ring-like structures such as the object located at x = —66.3, y = —16.6. T ie Cluster Catalogue 163 §3.2

GALAXY CLUSTER 029 21 31 14 - 6 2 L

•#

Figure 3.2.29 (a) Field of GALAXY CLUSTER 029: 21 SI U -62 15 T ie Cluster Catalane 164 §3.2

GALAXY CLUSTER 029 21 31 14 - 6 2 15

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTIBN

I I L r

•110.

-1» . Ï i S ^jn

f tn ! F LEGEND" I I AT.

EAST m ç rs = ? “ = c 8 r s

CLUSTER MAGNITUDE D ISTRIBUTION POSITION ANGLE D ISTR IB U TIO N

■0 . eo. 20. g 19. C ;s: : 16. U 15. g o u r s m SECT» 13. 12. E 11. C

1 0 . 7.*: 2 0 .

10.

^«NITl^RflGE „ ^ • EOBoeeeeeeooooooooo T « T f l I D E C R E E S ) k 8 8 e S S i Ji S S ° S s' !! ? s s s s s

Figure 3.2.29 (b) Cluster Morphology, (c) Surface Density Distribution. (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 165 §3.2

CBLRXY CLUSTER 029 21 31 14 -6 2 IS GALAXY CLUSTER 029 21 31 14 -6 2 15 GR.AXY CLUSTER 029 21 31 14 -62 15

i i

ELLIPTIC A L GALAXIES SPIRAL GALAXIES wr wr é # i

GALAXY CLUSTER 029 21 31 14 -62 15

F tE U J 145 Esa/SERC PLATE J17S9

X Y RA DEC L B Z IIS5Q] 119501 119501 119501 - 0 0 8 .4 7 1 .118.667 21 31 14.2 -52 15 40.3 331 40 36.2 -42 31 56.4 0.043

MORPHOLOGY DISPERSI0N ELLIPSE CLUSTER MEMBERS

E 125 MRJ0R A X IS 1 6 .0 5 SAMPLE POPULATION 298

SB 31 MIN0R AXIS 12.46 CORE POPULATION 107

S 132 ECCENTRICITY 0.63 LIMITING MAGNITUDE 19.0

SB 8 P0SN. a n c l e 7 6 .3 6

P 1

Figure 8.2.29 (f,g,h) Clugter Morphological Population Distributions. Table 8.2.29 Cluster Population Description.

GALAXY CLUSTER 029; 21 81 14 -62 15 : The cluster is located in the South-West quadrant of ESO/SERC Field 145. Within a diameter of 45mm as determined by mio we count 306 galaxies in this cluster and 298 to a limiting magnitude of miim = 19.0. The cluster is classified Abell type R because of its regular appearance and fairly uniform distribution of galaxies.

We count 93 galaxies brighter than mj + 2 and thus classify the cluster as T ie Cluster Catalane 166 §3.2

having an Abell richness of 2. We suggest a J5 — M type I classification for the cluster which has a dominant and centrally located cD galaxy. For mi,m 3 , and mio we give 14.0, 14.7 and 15.4, respectively. The value of mio implies a redshift of 0.048.

This rather elongated cluster displays a higher concentration of galaxies to­ wards the cluster center, falling ofi" radially to the cluster periphery. Dominated by a centrally placed cD galaxy the cluster has a few density concentrations, primar­ ily located North of the cluster center, although a single condensation is noticed South-West of center near the edge of the cluster.

We notice that the cluster magnitude distribution rises somewhat uniformly from the brightest cluster members to about niv = 18.0 after which it declines rapidly suggesting few very faint galaxies in the field. The position angle distri­ bution displays a higher numbers of member galaxies oriented East of North with ieveral peaks, the largest of which lies nearly North-South.

The elliptical galaxies are scatered throughout the cluster in few concentrations, mave the minor one located South-West at the cluster periphery. The numbers of spirals on the other hand, appear to be somewhat enhanced near the center of the cluster, within the dispersion ellipse. We find the [E : SO : S) ratio to favor the spirals being (l.O : 0.2 : 1.1). The core population of the sample comprises some

8 6 % of the galaxies resident within the dispersion ellipse. Since the cluster spans 0.22 square degrees, this amounts to some 486 galaxies per square degree in the core.

We note several close pairs of elliptical galaxies composed of an early and a late member such as that located at * = 7.0, y = —135.5, as well as a virtually superposed pair of late ellipticals of similar brightness at z = 9.1, y = —114.3. The Cluster Catalogue 167 §3.2

GALAXY CLUSTER 030 21 31 06 -53 50

Figure 8.2.80 faj Field of GALAXY CLUSTER OSO: SI SI 06 -5S 50 The Cluster Catalogue 168 §3.2

GALAXY CLUSTER 030 21 31 06 - 5 3 50

SURFACE DENSITY DISTRIBUTIBN CLUSTER MEMBERSHIP AND M0RPH0L0GY t s . tie .

m.

90. Î E E 2 90. # 3 90. ëïîsi e. 65 A.n m .

m. E A S T W WEST S

CLUSTER MAGNITUDE D ISTR IB U TIO N P05ITI0N ANCLE DISTRIBUTION ]0 Q. 25. 24. 90. 22.

0 0 . 19. & 70.

15. CKMT3 p m g C T W 13. ^

90.

2 0 .

10.

M B g irT lB E RANGE oeevoeeoODoE THETAoeoeooeo (DECREES) H

Figure 3.2.30 (b) Cluster Morphology, (c) Surface Density Distribution, (i) Magnitude Distribution and (e) Position Angle Distribution. Tie Cluster Catalogue 169 §3.2

GRLfln CLUSTER 030 21 31 06 -5 3 50 CFLRXY CLUSTER 030 21 31 06 -S 3 50 CafiX T CLUSTER 030 21 31 05 -5 3 50 I I

i

e # r ÜST i 4 4 i 4 i 1 i ^ * # # f ^ f "

GALAXY CLUSTER 030 21 31 06 —53 50

FIELD IBS ESa/SERC PLATE J1592

X Y RA DEC L B Z (19501 (19501 (IB50I (19501 0 2 8 . 75 5 064.519 21 31 5.9 - ■53 SO 8 .2 342 41 57.2 -45 23 37.9 0. 050

MORPHOLOGY DISPERSION ELLIPSE CLUSTER MEMBERS

E 7 7 MAJOR A X IS 1 1 .0 4 SAMPLE POPULATION 182

S0 21 MINOR A X IS 9 .2 8 CORE POPULATION 70

s 78 ECCENTRICITY 0.54 LIMITING MAGNITUDE 1 9 .0

SB 5 P0SN. ANGLE 5 3 . 13

P 1

Figure 8.2.30 (f,g,h) Cluster Morphological Population Distributions. Table 8.2.30 Cluster Population Description.

GALAXY CLUSTER 030: 21 31 06 -53 50 : The cluster is located in the North-East quadrant of ESO/SERC Field 188. Within a diameter of 45mm as determined by mio we count 225 galaxies in this cluster and 182 to a limiting magnitude of mjim = 19.0. The cluster is classified Abell type I because of its inherently high level of scatter.

We count 62 galaxies brighter than m@ +2 and thus classify the cluster as having The Cluster Catalogue 170 §3.2 an Abell richness of 1. We suggest a B — M type II classification for the cluster which has its brightest galaxies intermediate between the class cD and normal giant ellipticals. For m i,m s, and mio we give 14.6,14.9 and 15.4, respectively. The value of mio implies a redshift of 0.050.

We note that the cluster has a somewhat higher concentration of galaxies in its central regions with a number of dense groups found North-West of the cluster center. East of center and slightly South of center.

The magnitude distribution rises gently from the brightest galaxies to about «V = 17 0 upon where it levels off nearly horizontally to the magnitude limit. The position angle distribution displays an erratic scatter but has peaks, however, running East of North, North-South and North of West.

We notice that the elliptical galaxies tend to be more centrally situated than otherwise and that the spirals appear to be scattered more uniformly. The (E : SO : S) ratio is (1.0 : 0.3 : 1.1) indicating a slight excess of spirals. The core population contains some 38% of the sample in an area of 0.11 square degrees. This implies a surface density of 620 galaxies per square degree on the sky.

We notice several of the galaxies in this cluster to be superposed or in very close pairs. An unusual early elliptical galaxy with a corona appears superposed with a later elliptical at z = 26.3, y — 63.5. Another pair of bright paired early and late ellipticals is seen at z = 37.4, y = 61.4. A number of distressed barred spiral galaxies are seen, for example, like that at z = 34.9, j/ = 59.5. Finally, we notice what appears to a planetary nebula in the field located at z = 41.2, y = 59.8. The Cluster Catalogue 171 §3.2

GALAXY CLUSTER 031 21 32 18 - 5 2 44 i i ) 11I I 1111 ; 111 ri ] 11 j'; 111111111111111111111: 1III H 11111 ( 111 i'll 111 i t | 11 i"n 11 ri )'i 11 > i .,. , . N •

*

♦

♦ * #'

♦ •

Figure 3.2.81 fa) Field of GALAXY CLUSTER OSl: SI S2 18 -5S 44 The Cluster Catalogue 172 §3.2

GALAXY CLUSTER 031 21 32 18 - 5 2 44

SURFACE DENSITY DISTRIBUTIBN CLUSTER MEMBERSHIP AND M0RPH0L0GY ffO. I- I I 4' j ■ j ' I j I— r IfQ. in. no.

i f tio. no. LEGEND in. = 60= n . m . I ; '4 • r I ERST £ ? ? ? ' • m m

CLUSTER MAGNITUDE DISTRIBUTIBN PBSITI0N ANGLE DISTRIBUTIBN zs. 24.

2 2.

H 15. CfUKTS fO 3ECm 13. ^ 1 2.5

6. S

WCNITUg RAN% eoeoooeoeeeeTHETA (DECREES) 6 8 R S S g«S2®2£Rgggp

Figure 8.2.81 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 173 §3.2

CRLHXT auST E R 031 21 32 IB -52 M CflflXT CLUSTER 031 21 32 18 -5 2 45 Cft-HXr CLUSTER 031 21 32 10 -5 2 44

Î I

ELLIPTICAL ta.HXJES S0 GALAXIES SPIRAL GALAXIES BBT * t 1 i i i t 4 * ” * I t

GALAXY CLUSTER 031 21 32 18 -52 44

FIELO IBB ES0/SERC PLATE J1ES2

X Y RA DEC L B z IIBSOI (19501 (19501 (19501 039.266 123.490 21 32 18.2 -52 44 2.1 344 8 48.2 -45 51 52.5 0.044

M0RPH0LBGY DI5PERS10N ELLIPSE CLUSTER MEMBERS

E 61 MHJ0R AXIS 11.20 SAMPLE P0PÜ LA TI0N 151

S0 14 MIN0R AXIS 10.66 C0RE POPULATION 48

S 6 7 eccentricity 0 .3 0 LIMITING MAGNITUDE 19.0

SB 7 P0SN. ANGLE - 6 8 . 9 4 P 2

Figure 8.2.31 (f,g,k) Cluster Morphological Population Distributions. Table 8.2.81 Cluster Population Description.

GALAXY CLUSTER 081: 21 82 18 -52 44 : The cluster is located in the North-East quadrant of ESO/SERC Field 188. Within a diameter of 45mm as determined by mio we count 227 galaxies in this cluster and 151 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type I because of its irregular and scattered appearance.

We count 57 galaxies brighter than m s+2 and thus classify the cluster as having The Cluster Catalogue 174 §3.2 an Abell richness of 1. We suggest a B — M type III classification for the cluster which has no major dominant galaxies save the first brightest that appears to be an edgewise spiral. For m i,m s, and mjo we give 15.0, 15.4 and 15.5, respectively. The value of mio implies a redshift of 0.044.

We find this cluster possessing a rather scattered appearance, with few concen­ trations, except for two small density enhancements, the greater located somewhat East of center, the lesser located East South-East.

The cluster magnitude distribution shows a very slow rise from the brightest galaxies with a greater change of slope occurring near m„ = 18.0 to the magnitude limit. The position angle distribution appears to have a slight concentration of galaxies oriented East of North and a peak running North-South.

We find the elliptical galaxies slightly more concentrated in the third and fourth quadrants, whereas the spirals occur more frequently in the second and third quad­ rants. The cluster appears somewhat spiral enhanced with an (E : SO : 5) ratio of (1.0 : 0.2: 1.2). This scattered cluster has a core population comprising nearly 52% of the sample in a region spanning 0.13 square degrees. This represents a core surface density of 365 galaxies per square degree on the sky.

We notice six close pairs of elliptical galaxies consisting of an early and a late elliptical, the brightest occurring at z = 40.5, y = 133.9. There are also a number of spiral galaxies with ring-like structures or ansae such as the object located at X = 52.4, y = 136.7. Several rather peculiar galaxies are also noted, such as that residing at z = 56.7, y = 110.0 which appears to possess a double nucleus within a diffuse ovoid mass. T ie Cluster Catalogue 175 §3.2

GALAXY CLUSTER 032 21 41 46 -5 1 44

s

Figure 3.2.82 faJ Field of GALAXY CLUSTER OSS: 21 i l i6 -51 U T ie Cluster Catalogue 176 §3.2

GALAXY CLUSTER 032 21 41 46 - 5 1 44

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTIBN

-• 0. I -TO. h0 f O

£

• • C5U! LEGEND GO; I îiîî'H

ERST MM *CST fl 9 R e 2 8 ^ Ç g S S

CLUSTER MAGNITUDE D ISTR IB U TIB N P 0 5 I T I 0 N ANGLE D ISTRIB U TIB N 100. 2S. 24. 90. 22.

80.

70.

15.

13.

a. S

20 .

10.

E ■nCTO IDECREESJ o „ u, o 00000000000000000S

Figure 3.2.82 (b) CluBter Morphology, (c) Surface Density Distribution. (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 177 §3.2

OWXT aUSTER 032 21 il K -Si Ü CFlflXr CLUSTER 032 21

3 3

EUlPTICnL CflLRXIES SPIRAL GALAXIES I I # 3 ; f # # , * f f f

GALAXY CLUSTER 032 21 41 46 -51 44

FIELD 236 ES0/SERC PLATE J2331

X Y RA DEC L B Z tlB SD I 118501 118501 (18501 0 9 6 . 5 5 3 -0 9 3 .9 1 7 21 41 4 6 .5 - 51 43 5 7 .4 344 58 17.5 -47 32 0.7 0. 043

M0RPH0L0GY D IS PE R S I0N ELLIPSE CLUSTER MEMBERS

E BO MOJ0R AXIS 1 5 .0 7 SAMPLE POPULATION 197

80 7 MIN0R AXIS 13.71 CORE POPULATION 62

S 100 ECCENTRICITY 0 .4 2 L IM IT IN G MAGNITUDE 1 9 .0

SB 8 P0SN. ANGLE 6 8 .7 7

P 1

Figure 3.2.82 (},g,h) Clutter Morphological Population Distributions. Table 3.2.32 Cluster Population Description.

GALAXY CLUSTER 032; 21 41 46 -51 44 : The cluster is located in the South-East quadrant of ESO/SERC Field 236. Within a diameter of 60mm as determined by mio we count 202 galaxies in this cluster and 197 to a limiting magnitude of mum = 19.0. The cluster is classified Abell t>’pe I because of its irregular structure and wide scatter.

We count 85 galaxies brighter than ms + 2 and thus classify the cluster as The Cluster Catalopie 178 §3.2 having an Abell richness of 2. We suggest a B ~ M type III classification for the cluster which has an intermediate appearance without a dominant centrally located bright galaxy. For mi,mg, and mio we give 14.5, 14.8 and 15.1, respectively. The value of mio implies a redshift of 0.043.

We find few concentrations in this irregular cluster save for a slight enhance­ ment South of center and another to the South-East. The magnitude distribution shows a slow rise from the brightest members to about a magnitude fainter, near niv = 15.5 where the distribution tapers off to a plateau spanning some three mag­ nitudes. Beyond the plateau the distribution falls off rapidly to the sample limit. The position angles vary irratically for the brighter members with a slightly greater number of galaxies oriented West of North and a few peaks indicating North-South orientations and North-East orientations.

The elliptical galaxies in this cluster appear to be somewhat concentrated to­ wards the center of the cluster whereas the spirals seem to be more uniformly spread throughout the cluster. We note that the cluster is a bit spiral enhanced with the (E : SO : S) ratio being (1.0 : 0.1: 1.4).

The core population represents slightly over 34% of the sample contained in an area of 0.23 square degrees. This yields a core surface density of 273 galaxies per square degree on the sky.

We notice an unusual collection of a pair of close pairs of elliptical galaxies located at z = 90.5, j/ = -73.5. There also appear to be a number of apparently superposed spiral galaxies such as the object located at z = 130.1,p = —108.9. Finally, we make notice of an early elliptical galaxy with two faint companions situated at z = 95.7, y = —100.8. The Cluster Catalogue 179 §3.2

GALAXY CLUSTER 033 21 42 51 - 5 7 30

IT! i^!T; ; I'TM i IJ [ I 11 Vi ipy ; i iT] 11 tti : ‘ ‘ ^ ‘ ‘ ‘ ‘ ‘ l ‘ L* ' ‘ ‘ ‘ ^

- . - ^ r ^ . ’’■ • t # I:' t . - V;;.: , 5^». *• s y

#

* Y . V . •>. . Y ' . >• . : ; . . » :^ , v ■■■ ^. ••*

n_u* I I I I I • 11 . M I I t • I ! M I ? I l l I I I ' ' ' ! I T I ' ' I i ! ( f ' I ' ■■ M ) j L M t LL ■' !

Figure 3.2.83 fa) Field of GALAXY CLUSTER OSS: 21 42 51 -57 SO T ie Cluster Catalogue 180 §3.2

GALAXY CLUSTER 033 21 42 51 - 5 7 29

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY D IST R 1B Ü T I0N . I

: ga

: IfGEKD n o . z n ? ! ; i

— .£P^L— ■ » LM «. # mm

CLUSTER MAGNITUDE DISTRIBUTION POSITION ANGLE DISTRIBUTION 100. so. eo.

70.

1 n / 1 r i I 90.

ZD. V 1 . 10. ‘i

0 E THETA I CECA EES I o ^ «W u, o eeevveeeooo oe

Figure S.2.8S (bj Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 181 §3.2

CH.RXY CLUSTER 033 21 C SI -5 7 23 CBLBXY CLUSTER 033 21 42 51 -5 7 29 GBLRXY CLUSTER 033 2! 42 5! -5 7 29

ELLIPTICAL GALAXIES 90 GALAXIES SPIRAL GALAX ES # * * $ » * # f f

GALAXY CLUSTER 033 2 1 42 51 -57 29

FIELD 145 ESO/SERC PLATE J1759

X Y RA DEC L B Z (10501 (IBSOI (10501 (ISSOI 0 7 4 .2 1 5 1 3 4 .6 0 0 21 42 50.B - 57 2 9 4 8 .5 336 58 51.8 -45 44 51.4 0 .0 4 2

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 2 6 2 MAJ0R AXIS 1 4 .4 5 SAMPLE P0PULATI0N 574

S0 39 MIN0R AXIS 11.56 CBRE POPULATION 214

3 2 5 8 ECCENTRICITY 0 .6 0 L IM IT IN G MAGNITUDE 19 .0

SB 35 P0SN. ANGLE 2 6 .3 9

P 0

Figure 8.2.33 ff,g,hj Cluster Morphological Population Distributions. Table 3.2.33 Cluster Population Description.

GALAXY CLUSTER 033: 21 42 51 -57 30 : The cluster is located in the North-East quadrant of ESO/SERC Field 145. Within a diameter of 45mm as determined by mio we count 604 galaxies in this cluster and 574 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type R because of its smooth albeit dense distribution of galaxies.

We count 110 galaxies brighter than m 3 + 2 and thus classify the cluster as The Cluster Catalogue 182 §3.2 having an Abell richness of 2. We suggest a B - M type II classification for the cluster which has the brightest galaxies intermediate between the class cD and nor­ mal giant ellipticals. For m i,m 3 , and mio we give 14.1, 14.6 and 15.0, respectively. The value of mio implies a redshift of 0.042.

This dense cluster presents an almost linear concentration within the dispersion ellipse with several dense subgroups to the East and South-East of the cluster center. Other concentrations occur throughout the cluster namely to the North of center and slightly West of North.

The cluster magnitude distribution rises rapidly with an almost linear slope from the brightest to the faintest magnitude, with the bulk of the sample population lying between the single magnitude range from m„ = 17.5 to = 18.5. The position angle distribution shows bright galaxies oriented at virtually all directions with major peaks located North-South and East of North.

We note that the distribution of elliptical galaxies in this cluster is curiously linear, along the major axis of the dispersion ellipse, whereas the spirals seem to be more uniformly scattered throughout the cluster save for a slight zone of avoidance to the West of cluster center. The population is practically evenly divided between ellipticals and spirals with an {E SO : S) ratio of (1.0 : 0.1 : 1.0). The core population comprises some 37% of the sample contained in an area of 0.18 square degrees. We thus find a core surface density of 1163 galaxies per square degree on the sky.

We find very few pairs of galaxies in this cluster, and those observed do appear to be combinations of early and late ellipticals, although several spiral galaxies in the sample appear to be superposed. Attention is drawn to a small group of elhptical galaxies in a faint subcluster located at a; = 8 6 .8 , y — 130.4. T ie Cluster Catalogue 183 §3.2

GALAXY CLUSTER 034 21 43 46 - 4 4 06

#

Figure 3.2.34 (a) Field of GALAXY CLUSTER OSJ^: U \S -U 06 T ie Cluster Catalane 184 §3.2

GALAXY CLUSTER 034 21 43 46 - 4 4 06

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DI5TRIBUTI0N 110. n'TTi.'iI m. ë : m. rr. e.

«5. 1 0«* 0»

esi!i $ LEGEND E = # 5 0 = ♦ II. G - * 6B= •

EAST *C ST B S 2 8 S S 8 ......

CLUSTER MAGNITUDE DISTRIBUTI0N P0SITI0N flNGLErfllSTRIBUTIDN 100. 24. to. eo.

70.

10. g - ,

30. 7. >-

E ■nC Tfi (DECREES) M o o u, «. o • ooe««eeeeeoeoooooe S 82 8SBB22»S8R22S2 2S

Figure 3.2.84 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 185 §3.2

CanxT Q.U5TER 034 21 43 46 -44 06 CRLRXT CLUSTER 034 21 43 46 -4 4 06 GR.BXT CLUSTER 034 21 43 46 -44 05

3

I

GALAXY CLUSTER 034 2 1 43 46 -44 06

FIELD z e e ESB/SERC PLB 'E J4S94

X Y RA DEC L B z IIBSOI (IBSOI IIBSOI IIBSOI - 1 1 9 .8 3 5 051.560 21 43 46.1 - 49 6 1 5 .9 356 6 55.3 -49 31 23.7 0. 049

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 167 MAJOR AXIS 15. 18 SAMPLE POPULATION 384

SB 27 MINOR AXIS 1 1 .7 4 CORE POPULATION 147

S 169 ECCENTRICITY 0 .6 3 L IM IT IN G MAGNITUDE 1 9 .0

SB 20 P0SN. ANGLE 1 1 .7 6

P 1

Figure 8.2.34 (f,g,h) Cluster Morphological Population Distributions. Table 3.2.84 Cluster Population Description.

GALAXY CLUSTER 034: 21 43 46 -44 06 : The cluster is located in the North-West quadrant of ESO/SERC Field 288. Within a diameter of 60mm as determined by mio we count 440 galaxies in this cluster and 384 to a limiting magnitude of mjim = 19.0. The cluster is classified Abell type I because of its irregularity and possibility of being superposed on a more distant cluster.

We count 97 galaxies brighter than mj -f 2 and thus classify the cluster as The Cluster Catalane 186 §3.2 having an Abell richness of 2. We suggest a B — M type II classification for the cluster which has a bright dominant galaxy with a corona that is intermediate in appearance between the class cD and normal giant ellipticals. For m i,m 3 , and mio we give 14.8, 14.9 and 15.3, respectively. The value of mio implies a redshift of 0.048.

We find this cluster to be somewhat linearly distributed with several small concentrations, lying East of center, North-West of center and South-West of center. There are numerous small voids in the cluster as well.

The magnitude distribution rises steeply from the brightest galaxies to the fainter with a nearly exponential rise to about m„ = 17.0 where a change of slope oc­ curs. There appears to be a large concentration of galaxies near m„ = 18.0 ofi’ering a mild suggestion of a subpopulation perhaps consisting of a faint background clus­ ter. The position angle distribution is chaotic at best, with several peaks, namely at the North-East, the North-South and the North-West orientations.

We note the high central concentration of the dispersion ellipse, with a similar population of ellipticals and spirals. The [E : SO : 5) ratio is almost equally divided between ellipticals and spirals and is (1.0 : 0.2 : 1.1). The core population comprises some 38% of the sample and is contained in an area of 0.2 square degrees. This gives a core surface density of 749 galaxies per square degree on the sky.

We notice only three pairs of close elliptical galaxies in this cluster, so rich in elliptical galaxies. The brightest of these is located at z = —124.5, j/ = 56.4. Over a dozen of the spiral galaxies in the sample appear to have obvious ring-like structures, for example, as that found at z = —94.6, y = 61.8. In addition we note a spiral with what appears to be a double nucleus at z = —132.7, y = 59.3. The Cluster Catalogue 187 §3.2

GALAXY CLUSTER 035 21 44 41 - 4 6 13

Figure 3.2.35 (a) Field of GALAXY CLUSTER 0S5: 21 U 4I -46 IS The Cluster Catalogue 188 §3.2

GALAXY CLUSTER 035 21 44 41 - 4 6 13

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUT20N

5 -40 I p o>

3 3% fâïM 5% ë s ëcüi IfGEND >no E - ' 5?5?!î 60= « ïï; •110 S = *. SB* •

8 8 8 « $ S 8 .«Sh—«

CLUSTER MAGNITUDE D IS T R IB U T I0 N P0SITI0N ANGLE MO I5TRIBUTI0N

22. 21. 3: g

15.

TîCTfl (DECREES)

Figure S.2.S5 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 189 §3.2

CALHXY auSTO? 035 Z 1 M 4 I -46 13 CRLAXT CLUSTER 035 21 44 41 -4 6 13 CALAXT CLUSTER 035 21 44 41 -4 6 13 I

3 3

ELLIPTICAL GALAXIES SPIRAL GALAXIES ■er mt mm i i i

GALAXY CLUSTER 035 2 1 44 41 -46 13

FIELD 2 8 8 ES0/SERC PLATE J4594

X Y RA DEC L B Z IlS S D I I195Q I (ISSDI (19501 - 1 0 7 . 000 -061.752 21 44 40.6 - 46 13 3 2 .3 352 51 36.7 -49 19 4.4 0 .0 4 3

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 141 MRJ0R AXIS 14.38 SAMPLE P0PULATI0N 354

SO 48 MINBR AXIS 12.98 C0RE P0PULATI0N 114

s 156 ECCENTRICITY 0 .4 3 L IM IT IN G MAGNITUDE 1 9 .0

SB 9 P0SN. ANGLE -8 .0 5

P D

Figure 8.2.35 (f,g,h) Cluster Morphological Population Distributions. Table 3.2.35 Cluster Population Description.

GALAXY CLUSTER 035; 21 44 41 -46 IS : The cluster is located in the South-West quadrant of ESO/SERC Field 288. Within a diameter of 60mm as determined by mio we count 395 galaxies in this cluster and 354 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type R because of the strong central condensation found in this cluster.

We count 86 galaxies brighter than mj + 2 and thus classify the cluster as Tie Cluster Catalogs 190 §3.2 having an Abell richness of 2. We suggest a B — M type II-III classification for the cluster which appears to have bright and dominant galaxies but no strikingly giant ellipticals. For mx,ms, and mio we give 13.4,14.6 and 15.1, respectively. The value of mxo implies a redshift of 0.043.

We notice that the cluster is centrally condensed with several density enhance­ ments, most notably near the cluster center. Slight groupings are also apparent N orth of center and West of center.

The cluster magnitude distribution is nearly linear from the brightest galaxies to the faintest, with a slight falloff near the magnitude limit. We find the position angle distribution for the brighter galaxies to be generally non-preferential, but with an excess running North-South and a relative depletion at small angles oriented Eastward.

We find the elliptical galaxies somewhat concentrated towards the center of the cluster with another slight concentration West of center near the periphery of the dispersion ellipse. The spirals appear more dispersed and are found without significant concentration throughout the cluster. The morphological distribution is somewhat skewed towards the spiral galaxies with an {E : SO : S) ratio of (1.0 : 0.3 : 1.2). The core population comprises some 32% of the sample and spans 0.2 square degrees. The core surface density thus derived is 555 galaxies per square degree on the sky.

We find several bright elliptical galaxies to posses a corona. There are very few pairs of galaxies seen in this cluster. Those that are seen are pairs of ellipticals with a curious group of three faint pairs located near x = —125.3, y = —62.7. We also note several spiral galaxies wkh ring-like structures, for example, as that located at X — —104.1,y = —67.7. T ie Cluster Catalogue 191 §3.2

GALAXY CLUSTER 036 21 50 32 - 5 8 04

Figure S.2.S6 (a) Field of GALAXY OLVSTER 0S6: SI 50 SS -5S Of The Cluster Catalogue 192 §3.2

GALAXY CLUSTER 036 21 50 32 - 5 8 04

auwrncr dcnsitt DisTniouTiBN CLUSTER MEMBERSHIP AND H0RPH0L0GY no. no.^ 140.1

110. £ 3 H

HD.

m. âf!

LEGEND m. ; K - • 1 8 0 = • fO. 8 * * 8B" •

EAST EST -'Wc'

CLUSTER MAGNITUDE DISTRIBUTION POSITION ANGLE D ISTRIBU TIO N 23.29. 2 2 . 21. 20. IS. IS. n. IE. 15. *0 # e 4 2 0 2 4 6 0 10 19. nUKTS fOl 9EnW 13. 12. 11. 10a.. 8. 7. G. 5. 9. - f t r 3. 2. r 1. _ l ______I______I______L. 0. IKNITire RANGE TÆTfl (DECREES) ■n CD ai2 £ S 5 5 ici ui

Figure 3.2.36 fbj Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 193 §3.2

WLfiXY CLUSTER 036 21 50 32 -5 6 (M CHLflXY CLUSTER 036 21 SO 32 -5 8 M CBLBXY CLUSTER 036 21 50 32 -SB OS

ELLIPTICAL GALAXIES S O f W X I E S SPIRAL GALAXIES IBT SBT Ml IBP BBT m ICSI f f i 1 i 1 1 ? M ♦ ( ^ 1 M M ? t 1 ? M f ? ? ; ! < <

GALAXY CLUSTER 036 2 1 50 32 -58 04

FIELD 14S ESe/SERC PLATE J17S9

X Y RA DEC L B z 119501 (19501 I19S0I (ISSOI 127. 534 102.014 21 50 3 2 .0 -5 8 3 4 8 .4 335 38 9.9 -46 27 19.6 0 .0 5 0

MORPHOLOGY DISPERSION ELLIPSE CLUSTER MEMBERS

E 147 MPJ0R AXIS 7 .8 0 SAMPLE POPULATION 295

50 14 MINOR AXIS 7 .5 9 C0RE POPULATION 112

S 129 ECCENTRICITY 0.23 LIMITING MAGNITUDE 1 9 .0

SB 3 P0SN. ANCLE -16.53

P 2

Figure 8.2.36 (f,g,h) Gluater Morphological Population Distributions. Table 3.2.86 Cluster Population Description.

GALAXY CLUSTER 036; 21 50 32 -58 04 : The cluster is located in the North-East quadrant of ESO/SERC Field 145. Within a diameter of 36mm as determined by mio we count 302 galaxies in this cluster and 295 to a limiting magnitude of miim = 19.0. The cluster is classified Abell type R because of its high central condensation.

We count 105 galaxies brighter than m 3 + 2 and thus classify the cluster as T ie Cluster Catalogue 194 §3.2 having an Abell richness of 2. We suggest a B — M type II-III classification for the cluster which has several bright galaxies, but none that could be considered other than normal giant ellipticals. For m i.m j, and mio we give 15.0, 15.1 and 15.4, respectively. The value of mio implies a redshift of 0.050.

We note the high central condensation of this cluster as well as its near circular appearance. There are several major concentrations within the body of the cluster, most notably a mass of galaxies East of center. Other less dense groups are found North-West and South-West of the center of the cluster.

The cluster magnitude distribution rises gradually from the brightest galaxies to a plateau a full magnitude in width centered on = 17.0. The distribution then suffers a rise for half a magnitude then drops in several steps to the magnitude limit. The position angle distribution shows no significant preference for orientation save for the excess noted with a North-South inclination.

We notice the strong concentration of elliptical galaxies towards the center of the cluster, whereas the spirals appear to be more evenly distributed except for * slight paucity of members a little South-West of cluster center. The cluster is about divided equally between ellipticals and spirals with an {E : SO : S) ratio of (1.0 : 0.1: 0.9) with a slight enhancenent of elliptical galaxies of about ten percent. The core population represents nearly 38% of the sample and resides in an area of some 0.06 square degrees. The core surface density is then determined as 1718 galaxies per square degree on the sky.

We notice very few pairs of galaxies in this sample, one, a set of faint early ellipticals at z = 123.6, y = 90.3 and another a set of lenticulars apparently super­ posed at z = 132.8, y = 98.9. There appear to be several elliptical galaxies with a corona such as the one located at z = 128.6, y = 101.1. The Cluster Catalogue 195 §3.2

GALAXY CLUSTER 037 21 55 17 - 6 0 35

« •

♦ « f

Figure S.2.S7 (aj Field of GALAXY CLUSTER 057: SI 55 17 -60 S3 The Cluster Catalogue 196 §3.2

GALAXY CLUSTER 037 21 55 17 - 6 0 35

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTI0N ft. 1 .

E •-tj I

• n . i

LEGEND; io= ’

CLUSTER MAGNITUDE DISTRIBUTI0N P 0 5 T I0N A TR IB U TI0N 100. to.

80 .

TO.

SO.

2 0. 1

1 0 .

E TÆTA (DECREES] M c u. o EESESSSiSiSSr : 3 : ; 5 ; n : H 5 H H H :

Figure 3.2.37 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 197 §3.2

(smrr ausTER 037 21 55 i? -ea as CflHXT CLUSTER 037 21 55 17 -6 0 35 CflLflXT CLUSTER 037 21 55 17 -SO 35

3 i

GALAXY CLUSTER 037 21 55 17 -60 35

FIELD 148 ES0/SERC PLATE JE201

X Y RA DEC L B z ■18501 119501 tlBSOl IISSOI 098.536 -032.830 21 55 17.4 -60 35 13.4 331 59 31.8 -45 51 3.0 0.048

M0RPH0L0GY D1SPERSI0N ELLIPSE CLUSTER MEMBERS

E 244 MAJ0R AXIS 14.41 SAMPLE P0PULATIBN 512

30 49 MIN0R AXIS 12.61 C0RE P0PULATI0N 173

S 20 2 ECCENTRICITY 0.48 L IM IT IN G MAGNITUDE 1 9 .0

SB n P0SN. ANGLE - 8 . 4 9

P 6

Figure 3.2.87 (f,g,h) Cluster Morphological Population Distributions. Table 3.2.37 Cluster Population Description.

GALAXY CLUSTER 087: 21 55 17 -60 85 : The cluster is located in the South-West quadrant of ESO/SERC Field 146. Within a diameter of 60mm as determined by mio we count 575 galaxies in this cluster and 512 to a limiting magnitude of = 19.0. The cluster is marginally classified Abell type R because of its high central condensation, but we do note some slight irregularities in the cluster membership distribution. T ie Cluster Catalogue 198 §3.2

We count 112 galaxies brighter than m 3 + 2 and thus classify the cluster as having an Abell richness of 2. We suggest a B — M type III classification for the cluster which has no major dominant galaxies, although several bright ellipticals are noted. For and mio we give 14.6,15.0 and 15.3, respectively. The value of mio implies a redshift of 0.048.

The cluster membership displays a somewhat extended distribution with high central condensation. The dense core of the cluster appears elongated and aligned with the minor axis of the dispersion ellipse. Several concentrations are noted near the cluster center and to the West as well as North of center. lu addition, we find a few concentrations at the North-East periphery of the cluster. The magnitude distribution rises rapidly from the brightest galaxies to a near plateau spanning almost two magnitudes. The bulk of the population resides in this range and may fuggest the possibility of a bright cluster superposed on a faint background. The position angle varies wildly with an excess noted in the number of galaxies West of North primarily caused by the peak indicating the North-South orientation.

We note the high concentration of elliptical galaxies in the sample, many of which are concentrated towards the center of the cluster. A large number of spiral galaxies are scattered throughout the cluster but without as high a central conden- lation as the ellipticals. The {E : SO : S) ratio is (1.0: 0.2 : 0.9) indicating some ten percent more ellipticals than spirals. The core population comprises nearly 84% of the sample and resides in an area of 0.2 square degrees. This yields a core surface density of 865 galaxies per square degree on the sky. Five bright elliptical galaxies in the sample appear to have coronas. The brightest of these is located at

X = —101.2, p = —36.8, and we find an interesting pair with a faint elliptical galaxy imbedded in the corona of a brighter one at x = —96.5, y = —51.8. Of the several peculiar galaxies seen we note an unusual barred spiral with a ring-like structure and a large spur or luminous bridge located at x = —91.7, y = —39.2. The Cluster Catalogue 199 §3.2

GALAXY CLUSTER 038 21 58 08 -6 0 11

Figure S.2.S8 (a) Field of GALAXY CLUSTER 0S8: 21 58 08 -60 11 The Cluster Catalogue 200 §3.2

GALAXY CLUSTER 038 21 58 09 - 6 0 11

SURFACE DENSITY DISTRIBUTI0N CLUSTER MEMBERSHIP AND M0RPH0L0GY #...... tt.

II. f I

». # -4. ■ •j5,i a W

LEGEND E = • : B0= • ■ L 5 * * i SB^ •

ERST m WEST *R8P86g2êR

CLUSTER MAGNITUDE DISTRIBUTI0N PI35ITÎ0N ANCLE 3I5TRIBUTI0N 25. 24.

5:5 18. %

13.

ë R s s B es

Figure S.2.88 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalopie 201 §3.2

c a j n CLUSTER 038 21 58 09 -6 0 11 OaflXT CLUSTER 038 21 58 09 -6 0 11 CRLHXT CLUSTER 038 21 58 09 -6 0 11

1

i i

I

GALAXY CLUSTER 038 21 58 09 -6 0 11

FIELD 146 ESB/SERC PLATE J620I

X Y RA DEC L B z (lesoi IlSSDI (18501 119501 080.549 -010.760 21 58 8.7 -60 11 45.0 332 14 19.1 -46 20 55.5 0.055

MORPHOLOGY DISPERSION ELLIPSE CLUSTER MEMBERS

E 149 MAJOR A X IS 9 .7 4 SAMPLE p o p u l a t io n 312

SO 43 MINOR A X IS 8 .6 3 CORE POPULATION 121

S 114 eccentricity 0 .4 8 LIMITING MAGNITUDE 19.0

SB 6 P0SN. ANGLE 6 3 .0 4

P 0

Figure 8.2.S8 (f,g,h) Cluster Morphological Population Distributions. Table S.2.S8 Cluster Population Description.

GALAXY CLUSTER 088: 21 58 08 -60 11 : The cluster is located in the South-West quadrant of ESO/SERC Field 146. Within a diameter of 45mm as determined by mxo we count 364 galaxies in this cluster and 312 to a limiting magnitude of miim = 19.0. The cluster is classified Abell type R because its high central concentration of elliptical galaxies.

We count 110 galaxies brighter than m 3 4- 2 and thus classify the cluster as T ie Cluster Catalogue 202 §3.2 having an Abell richness of 2. We suggest a B — M type I classification for the cluster which has a multiple cD type galaxy as its brightest member. For and mio we give 15.0, 15.4 and 16.0, respectively. The value of mio implies a redshift of 0.065.

We note the high central condensation of this cluster displaying a complicated density distribution. In addition we notice a concentration South of cluster center near the periphery of the dispersion ellipse.

The cluster magnitude distribution can be described as a rapid rise in the numbers of galaxies fainter thanm„ = 16.0 and then a gentler rise beyond m„ = 17.0 to the magnitude limit. The position angle distribution is somewhat chaotic and appears to show a slight preference for orientations West of North although this is motivated strongly by the peak near zero degrees.

We find the elliptical galaxies in this cluster strongly concentrated towards the center of the cluster. The spirals, on the other hand, appear less concentrated although there is a small group located South South-East of the cluster center. W e find an {E : SO : S) ratio of (1.0 : 0.3 : 0.8) indicating an increase of ellipticals over spirals of about twenty percent. The core population of this cluster represents nearly 39% of the sample residing in an area of 0.09 square degrees. This yields a cluster core surface density of 1307 galaxies per square degree.

We note a peculiar grouping of galaxies in the center of this cluster which is dominated by a bright cD type galaxy. The cD is apparently surrounded by several much fainter elliptical attendant galaxies in a tight group located at z = —79.1, y = —10.4. We also notice a very close pair of lenticular galaxies found at X = —77.7, y = —27.1, and a pair of ellipticals at z = —80.3, y = —9.6. The Cluster Catalogue 203 §3.2

GALAXY CLUSTER 039 22 01 11 - 5 8 18

«Vîÿie^sSs:?.'/

#'L-yr5T^%?r.')r.T!l^'.. f . . '

Figure 3.2.39 (a) Field of GALAXY CLUSTER 0S9: SS 01 11 -58 18 The Cluster Catalogue 204 §3.2

GALAXY CLUSTER 039 22 01 11 - 5 8 16

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTR1BUTI0N

MO. 5 i

«D.

lie . o . S

m. ■o #0.

S 0 = I S B " • m . m WEST c g g p e e s é

CLUSTER MAGNITUDE D IS T R IB U T I0 N P05ITI0N ANGLE ttH5TRIBUTI0N 100. 2S T f I—I r—%—I I I I—r ' I I—r- 24. 23. n. 22. 21. eo. 20. S' 29. 18. 70. 17. 16. eo, 15. 14. C#m3 n R 13. 12. 11. «g1 10. 8 . 8 . so. 7. 6. zo. 5. 4. 10 3. . 2. 1. y 0 . 0. « » _ ' I_I_u t—t * • I eoao*oooeeoaeooeoeE TICTA (DECREES) W eDP*p“ ffiUJinm^«"entn

Figure 3.2.89 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 205 §3.2

CPLAXY auSTER 039 2Z 01 11 -58 IB CFLflXT CLUSTER 033 22 01 11 -58 18 CHLRXY CLUSTER 039 22 01 11 -58 18

i 1

II ELLIPTICAL GALAXIES GALAXIES ■er ■or i

GALAXY CLUSTER 039 22 01 11 -58 18

FIE LD 146 ESB/SERC PLATE J62DI

X Y RA DEC L B 2 (IBSDI (1S50I (leSQI (19501 063.530 090.895 22 1 11.1 -58 18 36.8 334 23 10.0 -47 35 52.6 0.043

M0RPHBL0GY DISPERSIBN ELLIPSE CLUSTER MEMBERS

E 132 MRJ0R AXIS 1 6 .0 6 SAMPLE P0PULRTI0N 331

SB 56 MINBR AXIS 1 3 .7 7 C0RE PBPULRTI0N 90

S 131 ECCENTRICITY 0.51 LIMITING MAGNITUDE 19.0

SB g P0SN. ANGLE 5 9 .8 2

P 3

Figure 3.2.39 (f,g,h) Cluster Morphological Population Distributions. Table 3.2.89 Cluster Population Description.

GALAXY CLUSTER 039; 22 01 11 -58 18 : The cluster is located in the North-West quadrant of ESO/SERC Field 146. Within a diameter of 60mm as determined by ruio we count 374 galaxies in this cluster and 331 to a limiting magnitude of miim = 19.0. The cluster is classified Abell type I because of its inherent irregularity.

We count 62 galaxies brighter than + 2 and thus classify the cluster as The Cluster Catalane 206 §3.2 having an Abell richness of 1. We suggest a B — M type I II classification for the cluster which appears intermediate between prototypical cD dominated clusters and those with normal giant ellipticals. For m i,m s, and mjo we give 13.5,14.6 and 15.1, respectively. The value of mio implies a redshift of 0.043.

We find this irregular appearing cluster loosely bound and with numerous small condensations. The largest group lies just South of the cluster center, whereas other smaller groups are located to the East, South-East and North of the cluster center.

The cluster magnitude distribution rises slowly at first from the brightest galax­ ies through a span of over two magnitudes. From = 16.0 there is a steeper rise for another two magnitudes and then a gradual tapering of the distribution to the magnitude limit. The position angle distribution, although erratic, suggests a pref­ erence of the brighter galaxies to be oriented West of North with a peak near zero degrees. This direction is consistent with the direction of the major axis of the dispersion ellipse. We find the elliptical galaxies in this cluster to be widely scat­ tered with only few concentrations. The spirals are distributed similarly with the exceptions of a centrally located concentration and a zone of avoidance North of the cluster center. We note an [E : SO : S) ratio of (1.0 : 0.4 : 1.1) indicating a ten percent increase of spirals over ellipticals. The core population comprises only 27% of the sample and resides in an area of 0.24 square degrees. This yields a core surface density of 370 galaxies per square degree.

We notice several elliptical galaxies with coronas, in particular, a bright early elliptical with a fainter elliptical located in its corona found at z = —47.8, y = 95.3. We also note the diversity of spiral galaxies: several are found to possess ring-like structures such as the one located at z = —62.9, y = 114.4; and several are seen to be superposed as we find at z = —45.2, y = 82.8. We note a very peculiar galaxy a t z = —61.7, y = 78.3. The Cluster Catalogue 207 §3.2

GALAXY CLUSTER 040 22 01 07 - 5 0 18

“1

Figure 8.2.40 (a) Field of GALAXY CLUSTER O4O: 22 01 07 -50 18 T ie Cluster Catsdogue 208 §3.2

GALAXY CLUSTER 040 22 01 07 - 5 0 18

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTI0N

E I :

3 «a

;

•w. EAST S

CLUSTER MAGNITUDE O ISTR IB U TI0N P 0 5 IT I0 N ANGLE D I5T R IB U T I0N 100. 24.

n. 22.

BO,

■JO.

90. 7.5: 20.

10 .

0 . T>CTfl lOECREES) Ol/)OW90l/)OinOt/YOi/)OlAOIAOU>OI/>0M C N ITU O E RRtCE O)S0DC*‘ r^tDC&inul«V*rT)fY)fM(^2'^*«OO0)(7) 8 8 s si s S 8 5 s s

Figure 8.2.40 fbJ Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 209 §3.2

CRJ^XT CLUSTER MO 22 01 07 -50 16 CR.RXY CLUSTER MO 22 01 07 -50 18 GALAXY CLUSTER MO 22 01 07 -5 0 18

i

9 0 GALAXIES i 4 ^ ^ ^ H H 4 4 4 4 4

GALAXY CLUSTER 040 2 2 01 07 -50 18

FIELD 237 ESB/SERC PLATE J36SB

X Y RA DEC L B Z IIBSOI tlBSOI IISSOI IISSOI 0 0 8 . 125 -0 1 4 .4 0 4 22 1 6 . 9 - -50 18 11.9 345 35 47.8 -50 52 6.4 0. 042

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 117 MAJOR AXIS 1 6 .3 8 SAMPLE POPULATION 284

S0 22 MINBR AXIS 14.71 CORE POPULATION 93

s 137 ECCENTRICITY 0.44 LIMITING MAGNITUDE 19.0

SB 4 P0SN. ANGLE - 5 4 . 2 2

P 4

Figure 8.2.40 (f,g,h) Cluster Morphological Population Distributions. Table 3.2.40 Cluster Population Description.

GALAXY CLUSTER 040: 22 01 07 -50 18 : The cluster is located in the South-East quadrant of ESO/SERC Field 237. Within a diameter of 60mm as determined by mio we count 296 galaxies in this cluster and 284 to a limiting m agnitude of mum = 19.0. The cluster is classified Abell t>'pe R because of its central condensation and fairly regular scatter.

We count 15 galaxies brighter than ms + 2 and thus classify the cluster as T ie Cluster Catalogue 210 §3.2 having an Abell richness of 0. We suggest a B — M type I II classification for the cluster which has an intermediate appearance between the class cD and those clusters having as their brightest galaxies normal giant ellipticals. For m i,m 3 , and mio we give 12.6, 13.4 and 15.1, respectively. The value of mio implies a redshift of 0.042.

We find this cluster somewhat centrally condensed, with a small high density concentration right at cluster center. There also appear to be two other concentra­ tions to the North-East near the cluster periphery.

The cluster magnitude distribution rises steeply from the brightest members to a plateau over a magnitude in width terminating at m„ = 17.0 and then rising quickly once more to a peak at m„ = 17.5 and then falling somewhat rapidly to the magnitude limit. The position angle distribution shows a slight excess in position angles oriented East of North.

We find a relatively dense concentration of elliptical galaxies towards the center of the cluster, dominated by a group just South-West of center. The spirals appear to be more evenly distibuted with perhaps a small group located South-East of center. The {E : SO : S) ratio gives (1.0: 0.2 :1.2) indicating an excess of spirals over ellipticals of some twenty percent. The core population reflects some 33% of the sample in an area of 0.26 square degrees. This yields a core surface density of 350 galaxies per square degree.

We note only a single pair of close elliptical galaxies at z = 11.4, y = 13.3; and we see what appears to be a elliptical-spiral superposition at x = 16.6, y = —13.1. An unusual low surface brightness galaxy with a small bright nucleus and verj’ large faint envelope is seen at x = 18.5, y = 16.8. The Cluster Catalogue 211 53.2

GALAXY CLUSTER 041 22 19 59 - 5 0 23

♦ •

Figure 3.2.41 (a) Field of GALAXY CLUSTER 04I: 22 19 59 -50 2S The Cluster Catalogue 212 §3.2

GALAXY CLUSTER 041 22 19 59 - 5 5 23

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTR1BUTI0N

I f 1 1 1 I I I M M I J fei I >^7 t i t 1:4.1 j T W n

H7. 1£GEKD- C = • i 8 0 = ♦ ;

WEST S 9 g R s 3 wié£3iaap««

CLUSTER MAGNITUDE D IS T R IB U T I0N POSITION ANGLE DISTRIBUTION

■0 .

Ti€Tfl icecsresi o u, = g 8 e s 3 38 E 2 “ S 3 ;

Figure 8.2.41 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie CJuster Catalogue 213 §3.2

Ca.fiXT CLUSTER 04% 22 19 59 -55 23 CRLRXT CLUSTER M l 22 19 59 55 23 GALAXY [LUSTER M l 22 19 59 -55 23

•r

i i

I

i i

GALAXY CLUSTER 041 22 19 59 ■55 23

FIELD ISO ES0/SERC PLATE JS332

X Y RA DEC L B z fIBSDI 1:3501 (1B50I (19501 101.125 -022.117 22 19 59.2 -50 23 6.1 343 35 50.1 -53 37 12.6 0.04

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 16 3 MHJ0R A X IS I B . 63 SAMPLE POPULATION 348

50 2 5 MIN0R AXIS 12.67 CORE POPULATION 109

5 1 5 0 ECCENTRICITY 0.73 LIMITING MAGNITUDE 19.0

SB 9 P0SN. ANGLE 2 2 .8 3

P 1

Figure 8.2.41 (f,g,h) Cluster Morphological Population Distributions. Table 3.2.41 Cluster Population Description.

GALAXY CLUSTER 041; 22 19 59 -50 28 ; The cluster is located in the South-West quadrant of ESO/SERC Field 190. Within a diameter of 60mm as determined by mio we count 366 galaxies in this cluster and 348 to a limiting mag­ nitude of miim = 19.0. The cluster is classified Abell type I because of its irregular appearance and subgrouping; it appears to have three major concentrations.

We count 97 galaxies brighter than + 2 and thus classify the cluster as T ie Cluster Catalogue 214 §3.2 having an Abell richness of 2. We suggest a B —M type II-III classification for the cluster which has an intermediate population of bright galaxies that are intermediate between having no dominant galaxies and having giant ellipticals. For mi,m 3 , and mio we give 14.0, 14.3 and 14.9, respectively. The value of mio implies a redshift of 0.040.

This cluster appears somewhat elongated and has several obvious concentra­ tions. The main one is located just South-East of the cluster center. There are several smaller concentrations: South-West of the center near the periphery of the cluster; West of center; and a binary grouping North of center. The magnitude dis­ tribution rises in a serpentine manner from the brightest galaxies to a peak at about magnitude = 18.0 after which the distribution falls off rapidly. We notice that the cluster is almost devoid of verj' faint galaxies. The position angle distribution shows no very strong peaks and thus no significantly preferred orientation of the brightest galaxies. The population of elliptical galaxies is scattered throughout the cluster with a major concentration along the major axis of the dispersion ellipse just South-East of center. Likewise, the spiral population has a similar enhancement of numbers, albeit not as dense. We find the (E : SO : S) ratio to be (l.O : 0.2 : 1.0) giving a nearly equal distribution of ellipticals and spirals. The core population of the cluster represents some 31% of the sample residing in an area of 0.26 square degrees. This gives a core surface density of 419 galaxies per square degree on the sky.

We notice three pairs of ellipticals composed of an early and later member in very close proximity or superposed, the brightest of which is located at x = —117.6,ÿ = —24.8. A subgroup of many faint spirals is located at x = -122.3, y = —19.4. Finally, we call attention to several close pairs of what appear to be barred spiral galaxies with double nucleii located at x = —93.1, y = 4.1 and x = —81.9, y = -40.2. Tie Cluster Catalogue 215 §3.2

GALAXY CLUSTER 042 22 21 26 - 5 6 33

Figure 8.2.42 (a) Field of GALAXY CLUSTER Of2: 22 21 26 -56 S8 T ie Cluster Catalogue 216 §3.2

GALAXY CLUSTER 042 22 21 26 - 5 6 38

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTI0N

5 I O- O*

3

•MO. .# •I to. LEGEND G 0 = :o 8 B - •

EAST m WEST i(^£Sânar.a:

CLUSTER MAGNITUDE D IS T R IB U T I0 N P 0 5 IT I0 N ANGLE DISTRIBUTI0N too.

60.

60.

70. 2 4 e 0 w m aECT*

90.

20.

10.

E THETA (DECREES) W o U, o m : 3 ; : 5 : ; g : 5 H H ; H- H

Figure 3.2.42 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. Tie CJuster Catalogue 217 §3.2

C O .R X 1 aUSTER 042 22 21 2S -56 38 Ca.nXY auSTER 042 22 21 26 -5 6 38 CflLRXT CLUSTER 042 22 21 26 -56 36

i

5 8 C a S X IE S i i i t

GALAXY CLUSTER 042 22 21 26 -56 38

FIELO ISO ESB/SERC PLATE JS332

X Y RA DEC L B z Iiasoi U950I I1950I (tasoi 0B7.961 -088.514 2 2 21 25.9 -56 38 22.8 334 28 44.6 -50 47 22.1 0.043

MORPHOLOGY DISPERSION ELLIPSE CLUSTER MEMBERS

E 139 MRJ0R AXIS 1 5 .7 2 SAMPLE p o p u l a t io n 327

5 0 10 MINOR AXIS 1 2 .3 7 C0RE POPULATION 96

S 165 ECCENTRICITY 0.62 LIMITING MAGNITUDE 19.0

SB 11 P0SN. ANGLE - 7 7 . BO

P 2

Figure 8.2.42 f/,g,hj Cluster Morphological Population Distributions. Table S.2.42 Cluster Population Description.

GALAXY CLUSTER 042; 22 21 26 -56 38 ; The cluster is located in the South-West quadrant of ESO/SERC Field 190. Within a diameter of 60mm as determined by mio we count 352 galaxies in this cluster and 327 to a limiting magnitude of miim = 19.0. The cluster is classified Abell type [ because the cluster has no spherical symmetry and no marked central condensation.

We count 120 galaxies brighter than mj + 2 and thus classify the cluster as Tie CJuster Catalogue 218 §3.2 having an Abell richness of 2. We suggest a B — M type II-III classification for the cluster which has the brightest galaxies somewhat intermediate between giant ellipticals and normal ellipticals. For m i,m 3 , and mio we give 14.0, 14.6 and 15.1, respectively. The value of mio implies a redshift of 0.043.

We find this cluster somewhat elongated with a few general concentrations in the field. The main concentration is located just South of cluster center, and there are other smaller groups concentrated to the North-East of center near the cluster periphery.

The magnitude distribution rises smoothly from the very brightest galaxies to a plateau spanning nearly two magnitudes from about m„ = 17.0 to m„ = 19.0 with a peak at m^ = 18.0. The position angle distribution is rather erratic with slightly more contributions made from bright galaxies oriented East of North and with large peaks near zero and sixty degrees in the positive sense as well as near ninty degrees in the negative sense.

We notice the distribution of elliptical galaxies to be loosely scattered except for a subgrouping South of center and a slight density enhancement of the second quadrant. The spirals also appear to be scattered again with a slight subgrouping South of center. We find an (E : SO : S) ratio of (1.0 : 0.1 ; 1.3) indicating «. slightly spiral-rich cluster. The core population represents 29% of the sample enclosed in an area of 0.21 square degrees. This yields a core surface density of 448 galaxies per square degree on the sky. We notice several elliptical galaxies with coronas, the brightest of which is located at z = —64.5, y = —107.5. Several close pairs of elliptical galaxies are seen, like the pair at z = —76.2, y = —82.0; and amidst the diversity of spirals, several distressed pairs, as the one found at z = —116.5, y = —86.8 which has a luminous bridge between its members. Tie Cluster Catalogue 219 §3.2

GALAXY CLUSTER 043 22 22 36 - 5 6 OS

Figure 3.3.43 faj Field of GALAXY CLUSTER 04S: 22 22 36 -56 06 The Cluster Catalogue 220 §3.2

GALAXY CLUSTER 043 22 22 36 - 5 6 06

SURFACE DENSITY OISTRIBÜTI0N CLUSTER MEMBERSHIP AND M0RPH0L0GY » ft.

• f l. I I

-«.Ï 3 i

IfGEND.

8 0 = ' Ib=: - E A S T m I C 9 T , m m

CLUSTER MAGNITUDE D IS T R IB U T I0N P0SITI0N ANGLE DISTRÎBUTI0N too. 2 5 . 24.

•0. 2 2. 80. 19. 70. 1 7 .

1 3 . ^

2 0 .

1 0 .

0 . E TÆTfl (DECREES) ; ;

Figure 3.2.48 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The CJuster Catalane 221 §3.2

CaflïT CLUSTER 043 22 22 36 -56 06 GH.RXT CLUSTER 043 22 22 36 -58 06 CRLRXT CLUSTER 043 22 22 36 -56 05

i

30 GALAXIES

GALAXY CLUSTER 043 22 22 36 -56 06

FIELD ISO ESO/SERC PLATE JS 332

X Y RA DEC L B z (lasoi US5CI (1S5DI (19S0I 079.768 -059.436 22 22 36.0 -56 5 57.1 335 3 58.2 -51 12 57.0 0.043

MORPHOLOGY DISPERSION ELLIPSE CLUSTER MEMBERS

E IBB MAJOR AXIS 1 0 .8 9 SAMPLE POPULATION 313

SO 13 MINOR AXIS 9 .8 4 CORE POPULATION 99

S 120 ECCENTRICITY 0.43 LIMITING MAGNITUDE 19.0

SB 14 P0SN. ANGLE 7 7 .0 2

P O

Figure 3.2.43 (f,g,h) CluBter Morphological Population Distributions. Table 3.2.43 Cluster Population Description.

GALAXY CLUSTER 043: 22 22 36 -56 06 : The cluster is located in the South-West quadrant of ESO/SERC Field 190. Within a diameter of 45mm as determined by mio we count 334 galaxies in this cluster and 313 to a limiting mag­ nitude of mum = 19-0. The cluster is classified Abell type I because it appears more nearly linearly symmetric than otherwise; there are several cases of subclustering.

W'e count 72 galaxies brighter than -t- 2 and thus classi^’ the cluster as The CJuster Catalogue 222 §3.2 having an Abell richness of 1. We suggest a B — M type HI classification for the cluster which has no dominant galaxies. For 7ni,ms, and mio we give 14.1, 14.7 and 15.1, respectively. The value of mio implies a redshift of 0.043.

The cluster is slightly linearly condensed with concentrations found along the major axis of the dispersion ellipse. The major subclustering occurs a little East of South of the cluster center. There are other slight concentrations, but none as dense as the previously mentioned one.

We find the cluster magnitude distribution rising from the brightest members to a minor plateau about a magnitude and a half wide after which it rises more steeply to a peak near my = 18.0 and falls to the magnitude limit. Perhaps we see here the suggestion of a two-population cluster. The position angle distribution appears to be erratic and somewhat skewed to position angles East of North.

The population of elliptical galaxies is scattered throughout the cluster but with a linear concentration along the major axis of the dispersion ellipse. The spirals show a slight enhancement just South of the cluster center a little East of South. The {E : SO : 5) ratio gives (1.0 : 0.1: 0.8) suggesting a slightly elliptical- rich cluster. The core population represents nearly 32% of the sample and lies in an area of nearly 0.12 square degrees. This yields a core surface density of 839 galaxies per square degree on the sky.

We note six pairs of elliptical galaxies consisting of an early and late member, the brightest of which is located at x = —64.7,y = —73.9. Several of the elliptical galaxies are seen with coronas as we find at z = —77.8,%/ = —63.0. We also notice, amidst the diversity of spirals, several possessing ring-like structures such as the object located at z = —77.2, y = —51.9. Tie CJuster Catalogue 223 §3.2

GALAXY CLUSTER 044 22 24 46 - 3 0 52

Figure 8.2.44 fa) Field of GALAXY CLUSTER 044: 22 24 4 6 -SO 52 T ie Cluster Catalogue 224 §3.2

GALAXY CLUSTER 044 22 24 46 - 3 0 51

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTION

•le 5 I ■ O CD o •ô tÉm i tSss Ëiÿ èraSi

S 0 =

ERST WEST 8 G 8 S s 8 é S 8 §

CLUSTER MAGNITUDE DISTRIBUTI0N PO SITIO N ANGLE DISTRIBUTION too.

•0. eo. IS. IB. 70. n. 15.

90. ».

10.

TtETfl IDECREESl S S 2 g

Figure 8.2.44 (b) Clutter Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 225 §3.2

CfVlxr auSTER o n ZZ 24 46 -30 51 Ca.BX'r aUSTER dm ZZ 29 46 -30 51 CnjlXY CLUSTER 044 22 24 46 -30 51

i i

ELLIPTIC»- GALAXIES n r i i i i i i i i i i t i i i i i i t i i i i i

GALAXY CLUSTER 044 22 24 46 -3 0 51

riE L D 466 ES0/SEFÎC PlR•E J6436

X Y RB DEC L B H ciBsai iiesoi 119E0I (19501 -1 4 3 .5 1 1 -0 4 5 .1 2 5 22 24 46.3 - 30 51 4 2 . 7 017 55 41.2 -58 26 56.1 0. 038

M0RPHBL0CY DISPERSIONELLIPSE CLUSTER MEMBERS

E 105 MBJ0R AXIS 1 4 .6 9 SAMPLE POPULATION 226

S0 18 MIN0R AXIS 12.91 C0RE POPULATION 81

S 100 ECCENTRICITY 0 . 4 8 L IM IT IN G MAGNITUDE 1 9 .0

SB 2 P0SN. ANGLE - 8 0 . 0 7

P 1

Figure S.2.44 Cluster Morphological Population Distributions. Table 3.2.44 Cluster Population Description.

GALAXY CLUSTER 044: 22 24 46 -80 52 : The cluster is located in the South-West quadrant of ESO/SERC Field 468. Within a diameter of 60mm as determined by mio we count 229 galaxies in this cluster and 226 to a limiting magnitude of rnnm = 19.0. The cluster is classified Abell type RI because of its approach to central condensation even though somewhat scattered; it appears more nearly regular than irregular. The Cluster Gatalog'ue 226 §3.2

We count 73 galaxies brighter than ms + 2 and thus classify the cluster as having an Abell richness of 1. We suggest a B — M type II classification for the cluster which has as its brightest member a galaxy intermediate between the class cD and normal giant ellipticals. For mi,m 3 , and mio we give 13.5, 14.7 and 14.8, respectively. The value of mio implies a redshift of 0.038.

The cluster appears somewhat scattered, but has several density concentra­ tions the main one of which lies slightly East of the cluster center. Several smaller concentrations are noted, most of them lying North of center whilst a single small high density region lies South-East of the center of the cluster.

The cluster magnitude distribution rises in ramp-like fashion from the brightest galaxies in the cluster to a maximum near m„ = 18.0 and drops off rapidly half a magnitude later. The position angle distribution of the brighter galaxies shows no obvious trend; but a slight peak is found at orientations West of North.

We find the elliptical galaxies somewhat more concentrated towards the center of the cluster with their highest density in a region East of center. The spirals appear to have a similar distribution, albeit more sparsely scattered. The {E : SO : S :) ratio is ( 1 . 0 : 0 . 2 : 1 .0 ) giving a similar number of ellipticals and spirals in the cluster. The core population comprises nearly 36% of the sample contained in 0.21 square degrees. This yields a core surface density of 388 galaxies per square degree.

We note that the brightest galaxy in the cluster has a corona. There appears to be a small subgroup of elliptical galaxies located at 2 = —159.5,y = —50.3. Of the myriad and diverse spirals, we find several superposed such as those found at * = —140.3,1/ = —66.7 and at z = —136.1, y = —19.6. Several peculiar galaxies are seen such as the object located at 2 = -131.6, y = —17.9 which boasts a broken ring-like structure. The Cluster Catalogue 227 §3.2

GALAXY CLUSTER 045 23 16 35 - 4 2 22 j j 11 M 111 j 11 ; 1 i 1111 i 11111 M 1111111111111'l 111 i 11 u IJLI1111111 i 11 M 111 M I n ri rn \t \-\ . i r. ; :— - r —

♦ .

■ \ ï 1

s %

Figure 3.2.45 (a) Field of GALAXY CLUSTER 045: 2S 16 S5 -42 22 T ie Cluster Catalogue 228 §3.2

GALAXY CLUSTER 045 23 16 35 - 4 2 22

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTI0N

■ r y T ir T T T .»:! I I n i 'M ' tt t t t I h 11 > h I n n : I

- 110.

L £ G £ N D

ERST WEST iiim. c

CLUSTER MAGNITUDE OI5TRIBUTI0N P05ITI0N ANGLE DISTRIBUTIBN too.

2 2 .

19. 16.

16. 6 0 . 15.

13. 5 0 . 12. E

6 . a

oi/)0inoi/ioinoi/)o(/>04fî0i/)MRCHITUDE RANGE :i : p s 3 s ê E S

Figure 3.2.45 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 229 §3.2

e n j w CLUSTER m s 23 le as -42 22 GRLRXY CLUSTER M S 23 16 35 -4 2 22 CfiLBXT CLUSTER M S 23 16 3S -42 22 I

3 3

« •

ELLIPTICAL GALAXIES » G ALAXIES SPIRAL GALAXIES nr i t

GALAXY CLUSTER 045 23 16 35 -42 22

FIELD 347 ESB/SERC PLATE J2413

X Y RA DEC L B 2 ItBSCI 119501 (19501 (19501 - 0 7 5 .5 4 7 -126.152 23 16 35.3 -42 22 36.6 348 24 55.0 -65 59 2.5 0.030

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 2 8 3 MRJ0R AXIS 2 1 .6 0 SAMPLE POPULATION 565

S0 37 MIN0R AXIS 18.30 C0RE POPULATION 208

S 23 8 ECCENTRICITY 0.53 LIMITING MAGNITUDE 19.0

SB 15 P0SN. ANGLE - 4 5 . 6 6

P 12

Figure 3.2.45 (f,g,h) Cluster Morphological Population Distributions. Table 8.2.45 Cluster Population Description.

GALAXY CLUSTER 045: 23 16 35 -42 22 : The cluster is located in the South-West quadrant of ESO/SERC Field 347. Within a diameter of 90mm as determined by mio we count 591 galaxies in this cluster and 585 to a limiting magnitude of rrium = 19.0. The cluster is classified Abell type I because of its lack of spherical symmetrj’ and the presence of multiple nuleii, or sub clustering.

We count 120 galaxies brighter than mj + 2 and thus classify the cluster as T ie CJuster Catalogue 230 §3.2 having an Abell richness of 2. We suggest a B — M type HI classification for the cluster which has no dominant galaxies. For mi,m 3 , and mio we give 13.5, 14.2 and 14.8, respectively. The value of mio implies a redshift of 0.030.

We note a general tendency of subclustering in this cluster of galaxies. There appears to be a concentration of membership near the center of the cluster, but even this is made of several small groups. We point out a dense group lying North-East of center.

The cluster magnitude distribution shows nearly an exponential rise from the brightest to the faintest galaxies, peaking at about m„ = 17.5, after which there is a rapid fall with relatively very few found near the magnitude limit. The posi­ tion angle distribution is erratic with a few outstanding peaks with the major one showing an slight excess of orientation along the North-South direction.

We find the elliptical galaxies somewhat centrally condensed with dense sub­ populations near the cluster center and in particular to the South-West near the cluster periphery. We notice a more scattered distribution for the spirals save per­ haps for the very slight enhancement of numbers found just North of the cluster center. The {E : SO : S ;) ratio is (1.0 : 0.1 ; 0.9) giving an almost ten percent increase of ellipticals over spirals. The core population comprises some 35% of the sample and is located in an area of nearly 0.44 square degrees. This yields a core surface density of 478 galaxies per square degree on the sky.

With the diversity of the cluster in mind we point out several interesting mem­ bers; a tight group of bright ellipticals at * = -74.9, y = —119.8; a group of superposed peculiar galaxies at z = —63.4, y = —109.8; an early elliptical galaxy with a host of faint attendant galaxies at z = -52.7, y = —114.4; and a pair of peculiar galaxies with unusual ansae located at z = —46.5, y = —151.9. The Cluster Catalogue 231 §3.2

GALAXY CLUSTER 046 23 27 36 - 3 9 37 m i l rri 1111 ; i i i 1 1 rn ; I m 11111111 i"ri 1111111111 ij -| . l i i i i i i i i i 'i i i i t i t i i i i i i i m . i i u i l i i , , , ,...... —::

\T rcr.ji,-.-- \...

| : r , ' -r^ •* i' ' ' '*" *• 'AI p " ■ ‘ rj.,..' » I# . y. ;- •; -i*' "T - r- i l - , . ^ ' # * ■ * I * =F ' ' 2 - 5' 3 r ' ■ •-» ♦ ■. & • 1 ■ ' ....• •■ |^< ^ .• » f ^ ® . --•• ' «« ~ _-y - - - r ' - ^ V >■ Y* -... % • T il

J

#

. 4 :

S • I I ! I I I I ’ M [ I ■ I 1 - 1 t t 1 ' I I t I I M I M I I M t I I I I ; ' I : I I I I I : ■ '

Figure S.2.46 (a) Field of GALAXY CLUSTER O46: 8S 27 S5 -S9 S7 The Cluster Catalogue 232 §3.2

GALAXY CLUSTER 046 23 27 36 - 3 9 36

SURFACE DENSITY DISTRIBUTION CLUSTER MEMBERSHIP AND MORPHOLOGY •Q. tf. I I .O

m. i E

H.

• tl .

EAST » ? ? S

CLUSTER MAGNITUDE DISTRIBUTION PO SITIO N ANGLE DISTRIBU TIO N lOO.

28. 17. 16. 15. C M T S m 9ECTW

RBNGE TÆTReoeooooo IDECREESl 8 8 P 8 S 8 S 8 8 8 S S

Figure 3.2.46 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The CJuster Catalogue 233 §3.2

CflLHXr CLUSTER MG 23 27 36 -39 36 CaJXT CLUSTER MG 23 27 36 -39 36 CHLAXT CLUSTER M 6 23 27 35 -3 9 35

I

SPIRAL GALAXIES

4 4 4 i i * 4 4 * * 4 i 4 i i 1 4 ^ *

GALAXY CLUSTER 046 2 3 27 36 -39 36

F IE L D 3 4 7 E se/SE R C PLATE J2413

X Y RA DEC L 8 Z c i a s o i ( l a s o i I1B50I tissai 0 3 8 .7 9 4 021.784 23 27 57.5 - -39 37 6 . 8 351 47 3 6 .1 -6 9 14 1.1 0. 043

M0RPH0L0GY DISPERSIONELLIPSE CLUSTER MEMBERS

E 58 HRJ0R AXIS 8 . 8 5 SAMPLE P0PULATI0N 134

SB 7 MINOR AXIS 7 . 8 0 C0RE P0PULRTI0N 45

S 62 ECCENTRICITY 0.47 LIMITING MAGNITUDE 1 9 .0

SB 0 P0SN. ANGLE - 3 7 . 2 9

P 7

Figure S.2.46 (f,g,h) Cluster Morphological Population Distributions. Table S.2.46 Cluster Population Description.

GALAXY CLUSTER 046: 2S 27 S6 -S9 ST : The cluster is located in the North-East quadrant of ESO/SERC Field 347. Within a diameter of 36mm as determined by mio we count 138 galaxies in this cluster and 134 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type I because of its lack of spherical symmetry and due to its mild, but multiple, subclustering.

We count 62 galaxies brighter than mj 2 and thus classify the cluster as The Cluster Catalogue 234 §3.2 having an Abell richness of 1. We suggest a B — M type I classification for the cluster which has a dominant cD type galaxy located near the cluster center. For nil,m s, and mio we give 13.4,15.1 and 15.3, respectively. The value of mio implies a redshift of 0.049.

We notice that the cluster is mildly centrally condensed with slight condensa­ tions immediately surrounding the center. A somewhat high density grouping lies North of the center of the cluster near its periphery.

The cluster magnitude distribution shows a gentle rise from the brightest galax­ ies to a maximum near m„ = 17.5 afer which it rapidly falls off. The position angle distribution shows little preference for orientation save for the slight excess in the North-South direction.

W^e find the elliptical galaxies in the cluster to be slightly more concentrated in the Southern portions of the cluster with a preference for the third and fourth quadrants. The spirals, on the other hand, appear to be slightly more concentrated towards the center of the cluster. The [E : SO : S) ratio is (1.0 : 0.1 : 1.2) suggesting a slightly spiral enriched cluster.

The core population comprises almost 34% of the sample, and resides in an area of nearly 0.08 square degrees. This yields a core surface density of 592 galaxies per square degree on the sky.

We note several galaxies in this cluster that possess ring-like structures such as the objects located at x = 35.4, y = 7.8 and x = 50.9, y = 24.4. In addition we point out that there are several peculiar galaxies in the cluster such as the one found at X = 24.9, y = 27.7. The Cluster Catalogue 235 §3.2

GALAXY CLUSTER 0 4 7 23 34 24 - 6 9 35

• #

Figure 3.2.47 (a) Field of G A L A X Y CLUSTER 047: 2S S4 24 - 69 S5 The Cluster Catalogue 236 §3.2

GALAXY CLUSTER 047 23 34 24 - 6 9 34

SURFACE DENSITY DI5TRIBUTI0N CLUSTER MEMBERSHIP AND M0RPH0L0GY m.

«7.

3 t4.

Jl---- I

(ASTICST t S

CLUSTER MAGNITUDE D ISTR IB U T10N P0SITI0N ANGLE DISTRIBUTI0N 100. 25. 24. to.

•0. 20. g - w. m

n. zc.

1 0 .

0 . TICTB I DECREES: o RAN% ^ oveeeoeooeoo e s r> r*> (o CD tn tn 2 I

Figure 3.2.47 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. The Cluster Catalogue 237 §3.2

CfUXT CLUSTER M7 ZS 34 24 -S3 34 Cftflxr CLUSTER 047 23 34 24 -6 9 34 CHLflXT CLUSTER 047 23 34 24 -6 3 34

i i

ELLIPTICAL Ca-PXI£S # f # * f 4 $ f ^ '

GALAXY CLUSTER 047 23 34 24 -69 34

FIELD 077 ESa/SERC PLATE J3564

X Y RR DEC L B Z (1S50J UBSOI tISSOI (13531 038. 221 025.705 23 34 24.3 - 69 34 4 3 .5 312 19 10.5 -46 27 4.8 0 .0 57

M0RPH0LBGY D15PERSI0N ELLIPSE CLUSTER MEMBERS

E 76 MRJ0R AXIS 10.77 SAMPLE P0PULRTI0N 149

50 20 MIN0R AXIS 9 .3 0 C0RE P0PULATI0N 43

S 47 ECCENTRICITY O.Sl LIM ITING MAGNITUDE 19. 0

SB 6 P0SN. ANGLE 25.49

P 0

Figure S.2.47 (f,g,h) Glueter Morphological Population Distributions. Table 8.2.47 Cluster Population Description.

GALAXY CLUSTER 047: 28 84 24 -69 85 : The cluster is located in the North-East quadrant of ESO/SERC Field 077. Within a diameter of 45mm as determined by mio we count 258 galaxies in this cluster and 149 to a limiting magnitude of miim = 19.0. The cluster is classified Abell type I because of its lack of spherical symmetry and the presence of multiple subclustering.

We count 42 galaxies brighter than mj -f 2 and thus classifj' the cluster as The Cluster Catalogue 238 §3.2 having an Abell richness of 0. We suggest a B — M type HI classification for the cluster which has no dominant galaxies. For mi,ms, and m io we give 15.1, 15.4 and 15.7, respectively. The value of mio implies a redshift of 0.057.

We find the cluster somewhat scattered in appearance, with several density concentrations to the North, East and West of cluster center. Several others abound as is noticed, for example, just South of center.

The cluster magnitude distribution suffers a slow rise from the brightest cluster members to the faintest in a steady increase. The position angle distribution shows a few dominant peaks most notably the slight excess West of North at about 35 degrees in the negative sense.

We notice the elliptical galaxies in several concentrations, one near the center of the cluster and another at a location North of center. There appears to be a relative paucity of elliptical galaxies in the third and fourth quadrants. The spiral galaxies, on the other hand, appear in larger numbers towards the outskirts of the cluster. The (E : SO : S) ratio gives (1.0 : 0.3 : 0.7) indicating a 30% increase of ellipticals over spirals. The core population comprises nearly 29% of the sample and is contained in an area of 0.11 square degrees. This gives a core surface density of 390 galaxies per square degree on the sky.

We count eleven close faint pairs of galaxies in the sample the brightest of which lies at z = 20.2, y = 33.2; these are typically composed of an early and a later elliptical. A number of the galaxies in the cluster appear superposed such as the object located at z = 29.7, y = 16.7. Finally, we note the presence of several distressed galaxies such as that seen at z = 49.5, y = 13.8. Tie Cluster Catalogue 239 §3.2

GALAXY CLUSTER 0 4 8 23 3 8 42 - 3 0 30

##

Figure 3.2.48 (a) Field of GALAXY CLUSTER O48: SS S8 42 -SO SO T ie Cluster Catalogue 240 §3.2

GALAXY CLUSTER 048 23 38 42 - 3 0 30

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTION m M i I :

-II -e 1 i Î

A LBGEKD^ C = • i I 8 0 = • i % S » * I S B = • :

EAST m 9 n s s s e s .JaSJm

CLUSTER MAGNITUDE D I5 T R IB U T I0 N P0SITI0N ANGLE DI5TRIBUTIBN too.

0 0 . 22.

BO. 20. g 1 9 . X

1 5 . 2 - H. ®- 1 1 3 . 12. E- 1 ir. E . 0 0 . 2 . t 20. ■n 10.

0. ooeoThCTfi o eooo (DEGREES: e 2 8 R S 8 S

Figure 3.2.48 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. Tie Cluster Catalogue 241 §3.2

Cfmxr n-lBTCT MB 23 38 42 -30 30 CajXT CLUSTER MB 23 38 42 -30 30 CRLHXT CLUSTER 04B 23 38 42 -30 30 I

99

I

GALAXY CLUSTER 048 2 3 38 42 -3 0 30

FJEU J 471 ESa/SERC PLHTE J613B

X Y RR DEC L B Z riB soj 119501 I19S0I tlSSOI -086.52B -026.639 23 38 44.8 -30 30 4.2 017 24 7.9 -74 20 20.9 0. 044

M0RPH0L0GY DISPERS10N ELLIPSE CLUSTER MEMBERS

E 113 MRJ0R AXIS 16.03 SAMPLE POPULATION 249

30 15 MIN0R AXIS 12.45 C0RE P0PULRTIBN ■ 95

S 113 ECCENTRICITY 0 . 6 3 LIMITING MAGNITUDE 1 9 .0

SB 4 P0SN. ANGLE 7 . 12

P 4

Figure 8.2.48 (f,g,h) Cluster Morphological Population Distributions. Table 8.2.48 Cluster Population Description.

GALAXY CLUSTER 048; 23 8 8 42 -80 80 : The cluster is located in the South-West quadrant of ESO/SERC Field 471. Within a diameter of OOnim as determined by mio we count 266 galaxies in this cluster and 249 to a limiting magnitude of rniim = 19.0. The cluster is classified Abell type I because of its lack of spherical symmetry and the presence of several concentrations in the body of the cluster. The Cluster Catalogue 242 §3.2

We count 65 galaxies brighter than mj + 2 and thus classify the cluster as having an Abell richness of 1 . We suggest a B — M type I classification for the cluster which has a dominant centrally located cD galaxy. For m i,m 3 , and mio we give 14.6, 14.8 and 15.1, respectively. The value of mio implies a redshift of 0.044.

We note the elongation of the cluster and its several density concentrations. A somewhat linear concentration of galaxies to the East of center appears to run diagonally from South-East to North-West. There is another concentration just South of this feature as well as a pair North and South of its North-West pole. The cluster magnitude distribution shows a gentle rise to a maximum from the brightest galaxies in the cluster to about m„ = 18.0. It then falls off slightly. We point out that the distribution appears somewhat bifurcated and may indicate, along with the several density concentrations, a multi-population cluster. The position angle distribution for the brighter galaxies seems skewed to an excess of galaxies oriented East of North.

There appears to be a higher concentration of elliptical galaxies towards the center of the cluster as opposed to the outskirts, with a slight enhancement in the area of the Eastward density concentration mentioned earlier. There seems to be a relative scarcity of elliptical galaxies in the second quadrant. The spiral galaxies seem to follow a similar pattern with a slight concentration of their numbers Eastward of cluster center. The (E : SO : S) ratio is (1.0 : 0.1 : 1.1) suggesting nearly a ten percent increase of spirals over ellipticals in this cluster. The core population comprises some 38% of the cluster sample and resides in an area of 0.22 square degrees. This yields a core surface density of 432 galaxies per square degree on the sky.

We note that the brightest member of the Eastern concentration lies at z = —76.2, y = —24.9 and appears to be an elliptical galaxy with a corona. Tie Cluster Catalogue 243 §3.'

GALAXY CLUSTER 0 4 9 23 44 55 - 2 8 25 j 1111 M 11 ] 11 ■ 1T) T. I jT I’ll 11111 j 1111,111 1, 11111111111111111111u ILi 1111111 ) 11111111 ; 11111 rp'iTrp'rri 111 111 i rrj 111111111i; i 11... [., N

• •

* I I ♦

w . ■

- 0 • — % ♦

: T I ' l I ' I ■ I ' T T i : I ! 1 ' ' I I ' t 1 I I I t ■ i T i 4 i I I i I I ■ , $ , i...... > n i i i t t : i i t t i i * i I ' i i : i i . i i '

Figure 8.2.49 (a) Field of G A LA X Y CLUSTER 049: SS 44 55 -28 25 The Cluster Catalogue 244 §3.2

GALAXY CLUSTER 049 23 44 55 - 2 8 24

CLUSTER MEMBERSHIP'miÿ) M0RPH0L0GY . SURFACE DENSITY DISTRIBUTION

***»9 S ° ° i e g e n d ;

' Î It m i« t I !♦ n I Kt 1 t* I I * t . i . i . i t i 11 f , I t , '

ERST WEST

CLUSTER MAGNITUDE DI5TR1BUTI0N too. POSITION RNG DISTRIBUTION

0 0 . to.

TO.

: i X. n .

10.

0 , •nCTfl I DECREES! m . « . RgKE^ ...... E25DC;S!2!2ïiSÏ22Sîi

Figure 3.2.49 (b) Cltister Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 245 §3.2

CHLRXr CLUSTER 0 4 9 23 44 55 - 2 8 24

i

I

GALAXY CLUSTER 049 23 44 55 -28 24

FIELD 471 ES0/SEFC Pl BTE J613B

X Y RP □EC L B Z C1850I (19501 (19501 (ISSOI - 0 1 5 . 47 9 0 8 5 .9 9 5 23 44 55.4 - 28 24 4 2 .6 025 10 13.4 -75 49 4.7 0 . 023

MORPHOLOGY D ISPER SIO N ELLIPSE CLUSTER MEMBERS

E 62 6 MAJOR A X IS 2 7 .0 3 SAMPLE POPULATION 1140

50 97 MINOR AXIS 25.34 CORE POPULATION 409

S 324 ECCENTRICITY 0.35 LIMITING MAGNITUDE 1 9 .0

SB 66 P0SN. ANGLE 3 2 .8 1

P 27

Figure 3.2.49 (f,g,h) Cluster Morphological Population Distributions. Table 3.2.49 Cluster Population Description.

GALAXY CLUSTER 049: 28 44 55 -28 25 : The cluster is located in the North-West quadrant of ESO/SERC Field 471. Within a diameter of 120mm as determined by mjo we count 1260 galaxies in this cluster and 1140 to a limiting magnitude of rnnm = 19.0. The cluster is classified Abell tj'pe R because of its strong central concentration and tendency to be sphericall symmetric.

We count 68 galaxies brighter than mj + 2 and thus classify the cluster as The Cluster Catalogue 246 §3.2

having an Abell richness of 1 . We suggest a B — M type I-II classification for the cluster which has an intermediate appearance with several bright normal giant elliptical galaxies near the central regions of the cluster. For m i,m 3 , and mio we give 12.5, 13.1 and 13.6, respectively. The value of mio implies a redshift of 0.023.

This large rich cluster appears centrally condensed with the central regions re­ solved into a myriad of minor density enriched groups of galaxies. The concentration located at the center of the cluster appears somewhat elongated and slightly inclined North of West. The cluster magnitude distribution rises nearly exponentially from the brightest cluster members to a peak near m^ = 16.0 where the distribution falls oflf some 30%, suffers a change in slope and rises again to the magnitude limit. Since the numbers of faint galaxies are very large we may be seeing the effects of our cluster being superposed on a faint background of galaxies, but to resolve that question we require a series of nearby galaxy counts to determine the background. The position angle measurements suggest an excess of orientations East of North in this case.

We notice a certain clumpyness to the distribution of the elliptical galaxies in this cluster in particular near cluster center. We note also, a peculiar avoidance by these galaxies of the interior first quadrant. The spiral galaxies seem to be more uniformly scattered throughout the cluster. We find an {E : SO : 5) ratio of (1.0 : 0.2; 0.7) suggesting a nearly 30% increase of ellipticals over spirals. The core population embraces some 36% of the sample in an area 0.75 square degrees. This yields a core surface density of 542 galaxies per square degree on the sky.

We note thirty-nine objects close enough to be considered superposed as well as thirty-five close pairs composed of what are generally an early and a late elliptical. We find several small groups dominated by a brightest elliptical with many faint attendants such as that found at z == —18.3, y = 76.4. The Cluster Catalogue 247 §3.2

GALAXY CLUSTER 050 23 59 06 - 4 4 07

J 11111 i 11111111111 i 111 i 1111 M 1111111111111 rn~n 1111' rriT n i ii 11 ri r m 111 111 i . i : : . : rrrr

.... ' , * - . .V ' • ' s . 1 ^ ^ - • •• • - - « ' r# .. . _ ;_V--r, '..y : V* .

-.ji ' . -JV.*.:- • ■ ■■

. • • - . W . . . . r4 .A S K '\ Z . , , .L/...- ...T . . . • ^ - - V— - ■« 4 -•■•* Jk

- r f -

. . ..I T 'A ■ ' - î - - ^ .* .» • - -j- - . f * -■ ......

" " P . * L . W U. ’ , 7 * % .«13 V ** »• ■ i* .. . .. I ' A «.• r . 4

“ t . 4 ' . *., t . . * • , . . . . « 4 .»«. * - # .« ..w . ..w ., .• - _ , . - .k . » “ ET. - ' • ' .••*••“ "k . •- ■ V-I'm "T- i’.-*. : '

' I * «. 4 v » *17 f/. ••'t' -.'•■•^'^' -•-

E # ' i - i » '«. • . .'TVi

t.: 7 .7 v '7 ^ :

1 E f' 4 ""

■ ■■'•■' - . 4 .'I/'- # L. ■■' • t - r t «

U ! : M ! t ' t t ) I I I I I ! ' ' I I 1 ! 1 I r ■ ' t I ^ ' I I I I ■ ' i , ' n ■ I I I ! Î M I ; I : ! I I I I ? I I I U I : I t I ■ t <

Figure S.2.50 (a) Field of GALAXY CLUSTER 050: 2S 59 06 -U 07 The Cluster Catalogue 248 §3.2

GALAXY CLUSTER 050 23 59 06 - 4 4 07

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTI0N

£ i o m. «V m. 00 3

Êhî ÏI

S 0 = ■o

ERST *EST ! 8 S 8 ? ? ? ? MM .WEST

CLUSTER MAGNITUDE DISTRIBUTION P05ITI0N ANGLE DISTRIBUTION 100. 2 4 . K.

8 0 . 1 3 . h

7 0 .

1 5 .

3 0 .

20.

10.

0 , eeeeeoooeeooTHETfl (DECREES) 3 3^32 ÎRS B 8 9 8 3 8 8 S

Figure S.2.50 (b) Cluster Morphology, (c) Surface Density Distribution, (d) Magnitude Distribution and (e) Position Angle Distribution. T ie Cluster Catalogue 249 §3.2

CRLflXY CLUSTER 050 23 59 06 -49 07 CaJXY CLUSTER 050 23 59 06 -44 07 GRLRXY CLUSTER 050 23 59 06 -4 4 07 I

a i

SPIRBL GRLflXIES fier fier Ml ICI 1

GALAXY CLUSTER 050 23 59 06 -4-4 07

FIELD 2 9 2 ESB/SEBC PLATE J4504

X Y RR DEC L B Z (195D1 119501 119501 119501 104. 7 9 4 0 4 7 .0 5 8 23 59 5.8 - 44 6 4 8 . 5 330 42 13.2 -70 30 40.1 0 .0 3 8

MBRPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 2 2 4 MBJ0R A XIS 15. 18 SAMPLE P0PULRTI0N 334

SB 30 MIN0R A XIS 1 3 .8 9 C0RE P0PULRTI0N 123

S 7 7 ECCENTRICITY 0 . 4 0 L IM IT IN G MRGNITUOE 1 9 .0

SB 2 P0SN. ANGLE - 4 0 . 0 6

P 1

Figure S.2.50 (f,g,h) Clugter Morphological Population Distributions. Table S.2.50 Cluster Population Description.

GALAXY CLUSTER 050; 28 59 06 -44 07 : The cluster is located in the North-East quadrant of ESO/SERC Field 292. Within a diameter of 60mm as determined by mio we count 342 galaxies in this cluster and 334 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type I because of its lack of spherical symmetry and presence of several concentrations indicating subclustering.

We count 43 galaxies brighter than mj -f 2 and thus classify the cluster as The Cluster Catalogue 250 §3.2 having an Abell richness of 0. We suggest a B — M type II classification for the cluster which has as its brightest galaxies those intermediate in appearance between class cD and normal giant ellipticals. For m i,m 3 , and mio we give 12.7, 13.4 and 14.8, respectively. The value of mio implies a redshift of 0.038.

The cluster appears somewhat elongated and has several noticable concentra­ tions, notably that immediately South of center and that East of center, which are the most dense and a number of less dense groups scattered throughout mainly the third and fourth quadrants of the cluster.

The cluster magnitude distribution appears somewhat bifurcated rising rapidly from the brightest galaxies to a small peak near m„ = 15.0 then falling to a trough a magnitude later only to rise rapidly to another peak near m„ = 18.0 after which it falls rapidly to the magnitude limit. This phenomenon may be interpreted as the possible superposition of two clusters. The position angle distribution is scattered, but suggests an excess in the numbers of bright galaxies oriented West of North.

We note the central condensation of elliptical galaxies and their paucity in the Southernmost regions of the cluster. The spirals appear to be loosely scattered throughout the cluster. We find the (E : SO : 5) ratio to be (1 . 0 : 0 . 1 : 0.4) indicating nearly sixty percent more ellipticals in this cluster than spirals. The core population comprises nearly 37% of the sample enclosed in 0.23 square degrees. This gives a core surface density of 530 galaxies per square degree on the sky.

We note a few pairs of galaxies in this cluster like that found at z = 120.9, y = 40.4. In addition, we find some peculiarities in some galaxies ranging from super­ position as we see at z = 98.0, y = 73.9 or structural peculiarities as is evident at

X = 79.1, y = 35.6. C H A PTER IV

AN ISOTHERMAL ANALYSIS OF CLUSTERS OF GALAXIES

Although the myriad things are many, their order is one. - Chuang-Tzu

One of the earliest attempts to determine the extent and population character­ istics of rich clusters of the “nebulae”, but excluding the Virgo Group of galaxies, was done by d’Arrest (1865) when he visually observed some twenty-five of the brightest nebulae in what is now known as the Coma cluster. Some time later nearly thirty such nebulae were catalogued in this area by Dreyer (1888) in his with an additional twenty listed in his Index Catalogues.

Some time later. Wolf (1901) photographed a minimally obscured region of the North Galactic Pole in the Constellation Coma Berenices and identified 108 nebulae within a circle of half a degree. This aggregate of galaxies, the Coma cluster, is considered a cluster prototype because of its richness, closeness and lack of obscuration. He continued his research and catalogued the positions of 1528 nebulae in the Coma field and described them in terms of Herschel’s system. Working in the

251 Isothermal Analysis 252 §4.0 same area with the 36-inch Crossley reflector at the Lick Observatory, Curtis (1918) counted some 304 galaxies in an area of only 40 x 50 minutes of arc and remarked that the region contained “the most remarkable aggregate of closely packed small nebulae known to me.”

While discussing the velocity-distance relation for galaxies Hubble and Huma-

8 on (1931) commented on the “sizes” of several clusters discovered till that time. These included the Perseus cluster studied by Wolf (1906), the Ursa Major cluster observed by Baade (1928), the cluster by Christie (1929) and the well-known clusters in Corona Borealis, Gemini and Cancer. The Perseus cluster was said to have some 500 nebulae within a radius of nearly one degree; the Coma cluster to have nearly 800 within a radius somewhat less than a degree; and the Leo and Ursa Major groups some 300 galaxies within radii corresponding to nearly 0.3 degrees.

The Coma cluster was given preliminary study by Lundmark (1927) to deter­ mine the distance and dimensions of the group and later, using Wolf’s material, Wallenquist (1933) gave the first study of the volume structure of the cluster. He discovered a strongly peaked number density profile common to member galaxies of differing . During the next decade Zwicky (1937c, 1941,1942a,b,c,d) carried out a systematic study of the distribution of galaxies in clusters which was to be the prototype of such analyses. For example, his examination of the Coma clus­ ter (Zwicky, 1937c) revealed 670 galaxies brighter than 16.5m within 160 arcminutes of the cluster center. He extended the total cluster membership to 1500 galaxies while noting that even 4.5 degrees from the cluster center the average projected number of galaxies still exceeded that of the surrounding field. He later claimed that as a result of studies to fainter limiting magnitudes (Zwicky, 1951) that the true population brighter than the limiting magnitude of 19.0 was detectable to a di­ am eter of nearly twelve degrees and contained some ten thousand galaxies. Zwicky maintained this point until 1972, in spite of the study by Oemler, Page and Wilson Isotbermal Analysis 253 §4.0

(1965) who assigned a diameter of about 100 minutes of arc to the cluster. It was to solve this dichotomy and after discussions with Zwicky in 1971 that Chincarini and Rood (1971) decided to study the extent of the Coma cluster by using redshifts. The hallmark result is the paper in Nature by Chincarini and Rood (1975) in which the first evidence of superclustering was discovered using the space distribution (i.e. R A , D and redshift) of galaxies.

The definition, however, of what is meant by cluster radii is not clear. Sim­ ilar to the distribution of light in globular clusters of stars, the projected surface density distribution of galaxies in clusters falls ofi" gradually and some realistic op­ erational definition should be agreed on. The observational situation is much more complicated because of the presence of an optically indistinguishable background population of galaxies and early size measurements were governed in part as to how conspicuously a cluster of galaxies stood out from its environment.

An attempt at modeling the distribution of galaxies in clusters was undertaken by Zwicky in 1937 when he noticed that the projected density distribution of the Coma cluster was similar to the luminosity distributions previously seen in elliptical galaxies by Hubble (1930). These approximated the distribution of mass in an isothermal gas sphere which refer to a self-gravitating assembly of mass points in hydrostatic equilibrium (Emden 1907). Subsequently, Zwicky (1957) found that the distributions of galaxies in Cancer, Hydra I and Perseus could likewise be interpreted by a bounded isothermal gas sphere model. The model was further extended by Bah call (1972,1973a,b,c, 1974a, 1975), Austin and Peach (1974a), MacGillivray et al. (1976), and others more recently. We mention in passing that the analysis of Zwicky of the Virial mass of the Coma cluster uncovered for the first time the mass discrepancy problem (or missing mass) in clusters of galaxies.

The isothermal procedures are based on the following relation (Bahcall 1972): Isothermal Analysis 254 §4.0

^(obs)(f) = or • J?(„o)(r/;3) + 7

where: H(cbs) and i 2 (t*o) are the observed and theoretical projected density distrbutions and or is a density normalization factor. ^ is a scaling factor in dis­ tance which relates the linear distance r from the center of the cluster to Emden’s dimensionless radius ( such that r = The term has been named the structural index of the cluster and is one of the primary cluster parameters. Values of i?(,so) as a function of ( have been tabulated by Chandrasekhar (1942) and Zwicky (1957, Table XXXV).

The values of ^ found by Zwicky (1957) were 22.4, 39.2, 40.5 and 52.3 jh kpc for the Cancer, Coma, Hydra I and Perseus clusters respectively and took this rather small spread as evidence that all regular clusters are similar in size and structure. Abell (1966), however, notes that the spread is practically over a factor of two. Nevertheless, the possibility of a consistent measure is attractive, and the idea was pursued further by Bahcall (1973a, 1975) who introduced the notion of the cluster core radius, Rc, as the angular radius at which the observed surface density of galaxies falls to one-half of its central value at which r = Zfi. For at least four of the five clusters Bahcall studied in 1973, the linear core radii were found to be within 15 percent of an average value even though their redshifts ranged over a factor of twenty. Later, in a fairly homogeneous sample of 15 low-redshift clusters she found similar agreement with the isothermal gas sphere model and an average linear core radius of Rc = (126 ± 23) Jh kpc. However, the matter is not clear; but the model is useful as a first approximation. We must point out that all clusters may not be stable and that in the final analysis. X-ray observations may be a better way to estimate the cluster potential. Nevertheless, it is this model that we have adapted to our analysis and is explained in detail in the next section. Isotbermal Analysis 255 §4.1

4.1 Theory of the Isothermal Gas Sphere

The theory of the isothermal sphere is well described, for instance, by Chan­ drasekhar (1942), and its application to clusters of galaxies by Zwicky (1957) but we follow the derivation of Chincarini (1980) to establish our method of analysis.

We consider a spherically symmetric distribution of mass in equilibrium as shown in Figure 4.1.1.

Figure 4.1.1 Idealized Isothermal Sphere of Galaxies

Using Poisson’s equation expressed in spherical coordinates we can write

" -4;rG f. (4 11) t C7Ç aÇ Isotberm al Analysis 256 §4.1

Because of spherical symmetry the radial part remains while the polar and azimuthal components vanish. We assume that the potential is entirely determined by the mass distribution and that the system is in hydrostatic equilibrium, so that

~ = -ffP- (4.1.2)

From the equation of state of an ideal gas we have

P = p y (4.1.3) and we derive , in terms of the density, the relation

Using dimensionless quantities we can write:

from which we obtain

P i(^0j + — 0. (4.1.6)

Tables exist for the solution of the above equation and we use that of Zwicky (1957) giving both the numerical solution and its projection on the celestial sphere. For small radii, however. King (1972) has shown that a good approximation is given by the relation -s/2 P (4.1.7) where J 2 e = 3^ with beta being a structural length. Isothermal Analysis 257 §4.1

Figure 4.1.2 Coordinate Projections on the Celestial Sphere

r* = with + 2 ®

The use of the above equation facilitates the visualization of its projection onto the celestial sphere as shown in Figure 4.1.2.

Using the relations + j/^ with Thus we can derive the projected surface density as

(4.1.8)

{i22 + r2 + z2)ï

Now; oo «a c+i->c = m * (4.1.9) L r(c)

BO we substitute

0 = 0, 0 = 2, c = |, = 1, m = r’ + Isotberm al Analysis 258 §4.1 to obtain (4.1.10) where (r is the projected density.

A special case of interest occurs when

g (r = Jig) _ 1

. Here, is called the core radius and is defined as the distance from the center of the cluster at which the projected density is 50% that of the central density. We use the isothermal formula to fit the observational data. The data are derived from ring counts which yield the number of galaxies per square degree as a function of the distance from the cluster center in minutes of arc.

In fitting the isothermal function we have several free parameters which need to be optimized. In particular, we write the density as:

p(r) = a»g(r/i9) + 7 (4.1.12) with q{rfP) the non-dimensional tabulated projected density, a a normalization constant which depends on the population in the cluster, and 7 , a quantity which is a function of the “background” and eventual cut-off radius. Oncea ,^ and 7 have been determined by minmizing the function we can estimate various cluster parameters. Isothermal Analysis 259 §4.2

4.2 Isothermal Fitting Procedure Utilizing

We choose a non-linear technique for fitting the surface density data to the required function

p(r) = a • g(r//3)-h 7 . (4.2.1)

Now, we can define a measure of goodness of fit

(4.2.2)

According to the method of least squares, the optimum values of the param­ eters Oj are obtained by minimizing x* with respect to each of the parameters simultaneously. That is,

-<>('■■11'} = “■ (4.2.3)

In our case, the parameters aj to be applied to the fitting function are a, the normalization constant; a core radius modification constant; and 7 , a “back­ ground” constant.

It is generally not convenient to derive an analytical expression for calculating the parameters of a non-linear function, so we consider x^ to be a continuous function if the n parameters oy describing a hypersurface in n-dimensional space where we search for the appropriate minimum value of x^ as shown in Figure 4.2.1.

One of the difiiculties of such a search is that for a given function there may be more than one local minimum for x* within a reasonable range of values for the parameters oy. Nevertheless, we begin by determining the variation of in the neighborhood of the starting point Xo> Isotbermal Analysis 260 §4.2

Figure 4.2.1 Function in an n-Dimensional Hyperspace

We compute the following derivatives of with respect to each of the chosen parameters and combinations of parameters oy:

dxo _ Xo(qt + Afli.gj) - Xq(q. - Aai,gy) (4.2.4) dai 2 A a , and ^^Xo ^ Xo(o, + Aai,gy) - 2xg(3.,aj) +Xo(q. ~ Aa.,ay) (4.2.5) ôa? Ao? and finally,

g^Xo ^ X o (q .- + A o„gy + Acy) - Xo(aj + Ao„oy) doidaj AOiAOy (4.2.6) _ Xo(a..Qj + Aoy) 4- Xo(o..Qj) Aa,-Aay where the Aoj are step sizes which must be large enough to prevent roundoff error in the computation and small enough to furnish reasonable answers near the minimum where the derivatives may be changing rapidly with the parameters.

In practice, we calculate doi/e, where c is some small integer 1 < e < 1 0 , and compute X* and its derivatives as described above monitoring its variation until Isotiermal Analysis 261 §4.2

X® begins to increase. The size of the increments is decreased still further if the first increment in a, does not yield a decrease in The last three points of the search are used to locate the minimum x^ by parabolic interpolation, provided uncertainties in the interpolation do not yield a higher value of than the lowest already found.

Since the solution of our fit is the result of a search along the x^ hypersurface rather than an exact analytical solution, there is no analytical form for the uncer­ tainties in the final values of the parameters. Following Bevington (1969) we use an algorithm which gives a reasonable definition of this uncertainty to approximate our error such that (4.2.7) and

Pi - (*"' )] (4.2.8) 3= 0 where ir® is the sample varaiance for the fit and u = N — n — 1 is the number of degrees of freedom after fitting N points with n + 1 parameters. Combining the above two equations, the uncertainty in the coeflBcient Oj is given by

(1.2.9) = 1 )

where Cjj(o’,- = 1 ) is the error matrix evaluated with Ci = 1 . Isotherm al Analysis 262 §4.3

4.3 The Isothermal Analysis

This section is concerned with the Isothermal Fitting of the surface density dis­ tribution of galaxy clusters. The general approach initially demands the calculation of a cluster’s surface density on the sky. We achieve this by the traditional means of ring counts, that is, by constructing a series of concentric annuli outwards from the cluster center and counting the number of galaxies found within the bounds of each annulus. The cluster center is that determined by the dispersion ellipse analysis. Once the counts have been performed the surface density is derived as the number of galaxies found per unit area of the annulus in question. The observed surface density is then corrected for “background” contamination from data derived from the predicted “field” count of galaxies on the ESO/SERC J-plates corresponding to limiting magnitudes calibrated on the assumption of z = 0 colors for elliptical galaxies as determined by Corwin (1985) and Rainey (1977).

Given the corrected surface density as a radial function of distance we can then apply our isothermal fitting function to the data. As a test of our procedure, we applied our analysis to Zwicky’s (1957) study of the Coma cluster of galaxies. Our results, particularly that of the core radius as determined by the parameter yield

P = 1.579 ±0.316.

In comparison, we quote the values obtained by Bahcall (1973) and Austin and Peach (1974) for the Coma cluster: P - 2.0 Bahcall (1973)

P = 1.75 ± 0.24 Austin and Peach (1974), and find our values in reasonable agreement.

In practice, however, we must point out that our method of analysis appears to be quite sensitive to starting values of the initial parameters and the non-uniform Isothermal Analysis 263 §4.3 radial distribution of surface density as a result of the effects of subclustering seen in a number of clusters in our sample. We also note that the x* fitting procedure experiences severe difficulty when test values of P are iterated to very small quan­ tities forcing a near divide-by-zero condition that is catastrophic to the calculating algorithm.

To offer the results of the Isothermal Fitting calculations, we present several informative plots of the data as an aid to understanding the observations and the scope of the analysis. The data are given in the following form:

1. Cluster Ring Counts. With the proper orientation of the positions of the cluster members, we locate the center of the cluster and proceed to draw concentric rings outward from the center of the cluster. The center is determined from the dispersion ellipse computations and the rings are drawn at two arcminute intervals to describe a counting annulus. The number of rings is derived from the average range along both the ordinate and absissa calculated from the positions of the most extended galaxies measured in the field. The resulting, generally rectangular shape, is then measured for both major and minor axes which are averaged to give a length which is then used as our maximum counting radius. Using this technique, we will often miss the outermost galaxies in our ring counts as can be seen in the plots.

2. Quadrant Counts. Given the positions of the cluster members and their relation to the cluster center we construct Cartesian axes with ordinate running North-South and absissa running East-West. Then, with the usual convention, we define the four quadrants in such a way that I:North-West, H:North-East, III:South- East, and IV:South-West. Once the orientations are set, we begin to construct in each quadrant an annulus that is t>'pically 2 . 0 minutes of arc in width and continue doing so to the maximum counting radius. We count all galaxies that fall within the bounds of each annulus terminating with the intersection of the annulus with Isothermal Analysis 264 §4.3 the ordinate and absissa defining the quadrant of interest. Given the number of galaxies within each annulus, or ring, we then plot a histogram and a smoothed curve through the data and this is displayed as four plots, one for each quadrant.

S. Cluster Strip Counts. As a qualitative tool, this plot is essentially a pair of orthogonal histograms that assist in determining the horizontal and vertical sym- metrj' of the cluster. The range of the plot is determined by the extrema of the data as described above and the observations are then segregated into 1 . 0 millimeter bins and counted. Once the counts have been performed, we plot a histogram of the data and using the observed count frequency and given bin width, determine the mean value and standard deviation of the mean. These values are used to plot a normally distributed probability curve through the data to give the eye a qualitative appre­ ciation of the distribution of the galaxy positions along each of the orthogonal axes. And by noticing peaks in the data, one can easily find, for instance, the location of concentrations in the cluster and also get some idea of the dispersion of the cluster members from the center of the cluster.

4. Cluster Surface Density. This histogram is a composite of the data found in the Quadrant Counts. For a given annulus, we count all galaxies found within its bounds and for all quadrants. The total count is then plotted as a histogram, the ordinate being the number of galaxies counted per annulus, and the absissa being the annulus number with each succeeding annulus extending radially away from the cluster center by increments of 2 . 0 minutes of arc.

5. Table of Data. The data table presents in numerical form the results of the preceeding operations. We give the ring, or annulus number, the total count of galaxies in that annulus, and the location of those counts in their respective quadrants. Next, we determine the counting radius as the one which, for a given annulus, divides it into sub-annuli of equal area. We then calculate the density Isothermal Analysis 265 §4.3 of galaxies within the annulus and express that density as the number of galaxies per square degree found in that circumscribed region. We also repeat the latter two data with the values of their logarithms. Finally, the total number of galaxies counted and the magnitude cutoff are given along with the coordinates of the cluster center and the ring width used for counting.

6 . The ho th erm d Fit. This plot uses the data from the preceeding table as the input to the Isothermal Fitting Procedure. This procedure attempts to minimize while independently varying three parameters. We plot the observations consisting of the cluster surface density as measured in units of galaxies per square degree agmnst the radial distance from the center of the cluster as measured in minutes of arc. The observed data is plotted as a broken line on a log-log scale. We then plot with a solid line the best fit from the isothermal analysis for the same input data, also on a log-log scale. Finally, we give the calculated value of the core radius in units of Mpc.

7. Cluster Parameters. The last table gives the calculated values of the cluster parameters and their variance. Beginning with the cluster identification, we display the isothermal fitting equation

p(r) = a«g(r/; 9 ) + 7

and the values and variance of the free parameters a, and 7 . We then print the best fit values of the parameters in equation form. Finally, we give the calulated core radius, Rc, of the cluster as determined by the isothermal fit in units of Mpc {H = 100/h kmfsecjMpc) and the cluster redshift, z, as determined by mio- IsotbermaJ Analysis 266 §4.4

4.4 Isothermal Analysis of Southern Galaxy Clusters

In this section we present a uniform description of the Isothermal Analysis of galaxies in our sample. Rather than publish the data in numerical form, we choose a graphical and tabular format for ease of comparison between cluster and cluster. The sample is magnitude-limited and uniform to = 19.0, In addition, ring-counts were performed uniformly with annulae of 2 . 0 arcminute widths. Isothermal Analysis 267 §4.4 GALAXY CLUSTER 001 00 00 46 - 3 6 19

CLUSTER RING C0ÜNTS = = EAST mmM N0RTH n i WEST :

== 20 MIN =z I

: * :

!!

= = E A S T S0Ü TH I W EST =

CUUOTCfT O TH ir C0UNTO

EAST I » north m i &CST == CLUSTER SURFACE DENSITY R B I N S = = I 5 0 . 40.

E 3 0 . S

2 5 . ë E 2 0 . “

n fllfWLUS NUMBER 12 RRCMIN WIDTH)

= CRST I SBirTH m m. NEST = : Figure 4.4.01. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 268 §4.4

GALAXY CLUSTER 001 00 00 46 -38 19

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAO) LOGfOEN)

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(RRCMIN) IGRL/SQOEG)

1 3 2 D 1 D 1 .259 1084.50 0.10001 3.03523

2 11 2 2 4 3 2.815 1325.51 0.44949 3.12238

3 16 4 2 3 7 4.539 1155.80 0.65698 3.06326

4 25 13 4 7 1 6.295 1291.08 0.79898 3.11095

5 17 3 7 2 5 8.061 682.84 0.90640 2.83432

6 20 5 4 4 7 9.833 657.28 0.9 9 2 6 7 2.81775

7 16 3 4 5 4 11.607 444.92 1.06472 2.64829

8 15 5 3 2 5 13.383 361.50 1.12655 2.55811

9 14 1 2 5 6 15.160 297.71 1.18069 2.47379

10 14 4 3 2 5 16.937 266.37 1.22885 2.42548

11 29 4 5 13 7 18.716 499.22 1.27220 2.69829

12 19 1 7 3 8 20 .4 9 4 2 9 8 .6 3 1.31163 2.47514

13 33 8 5 6 14 2 2 .2 7 3 4 7 7 .1 8 1.34778 2.67868

14 28 3 4 10 11 24.052 374.89 1.38115 2.57390

15 23 10 9 3 1 25.831 286.71 1.41215 2.45744

16 22 ID 7 4 1 27.611 256.55 1.44108 2.40917

17 16 9 6 1 0 2 9 .3 9 0 175.27 1.46820 2.24372

18 5 0 5 0 0 31.170 51.64 1.49374 1.71301

19 4 3 1 0 0 32.950 39.08 1.51785 1.59197

20 0 0 0 0 0 34.730 0.00 1.54070 0.00000

TOTAL NUMBER OF GALAXIES COUNTED = 330 MAGNITUDE CUTOFF. MV = 1 9 .0

CLUSTER CENTER AT XO = -3.684 YO = -69.349

RING WIDTH (RRCMIN) = 2 .0

Table 4.4.01. (a) Ring-Count Data Jar Galaxy Cluster 01. Isotbermal Analysis 269 §4.4

GALAXY CLUSTER 001 00 00 46 -36 19

ISOTHERMAL FIT pir) = a-q(r//5) + y

a 10 O UJo

00 Ù1 UJ 0 _ c n Œ ŒL3 10'

CORE RADIUS: Rc=3jg- 0.114 Mpc

RADIAL DISTANCE tARCMINUTES)

Figure 4.4.01. (e) hothermd Fit for Gdaxy Cluster 01. Isotbermal Analysis 270 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 001 00 00 46 -36 19

p(r) - a q(r//3) + y

a - 491.99 ±274.88 /S - l.G5±0.16 7 = 11.70±3.20

/ O ( r ) = 896. 43-q(r/l .04 ) + 12.36

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.114 Mpc Z = 0 .0 4 2

Table 4.4.01. (b) Cluster Parameters for Galaxy Cluster 01.

Using the cluster center as determined by the dispersion ellipse analysis, we count 330 galaxies within 19 rings of width 2.0 arcminutes and to the limiting magnitude ruv = 19.0. The East-West strip counts show a fairly smooth distribu­ tion along the absissa, perhaps with a little more deviation to the East, while the North-South distribution shows somewhat more scatter. The quadrant counts re­ veal the effect of subclustering as is evident in the extremities of the counting radii and apparent in all quadrants. The cluster surface density reveals a similar situa­ tion with an apparent bifurcation of the data. Rings 13 and 14 show considerable concentrations in the South-West quadrant.

The isothermal fit of this data is best in the regions of radial distance 1 0 ° ® < r < 10'-°. Near the “center" of the cluster, the surface density rises and falls and rises again giving a non-smooth distribution for the fitting. The large variance in the fitting parameters are likely due to this effect. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” from the mimimization procedure. Isotberm al Analysis 271 §4.4 GALAXY CLUSTER 002 00 03 14 - 3 5 04$

CLUSTER RING C0UNTS ram rsn : E R S T mmm N0RTH w WEST —

:= 20 MIN = Î!

N I r I

II

S == E R S T W EST ===

Cl_U3TCn 3TR ir C0UNT3 EAST m w N0RTH »»■ »C5T =

II CLUSTER SURFACE DENSITY

2 5 . g I i

{I ANNULUS NUfBER 12 BRW IN WIDTH)

= EAST mmm S8UTH «5T == Figure 4.4.02. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 272 §4.4

GALAXY CLUSTER 002 00 03 14 -35 04

HNG T0TAL QUADRANT C0UNTS C0UNTING 0BSERVED L0CIRAO) L0GIOEN)

JMBER C0UNT NW NE SE SW RADIUS DENSITY

(fiRCMIN) (GRL/SODEG)

1 8 1 5 0 2 1 .2 5 9 2 8 9 2.01 0.10001 3.46120

2 16 6 9 1 0 2 .8 1 5 1928.01 0.44949 3.28511

3 22 9 7 2 4 4.539 1590.61 0 .6 5 6 9 8 3 .2 0 1 5 6

4 20 9 7 3 1 6.295 1032.86 0.79898 3.01404

5 25 8 6 7 4 8.061 1D04.I7 0.90640 3.00181

6 28 9 5 7 7 9.833 920.19 0 .99267 2 .9 5 3 8 8

7 19 6 4 5 4 11 .6 0 7 528.35 1.06472 2.72292

8 35 15 12 3 5 13.383 843.50 1.12655 2 .9 2 6 0 9

9 37 9 11 5 12 15.160 786.80 I.18069 2 .8 9 5 8 6

10 25 6 5 5 g 16 .9 3 7 4 7 5 .6 6 1.22885 2.67730

11 26 0 8 5 13 18 .7 1 6 447.57 1.27220 2 .6 5 0 8 8

12 4 0 0 1 3 2 0 .4 9 4 6 2 .8 7 1.31163 1.79844

13 0 0 0 D 0 2 2 .2 7 3 0 .0 0 1.34778 0 .0 0 0 0 0

14 0 0 0 0 0 2 4 .0 5 2 0.00 1.38115 0 .0 0 0 0 0

T0TAL NUMBER 0F GALAXIES C0UNTEO = 265 MAGNITUDE CUT0FF. HV = 1 9 .0

CLUSTER CENTER AT XO = -3 5.B 21 YO = -3 .7 6 7

RING WIDTH fARCHINl = 2 .0

Table 4.4.02. (a) Ring-Count Data for Qalazy Cluster 08. Isotbermal Analysis 273 §4.4

GALAXY CLUSTER 002 GO 03 14 -35 04 1 0 ' ISOTHERMAL FIT p(r) = a-q(r//S) + y

O UJ or: ex a CO

Û-

CO UJ cc L3Π1 0 ^

CORE RADIUS: Rc=3/?~ 0.195 *h ^ Mpc

10 * 1 0 ° RADIAL DISTANCE (RRCMINUTESl

Figure 4.4.02. (e) Isothermal Fit for Galaxy Cluster OS. Isotbermal Analysis 274 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 002 00 03 14 -35 04

p(r) - a-q(r//S) + y

tx - 1648.92 ±393. 19 /S - 1.02±0.01 7 “ 10.01±0.00

p(r) = 2234.48-q(r/l.03 ) + 10.02

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.195 Mpc Z = 0 .0 7 2

Table 4.4.02. (b) Cluster Parameters for Galaxy Cluster OS.

Using the cluster center as determined by the dispersion ellipse analysis, we count 265 galaxies within 12 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. The strip counts in the East-West direction give a fairly uniform distribution along the absisa. The North-South ordinate appears more at variance dir to the effects of subclustering in this compact cluster. The quadrant counts reveal a rise in counts radially from the center except in the second, where we see a dramatic drop in counts beyond the second ring. The cluster surface density is seen to increase radially from center with the maximum number of counts seen in eighth and ninth rings.

The isothermal fit to this relatively smooth set of data appears to be fair, although somewhat dominated by the relatively high value for the central density. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 275 §4.4 GALAXY CLUSTER 003 00 06 49 - 3 5 43

CLUSTER RING COUNTS ran = = ERST ■■■ N0RTH ■■■ WEST

= 2 0 M IN =

SajTH WEST =

CLU3TCH 3TfTir C0UNT3 : C P 5 T mmu NBRTM w frCST == CLUSTER SURFACE DENSITY : B IN S = 5 0 .

35. g I I 25. Ë I

m W J L U S NUMBER 12 R R C M IN W IDTH!

— «M fn^m tDc**cooo = EBST Figure 4.4.08. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. IsotbermaJ Analysis 276 §4.4

GRLRXY CLUSTER 003 00 06 49 -35 43

RING T0TAL QUADRANT C0UNTS COUNTING 0BSERVEO L0G(RRD) L0GIDEN)

NUMBER C0UNT NW NE SE SW RADIUS DENSITY

(ARCHIN) IGRL/SODEG)

1 2 2 0 0 0 1 .2 5 9 7 2 3 .0 0 0 .1 0 0 0 1 2.85914

2 10 5 3 0 2 2.815 1205.00 0.44949 3.08099

3 16 12 2 1 1 4.539 1156.80 0.65698 3 .06326

4 19 7 3 2 7 6.295 981.22 0.79898 2.9 9 1 7 7

5 19 4 9 3 3 8.061 7 6 3 .1 7 0.90640 2.88262

6 34 6 13 10 5 9 .8 3 3 1117,37 0.99267 3.04820

7 42 11 14 14 3 11.607 1167.93 1.06472 3.06742

8 46 12 11 19 4 13.383 1108.60 1.1 2 6 5 5 3.04478

9 30 8 6 12 4 15.160 637.94 1.18069 2.80478

10 32 14 10 4 4 16.937 608.84 1.22885 2.78451

11 45 9 10 17 9 18.716 774.65 1.27220 2.88910

12 31 11 9 4 7 20.494 487.24 1.31163 2.68774

13 32 5 8 7 12 22.273 462.72 1.34778 2 .6 5 5 3 2

14 39 8 9 10 12 24.052 5 2 2 .1 7 1 .3 8 1 1 5 2.71781

15 29 9 9 3 8 25.831 361.50 1.41215 2.5 5 8 )1

16 26 2 8 9 7 27.611 303.19 1.44108 2.48172

17 25 8 4 4 9 2 9 .3 9 0 273.86 1.46820 2.43754

18 6 3 0 0 3 3 1 .1 7 0 6 1 .9 7 1.4 9 3 7 4 1.79219

19 0 0 0 0 0 3 2 .9 5 0 0.00 1.51785 0.00000

2 0 0 0 0 0 0 3 4 .7 3 0 0 .0 0 1 .5 4 0 7 0 0.00000

T0TAL NUMBER 0F GALAXIES C0UNTEO = 483 MAGNITUDE CUT0FF, MV = 1 9 .0

CLUSTER CENTER AT XO = -71.702 YO = -39.543

RING WIDTH (RRCMIN) = 2 .0

Table 4.4.08. (a) Ring-Count Data for Galazy Cluster OS. Isotbermal Analysis 277 §4 4

GALAXY CLUSTER 003 00 06 49 -35 44

ISOTHERMAL FIT p(T) = a-q(r//3) + y

a iq 3 CD OLU

l i ­ e n

CORE RADIUS; Rc=3jS~ 0.154 *h ^ Mpc

1 0 ° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.03. (e) Isothermal Fit for Galaxy Cluster OS. Isotbermal Analysis 278 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 003 00 06 49 -35 44

/D(r) “ ofq

a - 7 1 7 . 2 4 ± 4 1 9 . 1 8 /S - 1.05±0.15 y “ 50. 64j: 1.50

p(r) = 943. 23-q(r/l .03 ) + 50.54

CORE RADIUS; REDSHIFT: Rc=3/S~ 0.154 Mpc Z = 0 .0 5 7

Table 4.4.03. (b) Cluster Parameters for Galaxy Cluster OS.

Using the cluster center as determined by the dispersion ellipse analysis, we count 483 galaxies within 18 rings of width 2.0 arcminutes and to the limiting mag­ nitude niv = 19.0. The cluster strip counts reveal a fairly symmetric distribution of galaxies along the East-West absissa whilst the North-South ordinate shows nearly ten percent more scatter. The quadrant counts tend to show a general increase in population toward the extremities of the cluster, but with a noticeable void in the central regions of the cluster at the third quadrant. The cluster surface density rises sharply from cluster center and then falls off gradually. We notice several peaks in the distribution namely at rings 8 and 1 1 .

We find a general paucity of galaxies in the cluster center; the counts rise and then fall in that area. The largest inrease in density occurs near 1 2 arcsec from the center of the cluster and may seriously affect the isothermal fit. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the X* minimization procedure. Isotherm al Analysis 279 §4.4 GALAXY CLUSTER 004 00 07 29 - 5 7 15

CLUSTER RING C0UNTS Tuar == EAST ■ » N0RTH ■■■ WEST '

s= 2 0 MIN = II I

I : I I i

I II

= = E R S T W E S T =

Ct-UDTCn OTRir C0UNTO ERST B I NORTH n « ^ S T : CLUSTER SURFACE DENSITY n BINS = I

E

e

= ERST mm" SOUTH mm* Figure 4.4.04. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 280 §4.4

GALAXY CLUSTER 004 00 07 29 -57 15

RING T0TAL QUADRANT C0UNTS COUNTING 0BSERVED L0G(RRD) LBG(DEN)

NUMBER C0UNT NW NE SE SW RADIUS DENSITY

(ARCMINl IGAL/SQDEG)

1 1 1 0 0 0 1.259 361.50 0 .1 0 0 0 1 2.55811

2 12 2 1 7 2 2.815 1446.01 0.44949 3.16017

3 8 1 2 3 0 4 .5 3 9 4 3 3 .8 0 0.65698 2.63729

4 10 2 2 3 3 6 ,2 9 5 5 1 6 .4 3 0.79898 2.71301

5 15 5 3 5 2 8.061 602.50 0.90640 2.77996

6 16 4 5 1 E 9 .8 3 3 5 2 5 .8 2 0.99267 2.72084

7 7 2 2 1 2 11.607 194.65 1 .0 6 4 7 2 2 .28926

8 4 1 1 1 1 13.383 96.40 1.12655 1.98408

9 9 3 5 0 1 15.160 191.38 1.18069 2.28190

10 16 4 4 4 4 16.937 3 0 4 .4 2 1.22885 2.48343

11 9 6 1 0 2 18.716 154.93 1.27220 2.19013

12 6 3 2 0 1 20.494 9 4 .3 0 1 .3 1 1 6 3 1.97453

13 15 4 0 6 5 22.273 216.90 1.34778 2 .33526

14 11 4 2 3 2 24 .0 5 2 147.28 1.38115 2.16814

15 4 2 1 1 0 25.831 49.86 1.41215 1.59777

16 5 1 0 4 Q 27.611 58.31 1.44108 1.76572

17 3 1 0 1 1 29.390 32.86 1.46820 1.51672

18 1 0 0 1 0 31.170 10.33 1 .4 9 3 7 4 1.01404

19 1 0 1 0 0 32.950 9 .7 7 1.51785 0.98991

20 1 0 0 I 0 34.730 9.27 1.54070 0 .9 5 7 0 5

T0TAL NUMBER 0F GALAXIES C0UNTEO = 153 MAGNITUDE CUT0FF. MV = 1 9 .0

CLUSTER CENTER AT XO = -51.069 YO = -119.610

RING WIDTH (RRCMIN) = 2 .0

Table 4.4.04. faj Ring-Count Data for Galazy Cluster 04. Isotbermal Analysis 281 §4.4

GALAXY CLUSTER 004 00 07 29 -57 15 10 ' ISOTHERMAL FIT p(r) = a-q(r//S) + y

ne CD

ceLU =3Œ (nC3 Of LU û_

X CE L3CE

CORE RADIUS: Rc = 3^~0.119*h ^ Mpc

10 '

RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.04. fej Isothermal Fit for Galazy Cluster 04. Isotbermal Analysis 282 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 004 00 07 29 - 5 7 15

p(r) - £x q(r//S) + y

a~ 451. 15±247.89 /S - 1.05±0.16 y - 11.57±3.24

p(r) = 816.94 - q C r / l .04 ) + 12.07 •EST FIT *

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.119 Mpc Z = 0 .0 4 4

Table 4.4.04. (b) Cluster Parameters for Galaxy Cluster 04-

Using the cluster center as determined by the dispersion ellipse analysis, we count 153 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. Within this rather diffuse cluster the East-West strip counts reveal a less pronounced scatter than the North-South counts; but neither shows a small variance. The quadrant counts are low and erratic due to the diffuse nature of the cluster and the cluster surface density shows similar characteristics with rising and falling surface density as a function of radial distance from the cluster center.

The highest density of counts comes at rings 6 and 10.

The isothermal analysis tends to try to fit the observed distribution with an apparent bias towards the larger surface densities as seen in the preceeding figure. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 283 §4.4 GALAXY CLUSTER 005 00 18 08 - 4 9 32

CLUSTER RING COUNTS Tasrr % = £ R S 7 m m N0R TH mmm WEST

== 20 MIN = I ini s

s 1

ERST ■ S0UTM WEST =

CLUSTcr^ 3T m r c b u n t o E R S T m m »£RTH —" WEST =

CLUSTER SURFACE DENSITY

5 0 . = 1 MM B IN S —

1 5 . M.

5 5 . S

{ E 3 0 . I 35. Ë I 20.

1 5 . 10.

5 . I 0. II LP-^ flW W LllS NUMBER 12 HRCMIN WIDTH;

== ERST n > S O JTN m Figure 4.4.05. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 284 §4.4

GALAXY CLUSTER 005 00 18 08 -49 32

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOGIRAD) LOG(DEN)

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMINl IGAL/SOOEG)

1 12 8 0 1 3 1.259 4338.02 0.10001 3.63729

2 21 8 6 6 1 2.815 2530.51 0.44949 3.40321

3 25 9 9 16 4.539 1807.51 0.65698 3.25708

4 20 4 10 3 3 6.295 1032.86 0.79893 3.01404

5 18 6 4 5 3 8.061 723.00 0.90640 2 .8 5 9 1 4

6 28 4 4 13 7 9.833 920.19 0 .9 9 2 6 7 2 .9 6 3 8 8

7 22 2 5 9 6 11.607 611.77 1.06472 2.78559

8 15 3 6 5 1 13.383 361.50 1.12655 2.55811

9 21 4 6 6 5 15.160 445.56 1.18069 2 .6 4 9 8 8

10 18 5 5 3 5 16.9 3 7 342.48 1.22885 2.53463

11 12 8 0 1 3 18.7 1 6 206.57 1.27220 2 .3 1 5 0 7

12 2 2 0 0 0 20.494 31.43 1.31163 1.49741

13 0 0 0 0 0 22.273 0.00 1.34778 0.00000

TOTAL NUMBER OF GALAXIES COUNTED = 214 MAGNITUDE CUTOFF, MV = 1 9 .0

CLUSTER CENTER AT XO = 107.031 YO = 2 4 .6 1 7

RING WIDTH lARCMIN) = 2 .0

Table 4.4.05. (a) Ring-Count Data for Galazy Cluster 05. Isotbermal Analysis 285 §4^

GALAXY CLUSTER 005 00 18 08 -49 32 10' ISOTHERMAL FIT p(r) = a-q(r/^) + y

cn CD

on ΠO=3 c n

UJ o _ c n

c x CD

CORE RADIUS: Rc=3)S~ 0.131 Mpc

10 ' 10° RADIAL DISTANCE (ARCMINUTES!

Figure 4.4.05. feJ Isothermal Fit for Galaxy Cluster 05. Isothermal Analysis 286 §4 4

CLUSTER PARAMETERS GALAXY CLUSTER 005 00 18 08 -49 32

pCr) - a q(r//S) + y

CL - 3000.05 ±594.06 /S - 1.00 ±0.00 y - 13.06±0.63

p(r) = 3875.44-q(r/l.GO ) + 13.98

CORE RADIUS: RED SHIFT: Rc=3/S~ 0.131 Mpc Z - 0 .0 5 0

Table 4.4.05. (b) Cluster Parameters for Galaxy Cluster 05.

Using the cluster center as determined by the dispersion ellipse analysis, we count 214 galaxies within 12 rings of width 2.0 arcminutes and to the limiting magnitude m„ = 19.0. We note the high central condensation of this compact cluster as is shown by the cluster strip counts; there is a slightly larger dispersion in the North-South direction than along the East-West absissa, but a large peak rises out of the ordinate at a location spanning the cluster center. The quadrant counts show a strong enhancement of galaxies in the first quadrant near the center of the cluster; a large peak is seen in the third quadrant near the periphery of the cluster.

The cluster surface density shows a gradual rise to maximum density at ring 6 and then a quick fall.

The isothermal fit seems to mimic the data well at all radii and densities. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined firom the minimization procedure. Isothermal Analysis 287 §4.4 GALAXY CLUSTER 006 00 22 50 - 3 3 17

CLUSTER RING C0UNTS : E R S T mmm N0RTM — WEST :

z= 20 MIN — : I

:

i

= E R S T S0UTM I

CLU3TCR 3TKir C0UNT5

EAST N0RTH mmm tCST ==

CLUSTER SURFACE DENSITY I: B I N S s =

35. S

2 5 . ë E -X

c = ERST ■■■ S0UTH nm Figure 4.4.06. fa) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 288 §4.4

GALAXY CLUSTER 006 00 22 50 -33 17

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RADI L0G!DEfJ)

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMINl (GAL/SQOEG)

1 2 1 0 1 0 1.259 723.00 0.10001 2 .8 5 9 1 4

2 14 2 3 8 1 2.815 1687.01 0 .4 4 9 4 9 3 .2 2 7 1 2

3 17 5 4 3 5 4.539 1229.10 0 .6 5 6 9 3 3 .0 8 9 5 9

4 24 2 6 11 5 6 .2 9 5 1239.43 0 .7 9 8 9 8 3 .0 9 3 2 2

5 18 1 7 5 5 8 .0 6 1 723.00 0.90640 2.85914

6 16 3 5 6 2 9 .8 3 3 5 2 5 .8 2 0 .9 9 2 6 7 2.7 2 0 8 4

7 16 5 4 2 5 11.607 444.92 1 .0 6472 2 .6 4 8 2 9

8 8 2 0 4 2 13 .3 8 3 192.80 1.12655 2 .28511

9 20 5 5 G 4 15.160 4 2 5 .3 0 1 .1 8069 2.62869

10 27 6 7 8 6 16 .9 3 7 513.71 1.22885 2 .7 1 0 7 2

11 19 7 5 7 0 18.716 3 2 7 .0 7 1 .2 7220 2 .5 1 4 6 4

12 21 8 4 5 4 2 0 .4 9 4 330.07 1.31163 2.51860

13 24 7 9 2 6 2 2 .2 7 3 3 4 7 .0 4 1.34778 2.54038

14 20 8 3 5 4 2 4 .0 5 2 267.78 1.38115 2.42778

15 23 10 7 4 2 25.831 286.71 1.41215 2.45744

16 24 3 7 6 8 27 .6 1 1 279.87 1.44108 2.44696

17 16 7 4 3 2 2 9 .3 9 0 175.27 1.46820 2 .2 4 3 7 2

18 18 3 3 7 5 31.170 185.92 1.49374 2.26931

19 3 0 1 1 1 32.950 29.31 1.51785 1.46703

2 0 2 1 0 1 0 3 4 .7 3 0 18.54 1.54070 1 .26808

TOTAL NUMBER OF GALAXIES COUNTED = 335 MAGNITUDE CUTOFF, MY = 1 9 0

CLUSTER CENTER AT xo = 15 .2 7 2 YO = 94.597

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.06. faj Ring-Count Data for Galaxy Cluster 06. Isothermal Analysis 289 §4.4

GALAXY CLUSTER 006 00 22 50 -33 17

ISOTHERMAL FIT pir) = a-q(r//S) + 7

O ë Œcc Q CO lU

CO

CORE RADIUS: Rc = 3^~ 0.103 Mpc

RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.06. (e) Isothermal Fit for Galaxy Cluster 06. Isothermal Analysis 290 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 006 00 22 50 - 3 3 17

pCr) - a q(r//S) + y

a - 715. 43 ±436. 32 /? - 1.05 ±0.16 y ~ 11.71±3.20

yO(r) = 13B3. 33 •q(r/l.G4 ) + 12.39

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.103 Mpc Z = 0 .0 3 8

Table 4.4.06. [h] Cluster Parameters for Galaxy Cluster 06.

Using the cluster center as determined by the dispersion ellipse analysis, we count 335 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. This extended cluster displays a fairly large variance along both ordinate and absissa of the cluster strip count axes with a peak in the data somewhat East of the accepted cluster “center.” The quadrant counts show a general increase in number as a function of radial distance, in particular in the first quadrant. The surface density distribution appears to have two-population characteristics as it displays a bifurcated appearance.

The isothermal fit appears to match better at the periphery of the cluster and not as well near cluster center or at the major troughs in the data as is seen some 13 arcminutes from the center of the cluster. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isothermal Analysis 291 §4.4 GALAXY CLUSTER 007 01 29 34 -5 1 33

CLUSTER RING C0UNTS : e r s t b m N0RTH — WEST ==

= 2 0 M IN = I

: I II

== EAST 3 01/TH I W EST :

CLUSTER STR ir C0UNTS

: t o t —• N0fiTH NEST ==

CLUSTER SURFACE DENSITY c =1 m BINS = so.

4 5 .

4 0 .

3 5 . 5

3 0 . I 2 5 . 2 0 . 1 5 . i 10.

5 .

0.

_TL: ANNUL u s NUMBER (2 ARCMIN KIDTHJ

= ERST mmm S0UTH ■■■ NEST == Figure 4.4.07. faJ Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 292 §4.4

GALAXY CLUSTER 007 01 29 34 -51 33

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) LOG 1 DENI NUMBER COUNT NW NE SE SW RADIUS DENSITY (ARCMIN) (GAL/SQDEGl 1 4 2 0 2 0 1.259 1445.01 0 .1 0 0 0 1 3 .15 0 1 7 2 8 0 1 3 4 2.815 964.00 0.44949 2.98408 3 21 ID 2 7 2 4.539 1518.31 0.65698 3.18136 4 15 3 1 8 3 6 .2 9 5 7 7 4 .6 5 0 .7 9 8 9 8 2 .8 8 9 1 0 5 16 6 0 8 2 8 .0 6 1 6 4 2 .6 7 0 .9 0 6 4 0 2 .8 0 7 9 9 6 14 3 2 6 3 9 .6 3 3 4 6 0 .0 9 0 .9 9 2 5 7 2.66 2 8 5 7 14 2 5 2 5 11.607 389.31 1.06472 2.59029 8 22 7 4 3 8 13.383 530.20 1 .1 2 6 5 5 2 .7 2 4 4 4 g 22 3 9 5 5 1 5 .1 6 0 467.83 1.18069 2 .6 7 0 0 8 10 28 12 6 4 6 1 6 .9 3 7 5 3 2 .7 4 1.22885 2.72651 11 31 8 9 6 8 1 8 .7 1 6 533.64 1.27220 2.72725 12 15 2 4 1 8 20.494 235.76 1.31163 2.37247 13 14 2 7 2 3 2 2 .2 7 3 202.44 1.34778 2.30630 14 19 3 8 5 3 24.052 254.39 1.38115 2.40550 15 12 6 2 2 2 25.831 149.59 1.41215 2.17489 16 20 8 5 3 4 2 7 .6 1 1 233.23 1.44108 2.36778 17 6 0 0 3 3 2 9 .3 9 0 65.73 1.46820 1.81775 18 6 0 1 3 2 3 1 .1 7 0 6 1 .9 7 1.49374 :.79219 19 2 0 0 0 2 32.950 19.54 1.51785 1.29094

20 0 0 0 0 0 3 4 .7 3 0 D.OD 1 .5 4 0 7 0 0.00000

TOTAL NUMBER OF GALAXIES COUNTED = 289 MAGNITUDE CUTOFF. MV = 19 0 CLUSTER CENTER AT XO = 5 .7 7 4 YO = - 8 2 .2 5 9 RING WIDTH lARCHIN) = 2 . 0

Table 4.4.07. (aj Ring-Count Data for Galaxy Cluster 07. Isothermal Analysis 293 § 4 . 4

GALAXY CLUSTER 007 01 29 34 - 5 1 33

ISOTHERMAL FIT yo(r) = a-q(r//3) + 7

a

c n

CORE RADIUS; Rc=3jS~ 0.108 Mpc

10'

RflDIRL DISTANCE (ARCMINUTES)

Figure 4.4.07. fej Isothermal Fit for Galaxy Cluster 07. Isotbermaî Analysis 294 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 007 01 29 34 -51 33

pCr) - a q(r//S) + y

a - 728. 69 ±456. 34 /S - 1.05±Q.17 y - 11.72±3.29

p(r) = 1405.IG-q(r/1.04 ) + 12.37

CORE RADIUS; REDSHIFT: Rc=3/S~ 0.108 +h-i Mpc Z = 0 .0 4 0

Table 4.4.07. (b) Cluster Parameters for Galaxy Cluster 07.

Using the cluster center as determined by the dispersion ellipse analysis, we count 289 galaxies within 19 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. The cluster strip counts appear less variant along the East- West absissa, whereas along the North-South ordinate we find a much larger spread in the positional data. The quadrant counts are erratic at best, in particular in the first quadrant where we see three major peaks. There appears to be a general increase of surface density to about 19 arcminutes from center after which the density drops rapidly.

The isothermal fit is complicated by several dips in the data, especially that near the cluster center. We find the fit attempting to bridge the gap between the highs and lows in the data and settling on a compromise between them. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the X* minimization procedure. Isotbermaî Analysis 295 §4.4 GALAXY CLUSTER 008 01 39 50 -42 23

CLUSTER RING C0UNT5 : E flS T mmm N 0RTH mmm W EST =

s= 20 HIN =

I II

= = E A S T mm S0UTH mmm WEST —

CLUOTcrç D Tnir c b u n t o — E B S T miM MWrH >u NEST =

II CLUSTER SURFACE DENSITY E I

e 3 5 . È I

Œ É

flWM.US NUMBER 12 RRCMIN WIDTH)

=: ERST — 30UTM *mm N E S T = Figure 4.4.08. (aj Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 296 §4.4

GALAXY CLUSTER 008 01 39 50 -4 2 23 0

RING T0TAL QUADRANT C0UNTS COUNTING OBSERVED L0G(RAD) L8GIDEN1

JMBER C0UNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEGl

1 2 0 0 D 2 1.259 723.00 0.10001 2.85914

2 13 4 3 3 3 2.815 1566.51 0.44949 3.19493

3 15 6 3 3 3 4.539 1084.50 0.65698 3.03523

4 22 6 6 6 4 6.295 1136.15 0.79898 3.05543

5 14 2 5 3 4 8.061 562.34 0.90640 2.75000

6 15 4 2 4 5 9.833 492.96 0.99267 2.69281

7 19 4 3 5 7 11.607 528.35 1.06472 2.72292

e 16 3 5 5 3 13.383 385.60 1.12655 2.58614

9 16 5 3 5 3 15.160 340.24 1.18069 2.53178

10 14 2 8 3 1 16.937 266.37 1.22885 2.42548

11 25 S 1 11 4 18.716 430.36 1.27220 2.63383

12 25 11 5 5 4 20.494 392.94 1.31163 2.59432

13 12 3 3 5 1 22.273 173.52 1.34778 2.23935

14 6 2 2 1 1 24.052 80.33 1.38115 1.90490

15 0 0 0 0 0 25.031 0.00 1.41215 0.00000

16 0 0 0 0 0 27.611 0.00 1.44108 0.00030

17 0 0 0 0 0 29.390 0.00 1.46820 0.00000

T0TRL NUMBER 0F GALAXIES C0ÜNTED = 214 MAGNITUDE CUT0FF, MV 19.0 CLUSTER CENTER AT XO = 43.427 YO = -127.677

RING WIDTH (ARCMIN) = 2.0

Table 4.4.08. (a) Ring-Count Data for Galaxy Cluster 08. Isothermal Analysis 297 §4.4

GALAXY CLUSTER 008 01 39 50 -42 24 10' ISOTHERMAL FIT p(r) = oc-q(r/p) + 7

Q

ÜJ û _ c n

0Π10^

CORE RADIUS: Rc = 3)S~ 0.136 Mpc

10' 10° 10* 10’ RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.08. feJ Isothermal Fit for Galaxy Cluster 08. Isothermal Analysis 298 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 008 01 39 50 -42 24

pCr) - a q(r//S) + y

a - 666.59 ±401.44 /S - ].05±0.1B y- 11.61±3.20

p ( r ) = 1267. 54 - q C r / l . 04 ) + 12.20 B D T r i 7

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.136 Mpc Z = 0.050

Table 4.4.08. (b) Cluster Parameters for Galaxy Cluster 08.

Using the cluster center as determined by the dispersion ellipse analysis, we count 214 galaxies within 14 rings of width 2.0 arcminutes and to the limiting magnitude m„ = 19.0. This cluster appears to have more variance in the North- South ordinant than is seen in the East-West absissa. There are several obvious concentrations of peaks towards the Eastern portion of the cluster. The quadrant counts reveal an erratic scatter of galaxies throughout the cluster with an strong peak in ther first quadrant at ring 12. The cluster surface density distribution has a curious double peaked appearance with concentrations near the center of the cluster and periphery' as well.

The isothermal analysis trys to fit rather erratic data to the standard function; there are several depressions in the data, in particular at the cluster center. The fit tends to ride above these and the results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isothermal Analysis 299 §4 4 GALAXY CLUSTER 009 02 55 44 - 5 2 56

CLUSTER RING C0ÜNTS EAST M# N0RTH WEST =

2 0 M IN =

; J V |

S0 JTH A

CLUOTcrr 3T nir c b u n t o C A ST mmm NBRTH — NEST :

CLUSTER SURFACE DENSITY

35. § i 3 0 . S I 2 5 . g ! i rjV K k n r 0. II

= EAST I SftJTH « S T — Figure 4.4.09. {aJ Cluster Bing Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 300 §4.4

GALAXY CLUSTER 009 02 55 44 -5 2 56

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG IRAQI L0GIDEN1

JMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEGl

1 0 0 0 0 0 1.259 0.00 0.10001 0.00000

2 18 3 6 7 2 2.815 2169.01 0.44949 3.33626

3 22 8 3 8 3 4.539 1590.61 0.65698 3.20156

4 33 15 5 11 2 6.295 1704.22 0.79898 3.23153

5 33 8 11 7 7 8.D61 1325.51 0.90640 3.12238

6 36 8 13 7 8 9.833 1183.10 0.99267 3.07302

7 43 5 11 10 17 11.607 1195.74 1.06472 3.07764

8 38 8 4 18 8 13.383 915.80 1.12655 2.96180

9 20 2 7 7 4 15.160 425.30 1.18069 2.62869 10 33 7 8 15 3 16.937 627.87 1.22885 2.79787

11 25 8 5 2 10 18.716 430.36 1.27220 2.63383

12 16 5 2 6 3 20.494 251.48 1.31163 2.40050

13 25 5 5 4 11 22.273 361.50 1.34778 2.55811

14 14 1 13 0 0 24.052 187.45 1,38115 2.27287

15 0 0 0 0 0 25.831 0.00 1.41215 0.00000

16 0 0 0 0 0 27.611 0.00 1.44108 0.00000

17 0 0 0 0 0 29.390 0.00 1.46820 0.00000

TOTAL NUMBER OF GALAXIES COUNTED = 3SB MAGNITUDE CUTOFF. MV = 19.0

CLUSTER CENTER AT XO = -B7.306 YO = 109.669

RING WIDTH tORCMINI = 2.0

Table 4.4.09. faj Ring-Count Data for Galaxy Cluster 09. Isothermal Analysis 301 §4 4

GALAXY CLUSTER 009 02 55 44 -52 56

ISOTHERMAL FIT yo(r) = a-q(r//S) + y

QI

Or: c r ZD a (T)

X CE ΠO

CORE RADIUS; Rc = 3jS~ 0.132 Mpc

10' 10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.09. (e) Isothermal Fit for Galaxy Cluster 09. Isothermal Analysis 302 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 009 02 55 44 -52 56

p(r) - a q(r//S) + y

a - 1973. M±495. 13 /S - 1.02 ±0.01 7= 11.21±0.32

p(r) = 2699. 83-q(r/1. 03 ) + 11.68 '•E3T r n

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.132 Mpc Z = 0.049

Table 4.4.09. (h) Cluster Parameters for Galaxy Cluster 09.

Using the cluster center as determined by the dispersion ellipse analysis, we count 356 galaxies within 14 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. This rich cluster shows several peaks in the East-West strip count data that straddle the cluster center along the absissa; the North-South counts tend to reach their maximum near the cluster center as well, but with slightly more variance. The quadrant counts show a virtual absence of galaxies at the cluster center, but there is a quick rise in counts soon after with the counts then increasing in all directions. The surface density rises to a maximum at ring 7 and then slowly falls to the the cluster periphery.

The isothermal fit is seriously affected by the lack of data at small radii, but the fit tends to mimic the data fairly well beyond that point until the outer reaches of the cluster where the fit begins to overshoot the data. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isothermal Analysis 303 §4 4 GALAXY CLUSTER 010 03 44 05 -4 1 21

CLUSTER RING C0UNTS ; e r s t # * N0RTH WEST =

ss 20 MIN = II I

!

a

3

SBLITH I

CLUSTER STRIP C0ÜNT5

: EAST «■ N0RTH III t £ S T = CLUSTER SURFACE DENSITY : B I N S = =

4 5 .

2 5 . g

E 20 . 2 s É

II

= EAST W EST = Figure 4.4.10. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 304 §4.4

GALAXY CLUSTER 010 03 44 05 -41 21 5

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) LOCtOENI

NUMBER COUNT NW NE SE SW RADIUS DENSITY

lARCMIN) (GAL/SQOEG)

1 5 1 2 0 2 1.259 1807.51 0.10001 3.25708

2 19 1 5 7 6 2.815 2289.51 0.44949 3.35974

3 10 1 2 5 2 4.539 723.00 0.65698 2.85914

4 8 1 3 2 2 6.295 413.14 0.79898 2.61610

5 9 1 4 3 1 8.061 361.50 0.90640 2.55611

E 10 5 3 0 2 9.833 328.64 0.99267 2.51672

7 16 2 5 6 3 11.607 444.92 1.06472 2.64829

8 15 0 7 4 4 13.383 361.50 1.12655 2.55811

9 5 1 1 1 2 15.160 106.32 1.18069 2.02663

10 11 3 1 4 3 16.937 209.29 1.22885 2.32075

11 15 2 4 3 6 18.716 258.22 1.27220 2.41198

12 17 4 1 5 7 20.494 267.20 1.31163 2.42683

13 10 2 6 0 2 22.273 144.60 1.34778 2.16017

14 21 3 4 10 4 24.052 281.17 1.38115 2.44897

15 11 5 3 1 2 25.831 137.12 1.41215 2.13710

16 10 3 2 1 4 27.611 116.61 1.44106 2.05675

17 16 7 4 1 4 29.390 175.27 1.46820 2.24372

18 8 4 1 2 1 31.170 82.63 1.49374 1.91713

19 6 0 3 0 3 32.950 58.62 1.51785 1.76805

20 2 0 2 0 0 34.730 18.54 1.54070 1.26803

TOTAL NUMBER OF GALAXIES COUNTED = 224 MAGNITUDE CUTOFF, MV = 19.0 CLUSTER CENTER AT XO = 103.679 YO = -70.538

RING WIDTH (arcmin ; = 2.0

Table 4.4.10. {aJ Ring-Connt Data for Galaxy Ghister 10. Isotbermaî Analysis 305 §4.4

GALAXY CLUSTER 010 03 44 05 - 4 1 21

ISOTHERMAL FIT p(r) = a-q(r/^) + 7

acn

Û_ c n

CORE RADIUS:

Rc=3/S-0.134 Mpc

10 ' 10° RAOIAL DISTANCE (ARCMINUTES)

Figure 4.4.10. (e) Isothermal Fit for Galaxy Cluster 10. Isothermal Analysis 306 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 010 03 44 05 - 4 1 21

/oCr) - ot q(r/y5) + y

a ~ 757.01 ±503.96 /S - 1.05±0.18 y = n.56±3.49

p ( r ) = 1 4 8 1 . 8 3 - q C r / l .0 3 ) + 1 1 .9 0 « 3 T fIT

CORE RADIUS; REDSHIFT: Rc=3/S~ 0.134 *h-i Mpc Z = 0.050

Table 4.4.10. {bj Cluster Parameters for Galaxy Cluster 10.

Using the cluster center as determined by the dispersion ellipse analysis, we count 224 galaxies within 20 rings of width 2.0 arcminutes and to the limiting mag­ nitude mt, = 19.0. The cluster strip counts show a wide variance in this somewhat diffuse cluster. There appears to be a slight concentration of galaxies Eastward of cluster center along the absissa, whereas the North-South ordinate shows a concen­ tration very near cluster center. The quadrant counts show an erratic distribution of points in all directions, whereas the cluster surface density appears appears some­ what flat especially beyond ring 7.

The isothermal fit finds difficulty contouring itself along the quasi-plateau from the fourth to eighth rings. In addition, the density peak at the second ring is con­ siderably disproportionate and appears to be caused by the density concentration seen in the third quadrant. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isothermal Analysis 307 §4.4 GALAXY CLUSTER O il 04 04 04 - 3 9 00

CLUSTER RING C0UNTS ------— 1 IIMII------: EBST w N0RTH WEST = 11 — 2 0 M IN = : I s. :

E ... r-& .n.7Tn... I E i: s.I :

W EST = 1 ««ICUMMB 2 4 1 «iCUKlttlX

ci_u3Tcf\ oxnir c b u n t o E A S T a n N 0RTH mmm * E S T —

II CLUSTER SURFACE DENSITY I e=l B IN S =

35. § S i E I

II

o-^N(n«*iD(cr^CD9>0'~N(n«*Lnuc**cocTO = ERST S a jT H Figure 4.4.11. {aJ Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surjace Density. Isotbermaî Analysis 3 0 8 § 4 . 4

GALAXY CLUSTER O il 04 04 04 -3 9 00

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) LEGIDENI

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQOEG)

1 2 0 0 1 1 1.259 723.00 0.10001 2 .8 5 9 1 4

2 11 2 2 4 3 2 .8 1 5 1325.51 0.44949 3 .1 2 2 3 8

3 10 3 2 2 3 4.539 723.00 0.65698 2 .8 5 9 1 4

4 5 3 2 0 0 6 .2 9 5 258.22 0.79898 2 .4 1 1 9 8

5 7 3 2 1 1 8 .0 6 1 28 1 .1 7 0 .9 0 6 4 0 2 .4 4 8 9 7

6 13 0 6 5 2 9.833 427.23 0.99267 2 .6 3 0 5 8

7 7 1 2 2 2 11.607 194.65 1 .06472 2 .2 8 9 2 6

8 E 3 0 3 0 1 3.383 144.60 1.12655 2 .1 6 0 1 7

9 3 1 0 D 2 15.160 63.79 1.18069 1.80478

10 4 0 3 1 0 1 6.937 76.11 1.22885 1.88142

11 5 1 0 2 2 18.716 86.07 1.27220 1.93486

12 3 2 0 0 1 2 0 .4 9 4 4 7 .1 5 1.31163 1.67350

13 3 2 1 0 0 2 2 .2 7 3 4 3 .3 8 1 .3 4 7 7 8 1 .63729

14 4 0 0 1 3 24.052 53l56 1.38115 1.72881

15 11 5 1 2 3 25.831 137.12 1 .41215 2 .1 3 7 1 0

16 2 0 0 0 2 27.611 23.32 1.44108 1.38778

17 4 0 1 2 1 29.390 43.82 1.46820 1.64166

18 3 1 1 1 0 3 1 .1 7 0 3 0 .9 9 1 .4 9 3 7 4 1.49116

19 1 0 1 0 0 3 2 .9 5 0 9 .7 7 1 .51785 0.98991

20 3 0 3 0 0 34.730 27.81 1.54070 1.44417

T0TAL NUMBER OF GALAXIES COUNTED = 107 MAGNITUDE CUTOFF. MV = 1 9 .0

CLUSTER CENTER AT xo = - 1 0 1 .2 1 9 YO = 54 .3 7 5

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.11. (a) Ring-Count Data for Galaxy Cluster 11. Isotbermaî Analysis 309 §4.4

GALAXY CLUSTER O il 04 04 04 - 3 9 00 10' ISOTHERMAL FIT p(r) = a-q(r//S) + 7

a CO

Û_ CO

CORE RADIUS;

Rc=3jg- 0.113 Mpc

i o ‘ 10° 10* RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.11. ^ej Isothermal Fit for Galaxy Cluster 11. Isothermal Analysis 310 §4.4

CLUSTER PARAMETERS ______GALAXY CLUSTER O il 04 04 04 -39 00

p(r) - a q(r//3) + y

a - 454.53 ±261.26 /S - 1.04±0.17 y - 11.42±3.39

p(r) = 842. 85-q(r/l. 03 ) + 11.70

CORE RADIUS: REDSHIFT: R c= 3 /S ~ 0.113 Mpc Z = 0 .0 4 2

Table 4.4.11. (b) Cluster Parameters for Galaxy Cluster 11.

Using the cluster center as determined by the dispersion ellipse analysis, we count 107 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. This rather diffuse cluster shows a high near-central density distribution with a slight concentration of counts East of center as shown in the strip counts. The North-South distribution of galaxies is centrally concentrated but with a rather large variance. Likewise, the quadrant counts show somewhat larger numbers of galaxies near the cluster center and falling off slightly at larger radii. There is a peak at ring 6 in both the second and third quadrants. This also appears in the cluster surface density distribution as a dominant peak. Otherwise the distribution tails off to a slight increase at the cluster periphery.

The isothermal fit tends to fit the peaks in the data at the expense of the troughs and the results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isothermal Analysb 311 §4.4 GALAXY CLUSTER 012 05 24 GO - 4 5 01

CLUSTER RING C0UNTS : E R S T mmm NOiTH WEST =

== 20 MIN —

Î 3

: I I

8 3 u II

— E R S T ■> S0UTH — W EST =

CLuoTca OTnir cbunto EAST Ml HBRTH WEST =

II CLUSTER SURFACE DENSITY = 1 MM B IN S =

a s . §

I

II AWWLUS NUMBER 12 ARCMIN WIDTH)

0>^r4r>vi/itor>CD090»«

GALAXY CLUSTER 012 05 24 00 -4 5 01

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOGIRADI LBC(DEN)

JHBER COUNT NU NE SE sw RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

I 0 0 0 0 0 1 .2 5 9 0 .0 0 0.10001 0 .0 0 0 0 0

2 11 2 0 4 5 2 .8 1 5 1325.51 0.44949 3 .1 2 2 3 8

3 7 0 0 4 3 4.539 508.10 0.65698 2.70424

4 15 1 2 4 8 6.295 774.65 0.79898 2.88910

5 12 1 6 3 2 8.061 4 8 2 .0 0 0.90640 2.68305

6 12 4 1 G 1 9 .8 3 3 3 9 4 .3 7 0 .9 9 2 6 7 2 .5 9 5 9 0

7 4 2 0 2 0 11.607 111.23 1.06472 2.04623

8 7 3 2 2 0 13.383 168.70 1.12655 2 .2 2 7 1 2

9 9 1 0 2 G 15.160 191.38 1.18069 2 .2 8 1 9 0

10 10 0 2 7 1 16.937 190.26 1.22885 2 .2 7 9 3 6

11 7 0 3 2 2 18.716 120.50 1.27220 2 .0 8 0 9 9

12 7 3 1 1 2 20.494 110.02 1.31163 2 .0 4 1 4 8

13 5 4 2 0 0 22.273 86.76 1.34778 1.93832

14 4 2 2 0 0 24.052 53.56 1.38115 1.72881

15 4 0 4 0 0 25.831 49.86 1.41215 1 .69777

16 0 0 0 0 0 27.611 0.00 1.44108 0 .0 0 0 0 0

TOTAL NUMBER OF GALAXIES COUNTED = 115 MAGNITUDE CUTOFF. MV = 19.0

CLUSTER CENTER AT XD = 115.824 YD = -1 .2 7 1

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.12. (a) Ring-Count Data for Galaxy Cluster 12. Isotbermal Analysis 313 §4.4

GALAXY CLUSTER 012 05 24 GO - 4 5 01 10 ISOTHERMAL FIT pir) = aq(r//3) + 7

LD ÜJ O

Œ

Q_ c n

c r

CORE RADIUS;

Rc=3/3~ 0.164 *h ^ Mpc

10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.12. (e) Isothermal Fit for Galaxy Cluster 12. Isotbermal Analysis 314 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 012 05 24 00 -45 01

p (r) - a-q(r//S ) + y

a - 576.66 ±395.24 /S - 1.05±0.19 I1.37±3.76

p(r) = 1 15Q. 88-q(r/1. 03 ) + 11.34

CORE RADIUS: R ED SHIFT; Rc=3/S~ 0.164 Mpc Z = 0.061

Table 4.4.12. (b) Cluster Parameters for Galaxy Cluster IS.

Using the cluster center as determined by the dispersion ellipse analysis, we count 115 galaxies within 15 rings of width 2.0 arcminutes and to the limiting magnitude m-u = 19.0. This fairly sparce cluster shows a fairly wide scatter and variance in the determination of the cluster center. We find the quadrant counts to be virtually devoid of galaxies near the cluster center witha significant increase of counts at ring 4. Another minimum is seen W'est of center at ring 7. The surface density distribution is slightly bifurcated with peaks centered at rings 4 and 10. The largest number of counts appear in the North-East quadrant of ring 5.

The isothermal fit successfully models the core of the cluster but seriously overshoots the surface density data at radii greater than r = 10'^-* minutes of arc. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 315 §4 4 GALAXY CLUSTER 013 06 21 39 - 6 4 56

CLUSTER RING C0UNTS rw i EAST N0ATH u> NEST :

== 20 MIN =

S0inH mmm

CLUSTER STRIP C0ÜNT5 :z EBST •» N0RTH «u NEST —

II = J MM B IN S CLUSTER SURFACE DENSITY E SO. I I 1 I 1 » *7 ■ 1 I I I I I I n - i I I I 4 5 . -

4 0 . -

3 5 . I ■ I 3 0 . 1 - 2 5 . g - 2 0 . E P l b . i - 1 0 . ■ 5 . r 0 .

AIMJLUS NUMBER tZ ARCMIN WIDTH) ^ j,! [niiiHp. = = E R S T S 0 J T H mm# WEST =mmm Figure 4.4.13. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 316 §4 4

GALAXY CLUSTER 0 1 3 0 6 21 3 9 -6 4 5 6

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG (RAO) LOG(DEN)

NUMBER COUNT NW NE SE SU RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 2 0 0 2 0 1 .2 5 9 723.00 0.10001 2.85914

2 7 2 2 1 2 2 .8 1 5 843.50 0.44949 2.92509

3 £ 1 1 2 2 4 .5 3 9 4 3 3 .8 0 0.65698 2.63729

4 6 2 0 2 2 6 .2 9 5 3 0 9 .8 6 0.79898 2.49116

5 6 0 2 4 0 8 .0 6 1 241.00 0.90640 2.38202

6 11 4 2 2 3 9 .8 3 3 3 6 1 .5 0 0.99267 2.55811

7 8 2 2 3 1 11.607 222.46 1.06472 2.34726

8 13 5 1 3 4 13 .3 8 3 313.30 1.12655 2.4 9 5 9 6

9 3 2 0 0 1 1 5 .1 6 0 63.79 1.18069 1.80478

10 6 0 0 3 3 16 .9 3 7 114.16 1.22885 2.05751

11 5 1 0 2 2 18 .7 1 6 86.07 1.27220 1.93486

12 9 2 3 1 3 2 0 .4 9 4 141.46 1.31163 2 .1 5 0 6 3

13 13 2 6 5 0 2 2 .2 7 3 187.98 1.34778 2.27411

14 6 0 2 2 2 24.052 80.33 1.38115 1.90490

15 4 2 0 1 1 25.831 49.86 1.41215 1.69777

16 16 3 6 1 6 27 .6 1 1 186.58 1.44108 2 .2 7 0 8 7

17 7 3 0 1 3 29.390 76.68 1.46820 1.88469

18 7 3 1 1 2 31.170 72.30 1.49374 1.85914

19 6 2 2 2 0 32.950 58.62 1.51785 1.76805

20 1 0 0 0 1 3 4 .7 3 0 9 .2 7 1.54070 0,95705

TBTAL NUMBER OF GALAXIES COUNTED = 163 MAGNITUDE CUTOFF, MV = 19.0

CLUSTER CENTER AT xo = 8 3 .9 2 1 YO = 4 .0 1 6

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.18. (a) Ring-Count Data for Galaxy Cluster IS. Isothermal Analysis 317 §4.4

GALAXY CLUSTER 013 06 21 39 - 6 4 56

ISOTHERMAL FIT pCr) = a-q(r//S) + 7

a

O' Πa cn

û _ cn

CORE RADIUS: Rc=3)5~ 0.103 ^ Mpc

10 10° 10 ’ RADIAL DISTANCE (ARCMINUTES!

Figure 4.4.13. (e) Isothermal Fit for Galaxy Cluster IS. Isotbermal Analysis 318 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 013 06 21 39 -64 56

p(r) - a-q(r//S) + y

a - 389.27 ± 2 1 0 .97 /S ~ 1.05±G.17 -y - 1I.55±3.38

p(r) = 70G.75-qCr/1.03 ) + 12.19

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.103 Mpc Z = 0 .0 3 8

Table 4.4.13. ^bj Cluster Parameters for Galaxy Cluster IS.

Using the cluster center as determined by the dispersion ellipse analysis, we count 163 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude rriy = 19.0. This sparsely populated cluster shows wide variance in its center determination. The member galaxies are distributed somewhat uniformly East and West of center, while there appears to be more scatter in the North-South directions. The quadrant counts show low count levels as well as erratic peaks and valleys. The cluster surface density distribution similarly shows a pattern of rising and falling several times. We find the highest number of counts under the peak found at ring sixteen.

The resulting surface densities force the isothermal fit to contend with an erratic distribution giving a relatively poor fit at large radii. The mimimum at ring 15 appears to be a significant source of noise. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 319 54.4 GALAXY CLUSTER 014 06 25 02 - 5 3 39

CLUSTER RING C0ÜNTS TBBT w M R T H — W EST =

:

i s

:= ERST Sa/TH

CLUOTCn 3TK ir c b u n t o = ERST ■» WRTH mm« t£ST =

II CLUSTER SURFACE DENSITY S »=J MM BINS = I

S E E

E

!l

— ERST M MUTM W 3T = Figure 4.4.14. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 320 §4.4

GALAXY CLUSTER 014 06 25 02 -5 3 39

iING T0TAL QUADRANT C0UNTS COUNTING OBSERVED LOGIRAO) L0GIOENI

JMBER C0UNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQOEG)

1 7 1 2 2 2 1.259 2530.51 0.10001 3.40321

2 13 3 1 7 2 2.815 1566.51 0.44949 3.19493

3 13 2 5 4 2 4.539 939.90 0.65698 2.97308

4 17 3 8 2 4 6.295 877.93 0.79898 2.94346

5 22 6 4 7 5 8.061 883.67 0.90640 2.94629

6 21 5 6 4 6 9.833 690.14 0.99267 2.83894

7 17 4 3 5 5 11.607 472.73 1.06472 2.67462

8 27 6 6 4 11 13.383 650.70 1.12655 2.81338

9 23 6 8 2 7 15.160 489.09 1.18069 2.68939

10 24 4 8 7 5 16.937 456.63 1.22885 2.65957

11 17 3 5 5 0 18.716 292.64 1.27220 2.46534

12 20 7 6 3 4 20.494 314.35 1.31163 2.49741

13 7 4 1 2 0 22.273 101.22 1.34778 2.00527

14 4 0 1 2 1 24.052 53.56 1.38115 1.72881

15 0 0 D 0 D 25.831 0.00 1.41215 0.00000

16 0 D 0 0 D 27.611 0.00 1.44108 0.00000

17 0 0 D 0 0 29.390 0.00 1.46820 0.00000

TBTAL NUMBER 0F GALAXIES COUNTED = 232 MAGNITUDE CUT0FF. MV = 19.0

CLUSTER CENTER AT XD = 88.653 YO = 70.926

RING WIDTH (ARCMINl = 2.0

Table 4.4.14. (a) Ring-Count Data for Galazy Cluster I 4 . Isotbermal Analysis 321 §4.4

GALAXY CLUSTER 014 06 25 02 -53 39 10 ' ISOTHERMAL FIT p(.r) = a-q(r/^) + 7

Ql O '■— V OLU QiŒ C3 cn

LU Û-

ŒX CJŒ

CORE RADIUS; Rc=3jS~ 0.132 ^ Mpc

10' 10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.14. (e) Isothermal Fit for Galaxy Cluster 14- Isotbermal Analysis 322 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 014 06 25 02 - 5 3 39

pCr) - a-q(r//S) + y

a - 1211.57 ±460.22 /S - 1.04±Q.10 y - 11.77±1.79

p C r ) = 1 8 5 6 . 17-qCr/l . 03 ) + 1 2 .1 5 B O T F IT

CORE RADIUS: REDSHIFT; Rc=3/S~ 0.132 Mpc Z = 0 .0 4 9

Table 4.4.14. (b) Cluster Parameters for Galaxy Cluster 14-

Using the cluster center as determined by the dispersion ellipse analysis, we count 232 galaxies within 14 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. This compact cluster shows less scatter in the East-West absissa of the strip counts than does the North-South variance. The quadrant counts show a general increase of galaxy population with increasing radial distance. There appears to be a significant excess of counts in the fourth quadrant at ring 9. The cluster surface density increases slowly to about ring 8 after which there is a slow decline of population to the cluster periphery.

The isothermal fit overshoots the data at rings 4 and 5 but manages to conform to the data at radial distances slightly in excess of 13 arcminutes. Nevertheless, the fit seems to override the data and apparently could better mimic the obser\’’ations having been lowered somewhat. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isothermal Analysis 323 §4.4 GALAXY CLUSTER 015 06 26 25 - 5 4 22

ran CLUSTER RING COUNTS rw : E A S T mmu N0ATH ■■■ WEST =

2 0 M IN =

»» S0UTH ■■■ W EST z =

C t.U 3T C rC 3TfTir C0UNT3 EA ST warn NBRTH i£ST =

CLUSTER SURFACE DENSITY = 1 MM B I N S = =

3 5 . § I E i I II RNNULUS NUMBER 12 RRCMIN WIDTH]

= EA ST mm S0UTM ItST = Figure 4.4.15. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 324 §4.4

GALAXY CLUSTER 015 06 26 25 -54 22

RING TBTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) LOG(DEN)

JMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 5 1 1 1 2 1.259 1807.51 0.10001 3.25708

2 22 5 2 10 5 2 .8 1 5 2651.01 0.44949 3.42341

3 15 3 3 4 5 4 .5 3 9 1084.50 0 .6 5 6 9 8 3 .03523

4 18 4 3 5 6 6 .2 9 5 929.57 0.79898 2 .9 6 8 2 8

5 20 3 4 8 5 8.061 803.34 0.90640 2 .9 0 4 9 0

6 28 5 610 7 9.833 920.19 0 .9 9 2 6 7 2 .9 6 3 8 8

7 24 5 5 6 8 1 1 .6 0 7 6 5 7 .3 9 1.06472 2 .8 2 4 3 8

8 19 7 3 6 3 13.383 457.90 1.12655 2.6 6 0 7 7

9 9 4 0 4 1 15.160 191.38 1.18069 2.28190

10 21 11 1 3 6 1 6 .9 3 7 399.55 1.22885 2.60158

11 18 8 5 3 2 1 8 .7 1 6 3 0 9 .8 6 1.27220 2.49116

12 15 5 5 3 2 20.494 235.76 1.31163 2 .37247

13 17 4 7 4 2 22.273 245.82 1.34778 2 .3 9 0 6 2

14 4 0 13 0 24.052 53.56 1.38115 1.72881

15 0 000 0 25.831 0.00 1.41215 0.00000

16 0 0 0 0 0 27.611 0.00 1.44108 0.00000

17 0 0 0 0 0 29.390 0.00 1.46820 0 .00000

TBTAL NUMBER OF GALAXIES COUNTED = 235 MAGNITUDE CUTOFF, MV = 1 9 .0

CLUSTER CENTER AT XO = 7 6 .7 1 3 YO = 32.793

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.15. (a) Ring-Count Data for Galaxy Cluster 15. Isotbermal Analysis 325 §4 4

GALAXY CLUSTER 015 06 26 25 -54 22 10 ISOTHERMAL FIT yO(r) = a-q(r//S) + 7

CC C3 CO cm LU Û_ cn

CORE RADIUS:

Rc = 3/?~ 0.130 Mpc

10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.15. (e) Isothermal Fit for Galaxy Cluster 15. Isotbermal Analysis 326 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 015 06 26 25 -54 22

p(r) - a-q(r//S) + y

1342.45 ±382.24 /S - 1.02 ±0.01 y- 11.34±G.41

pCr) = 1933.29-q(r/l.03 ) + 11.98

CORE RADIUS: REDSHIFT: Rc=3/g~ 0.130 *h-i Mpc Z = 0 .0 4 8

Table 4.4.15. (b) Cluster Parameters for Galaxy Cluster 15.

Using the cluster center as determined by the dispersion ellipse analysis, we count 235 galaxies within 14 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. This rather compact cluster shows a slightly larger variance in the North-South ordinate than in the East-West absissa, but nevertheless, the cluster remains centrally condensed. The quadrant counts show a steady increase of counts at increasing radii, save for the void observed at ring 9 in the first and fourth quadrants. The cluster surface density displays a quick rise to a maximum at annulus 6 falling slowly with the exception of the above mentioned minimum.

The isothermal fit tends to envelope the surface density data with poor mod­ eling near the periphery of the cluster.

The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the x* minimization procedure. Isotbermal Analysis 327 §4.4 GALAXY CLUSTER 016 12 51 41 - 2 8 44

CLUSTER RING C0UNTS : EAST me# N0RTH mm. NEST :

== 20 MIN — I:

:

:

3 NW

= = E A S T p m * S 0U T H WEST =

CLuuTcn 3Tm r c b u n t o : EAST mi NBRTH tCST —

II CLUSTER SURFACE DENSITY E = 1 ftt BINS == I

r-TL I t É

= CAST ' S S U r n mmm NEST = Figure 4.4.16. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 328 544

GALAXY CLUSTER 016 12 51 41 -28 44

JING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) L0GIDEN)

JHBER COUNT NW NE SE SW RADIUS DENSITY

(RRCMIN) (GAL/SQDEG)

I 17 3 7 3 4 1.259 6145.52 0.1 0 0 0 1 3 .7 8 8 5 6

2 29 7 7 7 8 2 .8 1 5 3494.51 0.44949 3.54339

3 26 5 2 12 7 4.539 1879.81 0.65698 3.27411

4 26 2 9 11 4 6.295 1342.72 0.79898 3.12799

5 37 6 14 e 9 8.061 14 85.17 0 .9 0 6 4 0 3 .1 7 2 0 7

6 21 2 8 5 S 9.833 690.14 0.99257 2.83894

7 26 6 3 12 5 11 .6 0 7 7 2 3 .0 0 1.08472 2.85914

8 32 7 4 14 7 13.383 771.20 1 .1 2 6 5 5 2 .8 8 7 1 7

g 35 12 7 13 4 15.160 7 6 5 .5 3 1 .1 8 0 6 9 2 .88395

10 32 10 9 5 8 16.937 608.84 1 .2 2 8 8 5 2.78451

11 23 8 7 6 2 18.716 3 9 5 .9 3 1.27220 2.59752

12 21 7 3 4 7 2 0 .4 9 4 330.07 1.31163 2.51860

13 18 7 5 1 5 2 2 .2 7 3 2 6 0 .2 8 1.34778 2.41544

14 4 1 0 1 2 24.052 53.56 1.38115 1.72881

15 0 0 0 G 0 25.831 0.00 1.41215 0.00000

16 0 0 0 0 0 27.611 0 .0 0 1 .4 4 1 0 8 0 .00000

TBTAL NUMBER BF GALAXIES COUNTED = 348 MAGNITUDE CUTOFF. MV = 1 9 .0

CLUSTER CENTER AT XO = -1 4 6 .5 5 3 YO = 6 5 .3 4 8

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.16. (a) Ring-Count Data for Galaxy Cluster 16. Isotbermal Analysis 329 §4 4

GALAXY CLUSTER 016 12 51 41 -28 44 10' ISOTHERMAL FIT pir) = aq(r//S) + 7

ΠC3 cn

tn

CORE RADIUS: Rc = 3jS~ 0.129 th -i Mpc

1 0 ' 10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.16. (e) Isothermal Fit for Galaxy Cluster 16. Isotbermal Analysis 330 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 0 1 6 12 51 41 - 2 8 4 4

pCr) - a-q(r//S) + y

a - 3543 .86 ±275.51 /S = 1.03±0.00 7 11. 78± 0.14

iO (r ) = 3819.37 *q(r/l.03 ) + 11.92 ■E JT F IT

CORE RADIUS; REDSHIFT: Rc=3/S~ 0.129 *h-i Mpc Z = 0.048

Table 4.4.16. (b) Cluster Parameters for Galaxy Cluster 16.

Using the cluster center as determined by the dispersion ellipse analysis, we count 348 galaxies within 14 rings of width 2.0 arcminutes and to the limiting mag­ nitude m-u = 19.0. The cluster appears to have a somewhat linear constiution with a large number of galaxies aligned slightly Eastward of center along the absissa at the peak of the distribution. We find more scatter along the North-South ordinate and a wider distribution of galaxies. The quadrant counts are by no means sym­ metrical, and each quadrant possesses at least a single significant maximum. We find the cluster surface density to reflect the high central density of the cluster with significant peaks at rings 5 and 9.

The isothermal fit envelopes a quickly descending density distribution and is likely effected by the relatively high central density which is not quite twice as large as the value in the adjacent annulus. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 331 §4.4 GALAXY CLUSTER 017 13 03 25 - 3 7 18

CLUSTER RING COUNTS == EPST m u N0RTH *#« WEST =

20 MIN =

I II

== EftST i S0UTH I WEST —

CUUOTCn 3T m r CBUNTO : EAST — WRTH — ICST =

CLUSTER SURFACE DENSITY E I

S E

a 2 S .

i

Uhi B IW X U S NUMBER 12 URCHIN WIDTH]

: EAST wmt SRJTH — l£ST == Figure 4.4.17. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 332 §4.4

GALAXY CLUSTER 017 13 03 25 -37 18

UNO T0TAL QUADRANT COUNTS COUNTING OBSERVED LOG (RAD) LOG(DEN)

IMBER COUNT NW NE SE SW RADIUS DENSITY

(RRCMIN) (GAL/SQDEG)

1 7 2 0 1 4 1.259 253D.51 O.lDOOl 3.40321

2 15 1 8 3 3 2 .8 1 5 1807.51 0 .4 4 9 4 9 3.25708

3 8 1 2 2 3 4 .5 3 9 5 7 8 .4 0 0.65698 2.76223

4 20 1 4 7 8 6.295 1032.86 0.79898 3.01404

5 10 1 2 2 5 8 .061 401.67 0.90640 2.60387

6 17 4 4 3 6 9.833 558.68 0 .9 9 2 6 7 2.74717

7 23 3 7 7 6 11.607 63 3 .5 8 1 .0 6 4 7 2 2.80589

8 21 0 12 5 4 13.383 508.10 1 .1 2 6 5 5 2.70424

9 8 2 3 2 1 15.160 170.12 1 .1 8 0 6 9 2.23075

10 16 2 7 4 3 16.937 3 0 4 .4 2 1.22885 2.48348

11 9 2 5 1 1 18.716 154.93 1.27220 2.19013

12 17 7 5 3 2 20.494 267.20 1.31163 2.42683

13 7 2 2 0 3 22.273 101.22 1 .3 4 7 7 8 2.00527

14 2 0 0 0 2 24 .0 5 2 28.78 1.38115 1.42778

15 1 0 0 0 1 25.831 12.47 1.41215 1.09571

16 0 0 0 0 0 27.611 0 .0 0 1.44108 0.00000

TBTAL NUMBER 0F GALAXIES COUNTED = 181 MAGNITUDE CUT0FF, MV = 1 9 .0

CLUSTER CENTER AT XO = 9 5 .2 3 3 YO = -1 2 1 .7 2 8

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.17. (a) Ring-Count Data for Galaxy Cluster 17. Isothermal Analysis 333 §4 4

GALAXY CLUSTER 017 13 03 25 -37 18 10' ISOTHERMAL FIT pCr) = aq(r//S) + y

oa i o

CL. cn UJ

l .0 > CD

CORE RADIUS:

Rc = 3^~ 0.132 *h ^ Mpc

io‘ 10° 10' RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.17. (e) Isothermal Fit for Galaxy Cluster 17. Isotbermal Analysis 334 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 017 13 03 25 - 3 7 18

p(r) - a q(r//S) + y

a - 894.39 ±575.74 /S - 1.05±0.18 y - 11.63±3.54

p(r) = 1712.15 -q(r/1.03 ) + 11.92 K 3 T FIT

CORE RADIUS: REDSHIFT: Rc=3/8~ 0.132 Mpc Z = 0 .0 4 9

Table 4.4.17. (bj Cluster Parameters for Galaxy Cluster 17.

Using the cluster center as determined by the dispersion ellipse analysis, we count 181 galaxies within 15 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. We find the cluster strip counts to be somewhat skewed Eastward of center along the East-West absissa, but somewhat more symmetrical along the North-South ordinate but wüh larger variance. The quadrant counts show a relative avoidance of the first quadrant and a well-populated second quadrant with a significant maximum located at ring 8. The cluster surface surface density displays erratic behavior with peaks in the distribution located some twelve arcminutes from cluster center.

The isothermal fit is effected by the somewhat erratic distribution of surface densities and is able to form an envelope over the data fitting well at only a few points. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 335 §4.4 GALAXY CLUSTER 018 14 00 41 - 3 3 44

CLUSTER RING COUNTS : EBST WEST =

=% ERST W EST =

EPST c l u s t e r .STRIP.COUNTS „

CLUSTER SURFACE DENSITY

s

ANNULUS NUtBER 12 URCHIN WIDTH)

«= ERST

Figure 4.4.18. faj Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 336 §4.4

GALAXY CLUSTER 018 H 00 41 -33 44

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOGIRAD) LBGIDENl

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMIN) IGAL/SQDEG)

1 2 0 0 1 1 1.259 723.00 0.10001 2 .8 5 9 1 4

2 14 3 5 1 5 2 .8 1 5 1687.01 0.44949 3 .2 2 7 1 2

3 11 0 2 1 8 4 .5 3 9 7 9 5 .3 0 0.65698 2.90053

4 14 1 5 1 7 6.295 723.00 0.79898 2.85914

5 11 2 3 2 4 8.061 441.84 0.90640 2.64526

6 10 3 2 0 5 9 .8 3 3 3 2 8 .6 4 0 .9 9 2 6 7 2 .5 1 6 7 2

7 13 4 2 3 4 1 1 .6 0 7 361.50 1.06472 2.55811

8 7 5 1 0 1 13.383 168.70 1.12855 2 .2 2 7 1 2

9 3 0 2 0 1 15.160 63.79 1.18069 1.80478

10 13 1 1 5 6 16.937 247.34 1.22885 2.39330

11 9 2 0 2 5 18.716 154.93 1.27220 2.19013

12 15 3 4 5 3 20.494 235.76 1.31163 2.37247

13 8 1 2 4 1 22.273 115.68 1.34778 2.05326

14 7 3 1 1 2 24.052 93.72 1.38115 1.97184

15 21 4 3 2 12 25 .8 3 1 2 6 1 .7 8 1.41215 2 .4 1 7 9 3

16 9 2 2 2 3 27 .6 1 1 104.95 1.44108 2.02099

17 8 0 1 2 5 29.390 87.64 1.46820 1 .94269

18 7 1 1 3 2 3 1 .1 7 0 72.30 1.49374 1.85914

19 14 4 3 4 3 32.950 136.76 1.51785 2.13604

20 8 2 2 2 2 3 4 .7 3 0 7 4 .1 5 1.54070 1.87C14

TOTAL NUMBER OF GALAXIES COUNTED = 444 MAGNITUDE CUTOFF. MV = 19 0

CLUSTER CENTER AT XO = - 5 .2 2 3 YO = 6 9 .7 3 5

RING WIDTH (RRCMIN) = 2 .0

Table 4.4.18. (a) Ring-Count Data for Galaxy Cluster 18. Isothermal Analysis 337 §4.4

GALAXY CLUSTER 018 14 00 41 -33 44 10' ISOTHERMAL FIT p(r) = a-q(r/^) + 7

O oUJ LU g o CO Cd LU CL

CO

CORE RADIUS;

Rc=3jS~ 0.054 *h ^ Mpc

10‘ RADIAL DISTANCE (RRCM1NUTE51

Figure 4.4.18. (e) Isothermal Fit Jot Galaxy Cluster 18. Isothermal Analysis 338 §4.4

CLUSTER PARAMETERS ______GALAXY CLUSTER 018 14 00 41 -33 44

p(r) - oc q(r//S) + y

a - 570.20 ±342.73 /S - 1.05±0.17 y - 11.57±3.33

p(r) = 1067.88-q(r/1.03 ) + 12.01

CORE RADIUS; REDSHIFT: Rc=3/S~ 0.054 *h”‘ Mpc Z = 0 .0 2 0

Table 4.4.18. (b) Cluster Parameters for Galaxy Cluster 18.

Using the cluster center as determined by the dispersion ellipse analysis, we count 204 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. Although somewhat large in extent this cluster displays a slight central condensation; the East-West stripcounts have a wide variance as do the North-South counts which have a slightly higher population about the cluster center. The quadrant counts show no significant peaks until the cluster periphery is reached and the greater area encloses a larger number of objects. As a result, the cluster surface density is somewhat flat until at larger radii, the contribution made as a result of that increase in area grows.

The isothermal fit attempts to model the surface density and with exception made for the deep trough at ring 6 and the peak at ring 2, the fit is a fair repre­ sentation of the data. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isothermal Analysis 339 §4 4 GALAXY CLUSTER 019 14 09 18 - 3 2 50

CLUSTER RING C0UNT5 raw : ERST mmm N0RTH m»m WEST =

“ 2 0 M IN =

= - ERST S0UTH M B N E S T =

CLU3TCTT O Tm r C0UNTO

EAST m N0RTH Mt ICST —

CLUSTER SURFACE DENSITY B B IN S = 5 0 . 45.

4 0 .

3 5 , S ! 3 0 . I 2 5 . 2 0 . i n T l 1 5 .

10.

5 . 0 . I

= EAST m m # S0UTH ■■■ Figure 4.4.19. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotheimàl Analysis 340 §4 4

GALAXY CLUSTER 019 14 09 18 -32 50

RING T0TAL QUAORANT COUNTS COUNTING OBSERVED L0G(RAD) L06CDEN)

NUMBER C0UNT NW NE SE SW RADIUS DENSITY

(ARCHIN) (GAL/SQDEG)

1 1 0 0 0 1 1 .2 5 9 361.50 0.10001 2.55811

2 3 0 0 3 0 2.815 361.50 0.44949 2.55811

3 13 2 3 7 1 4 .5 3 9 939.90 0.65598 2.9 7 3 0 8

4 11 2 0 2 7 6 .2 9 5 5 6 8 .0 7 0.79898 2.75440

5 16 1 7 7 1 8 .0 6 1 6 4 2 .6 7 0.90640 2.8 0 7 9 9

6 15 2 7 1 5 9 .8 3 3 4 9 2 .9 6 0.99267 2.69281

7 17 2 9 4 2 11 .6 0 7 4 7 2 .7 3 1.06472 2.6 7 4 6 2

8 21 7 13 0 1 13 .3 8 3 506.10 1.12655 2.70424

9 16 1 4 5 6 15.160 3 4 0 .2 4 1.18069 2.53178

10 14 2 4 1 7 16.937 265.37 1.22885 2 .4 2 5 4 8

11 22 9 4 4 5 18.716 3 7 8 .7 2 1.27220 2.57831

12 8 5 1 0 2 20.494 125.74 1.31163 2 .0 9 9 4 7

13 9 2 4 1 2 2 2 .2 7 3 1 3 0 .1 4 1.34778 2.11441

14 19 6 5 2 4 2 4 .0 5 2 2 5 4 .3 9 1.38115 2.40550

15 15 2 7 2 4 25.831 186.98 1.41215 2 .27180

16 19 4 3 7 5 27.611 2 2 1 .5 7 1.44108 2.34550

17 11 1 1 3 6 2 9 .3 9 0 120.50 1.46820 2 .08099

18 7 0 2 1 4 31.170 72.30 1.49374 1.85914

19 1 0 0 0 1 3 2 .9 5 0 9.77 1.51785 0.93991

20 0 0 0 0 0 3 4 .7 3 0 0.00 1.54070 o.occoo

T0TAL NUMBER 0F GALAXIES C0UNTEO = 238 MAGNITUDE CUT0FF. MV = 1 9 .0

CLUSTER CENTER AT XO = -1 0 2 .1 4 8 YO = 117.241

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.19. faj Ring-Gount Data for Galaxy Chster 19. Isothermal Analysis 341 §4.4

GALAXY CLUSTER 019 14 09 18 -32 50

ISOTHERMAL FIT p(r) = a-q(r//S) + y

O

C3 cn

cn

X c r Œo 10'

CORE RADIUS; Rc=3/S~ 0.119 *h ^ Mpc

10° 10' RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.10. /^ej Isothermal Fit for Galaxy Cluster 19. Isothermal Analysis 342 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 0 1 9 14 0 9 18 - 3 2 50

p(r) - a-q(r//S) + y

a - 418.95 ±213.09 /? - 1.05±0.15 y - 12.0D±3.02

p(r) = 549.30*q(r/l,03 ) + 12.17 #C 5T F IT

CORE RADIUS; REDSHIFT: Rc=3/S~ 0.119 Mpc Z =0.044

Table 4.4.19. (b) Cluster Parameters Jar Galaxy Cluster 19.

Using the cluster center as determined by the dispersion ellipse analysis, we count 238 galaxies within 19 rings of width 2.0 arcminutes and to the limiting magnitude m-v = 19.0. We fine a fairly wide variance in the East-West strip count data with a slight density enhancement of counts Eastward of cluster center. Similar behavior is noted Southward of center alond the North-South ordinate. Quadrant counts show an avoidance for the center of the cluster and a large peak at the eighth ring of the second quadrant primarily due to subclustering. The surface density has a mildly bifurcated appearance with a trough near ring 12.

As a result of the low central density the isothermal fit is biased low and undershoots most of the data; models excluding data in the first two rings appear to have a better fit than using the full range of the data. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 343 §4.4 GALAXY CLUSTER 020 14 09 28 - 3 4 01

CLUSTER RING COUNTS “ EAST MB N0ATH *— WEST = . — 20 MIN =

: » E

i X I:

= = E R S T

CLUDTcn O Tm r cbunto : ERST mmm WRTH mm. WEST =

CLUSTER SURFACE DENSITY II = 1 MM BINS = 50. 45. 40. as. S 30. I 25. i 2 0 . 15. 10. 5. 0. AmULUS NIMER (2 ARCMIN WIDTH) O**ra>O)O'*C4(n.*i/)(fir'm cn o = EA ST Figure 4.4.20. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 344 §4 4

GALAXY CLUSTER 020 14 09 28 -34 01

RING T0TAL QUADRANT C0UNTS COUNTING OBSERVED LOG(RAO) L0G1DEH)

NUMBER C0UNT NW NE SE SW RADIUS DENSITY

(RRCMIN) (GAL/SQDEG)

I 1 0 0 1 0 1 .2 5 9 3 6 1 .5 0 0.10001 2 .55811

2 10 3 1 3 3 2 .8 1 5 1205.00 0.44949 3.08099

3 16 4 3 5 4 4 .5 3 9 1156.80 0.65698 3.06326

4 7 1 2 3 1 6 .2 9 5 361.50 0.79898 2.55811

5 9 4 0 4 1 8.061 3 6 1 .5 0 0.90640 2.55811

6 9 2 2 3 2 9 .8 3 3 2 9 5 .7 7 0.9 9 2 6 7 2 .4 7 0 9 6

7 16 0 6 B 2 11.607 444.92 1.06472 2.64829

e 15 2 4 7 2 13 .3 8 3 361.50 1.12655 2.55811

g 15 4 5 1 5 15 .1 6 0 318.97 1.18069 2.50375

10 16 7 3 2 4 16 .9 3 7 3 0 4 .4 2 1.22885 2.48348

11 17 2 4 6 5 1 8 .7 1 6 29 2 .6 4 1.27220 2.46634

12 14 3 6 0 5 2 0 .4 9 4 22 0 .0 4 1.31163 2.34251

13 16 3 5 2 6 2 2 .2 7 3 2 3 1 .3 6 1.34778 2.36429

14 10 I 4 3 2 2 4 .0 5 2 133.89 1.38115 2. 12675

15 13 4 5 3 1 2 5 .8 3 1 162.05 1.41215 2.20966

16 13 4 5 2 2 27.611 151.60 1.44108 2.18069

17 11 4 2 0 5 29.390 12 0 .5 0 1.46820 2.08099

18 9 D 1 4 4 3 1 .1 7 0 9 2 .9 6 1.49374 1.96828

19 2 0 0 1 1 32.950 19.54 1.51785 1.29094

20 0 0 0 D 0 3 4 .7 3 0 0 .0 0 1.54070 0 .0 0 0 0 0

T0THL NUMBER 0F GALAXIES C0UNTEO = 219 MAGNITUDE CUT0FF. MV = 1 9 .0

CLUSTER CENTER AT XO = -102.819 YO = 53.059

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.20. (a) Ring-Count Data for Galaxy Cluster SO. Isotbermal Analysis 345 §4.4

GALAXY CLUSTER 020 14 09 28 -34 01

ISOTHERMAL FIT p(r) = a-q(r//3) + 7

LÜ UJ OD1 oUJ UJÛi Œ ID (CO d LÜ û_

ŒX LDŒ

CORE RADIUS:

Rc=3/S~ 0.102 Mpc

10 10° 10 * RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.20. fej Isothermal Fit for Galaxy Cluster SO. Isotbermal Analysis 346 §4.4

CLUSTER PARAMETERS ______GAIAXY CLUSTER 020 14 09 28 -34 01

/j(r) - cx q(r//S) + y

a- 637. 12 ±442.73 /S - 1.05±O. 19 y - 11.50±3.75

p(r) = 1257.33-q(r/1.03 ) + 11.60

CORE RADIUS; REDSHIFT: Rc=3/S~ 0.102 *h-i Mpc Z = 0 .0 3 8

Table 4.4.20. (b) Cluster Parameters for Galaxy Cluster 20.

Using the cluster center as determined by the dispersion ellipse analysis, we count 219 galaxies within 19 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. This somewhat centrally condensed cluster shows a wide variance along the East-West absissa with a slight enhancement East of center; likewise the North-South distibution has wide variance and an excess North of center. The quadrant counts are erratic with an avoidance of the derived cluster center and an overall excess at large radii in the second quadrant. The cluster surface density distribution id for the most part flat with the exception of the dip seen near the fourth ring.

The low central density appears to effect the isothermal fit somewhat but with the exception of the trough seen near r = 8.1 arcminutes, the fit seems to reproduce the general trend of the data. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 347 §4.4 GALAXY CLUSTER 021 14 30 26 -31 32

CLUSTER RING COUNTS ram : E R S T wmm HBRJH mmm N E S T = =

s= 20 M IN z =

y v 12 i« It ta X

= = E A S T 50UTH WEST —

CLUUTCrX O T R ir C0UNTD ERST mm# N0RTM >C5T

I) CLUSTER SURFACE DENSITY =1 B IN S = =

5 * I 2 S . É E CC É

RNNULÜS N im ER 12 ARCMIN WIDTH)

mm SBUTH m#m WEST Figure 4.4.21. faj Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 348 §4.4

GALAXY CLUSTER 021 14 30 26 -31 32

RING T0TRL QUADRANT C0UNTS COUNTING OBSERVED LOGIRAD) L0GIDEN)

NUMBER C0UNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 4 1 1 2 0 1.259 1446.01 0.10001 3.16017

2 10 1 4 2 3 2 .8 1 5 1205.00 0.44949 3.08099

3 13 1 3 7 2 4.539 939.90 0.65698 2.97303

4 15 5 1 6 3 6 .2 9 S 774.65 0.79898 2.88910

5 11 3 3 4 1 8.061 441.84 0.90640 2.64526

6 6 3 2 1 0 9 .8 3 3 197.18 0.99267 2.29487

7 11 7 2 1 1 11.607 3 0 5 .8 9 1 .06472 2.48556

8 13 5 5 2 1 13.383 313.30 1.12655 2.49596

g 12 1 1 7 3 15.160 255.18 1.18069 2.40684

10 14 3 4 6 1 16.937 266.37 1.22885 2.42548

11 16 5 7 3 1 18.716 275.43 1.27220 2.44001

12 11 3 1 4 3 20.494 172.89 1.31163 2.23778

13 9 5 0 3 1 22.273 130.14 1.34778 2.11441

14 3 0 0 0 3 2 4 .0 5 2 4 0 .1 7 1 .3 8 1 1 5 1.60387

15 2 0 0 0 2 25.831 24.93 1.4121S 1.39574

16 0 0 0 0 0 27.611 O.OD 1 .4 4 1 0 8 0.00000

T0TRL NUMBER 0F GALAXIES COUNTED = 150 MAGNITUDE CUTOFF. MV = 1 9 .0

CLUSTER CENTER AT XO = 43.965 YD = -81.811

RING WIDTH lARCMIN) = 2.0

Table 4.4.21. faJ Ring-Count Data for Galaxy Cluster SI. Isotbermal Analysis 349 §4.4

GALAXY CLUSTER 021 14 30 26 -31 33

ISOTHERMAL FIT pir) = a-q(r//S) + 7

O ct: cr a CO

c n UJ

CC Π10^ L3

CORE RADIUS:

Rc=3/?~ 0.146 *h ^ Mpc

RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.21. (e) Isothermal Fit for Galaxy Cluster 21. Isotbermal Analysis 350 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 021 14 30 26 -31 33

p(r) - ot q(r//S) + y

a- 634. 30 ±397. 18 /S - 1.05±0.17 7 = 11.54±3.38

p(r) = 1221.45-q(r/l .03 ) + 11.94

CORE RADIUS: REDSHIFT; Rc=3/S~ 0.146 Mpc Z = 0 .0 5 4

Table 4.4.21. (b) Cluster Parameters for Galaxy Cluster SI.

Using the cluster center as determined by the dispersion ellipse analysis, we count 150 galaxies within 15 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. From the cluster strip counts we notice a significant peak East of the cluster center along the East-West absissa suggesting a strong linear component of concentration near the cluster center. The effect is corroborated by a Southward enhancement along the North-South ordinant. Quadrant counts reveal several minima especially near ring 6 and two relatively large peaks in the third quadrant at rings 2 and 9. The cluster surface density reflects this behavior being somewhat flat with a minimum at ring 6.

The isothermal fit agrees rather well with the data save for the minimum men­ tioned above seen at a distance of some ten arcminutes from cluster center. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 351 §4.4 GALAXY CLUSTER 022 19 56 35 - 3 8 32

CLUSTER RING C0UNTS = E A S T N E S T ===

II I 2

5I II

W EST —— E R S T W EST ——

:LU5TER,^%^P,C0UNTS fST W BINS = CLUSTER SURFACE DENSITY

5 0 .

4 5 .

3 0 . S 25. B 2 0 . “

1 5 . I 10.

ANNULUS NUMBER 12 ARCMIN WIDTH I

SBUTH Figure 4.4.22. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Fensity. Isotbermal Analysis 352 §4.4

GALAXY CLUSTER 022 19 56 35 -3 8 32

RING T0TRL QUADRANT COUNTS COUNTING OBSERVED LOGIRAD) LOG I DEN)

NUMBER C0UNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 1 1 0 0 0 1 .259 361.50 0.10001 2.55811

2 6 0 0 4 2 2,815 723.00 0.44949 2.85914

3 7 1 1 4 1 4.539 506.10 0.65698 2.70424

4 6 2 0 2 2 8.295 309.86 0.79898 2.49116

5 3 1 0 1 1 8.061 120.50 0.90640 2 .0 8 0 9 9

6 10 1 2 4 3 9 .8 3 3 3 2 8 .6 4 0.99267 2 .5 1 6 7 2

7 14 3 2 8 1 11.607 3 8 9 .3 1 1.06472 2.59029

6 14 3 0 6 5 13.383 3 3 7 .4 0 1.12655 2.52815

9 9 3 1 4 1 15.160 191.38 1.18069 2.28190

10 5 1 2 2 0 16.937 95.13 1.22885 1.97833

11 17 6 3 6 2 18.716 292.64 1.27220 2 .4 6 6 3 4

12 13 6 3 3 1 2 0 .4 9 4 204.33 1.31163 2 .3 1 0 3 3

13 11 7 2 1 1 2 2 .2 7 3 1 5 9 .0 6 1.34778 2.20156

14 20 7 3 6 4 2 4 .0 5 2 2 6 7 .7 8 1.38115 2.42778

15 15 6 2 5 2 25.831 186.98 1.41215 2.27180

16 11 5 1 2 3 27.611 1 2 8 .2 7 1.44108 2.10814

17 8 0 5 0 3 29.390 87.64 1.46820 1.94269

18 10 5 0 3 2 31 .1 7 0 103.29 1.49374 2 .01404

19 18 5 7 3 3 32 .9 5 0 17 5 .8 7 1.51785 2 .2 4 5 1 8

20 23 7 8 4 4 3 4 .7 3 0 2 1 3 .1 9 1.54070 2.32377

T0TPL NUMBER 0F GALAXIES COUNTED = 458 MAGNITUDE CUT0FF, MV = 1 9 .0

CLUSTER CENTER AT XO = -3 .5 8 1 YO = 80.348

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.22. faJ Ring-Count Data for Galaxy Cluster 22. Isotbermal Analysis 353 §4.4

GALAXY CLUSTER 022 19 56 35 - 3 8 33 10' ISOTHERMAL FIT p(r) = a-q(r//S) + y

y 10' o OLU orLU ex

ÛT LU Û_

CORE RADIUS: Rc=3jS~ 0.071 Mpc

io‘ 10° 10 * RADIAL DISTANCE (ARCMINUTES!

Figure 4.4.22. fe) Isothermal Fit for Galaxy Cluster 22. Isotbermal Analysis 354 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 022 19 56 35 -38 33

p(r) - a-q(r//9) + y

a ~ 356.22 ±177.24 /S - 1.05±0.16 y- 12.0I±3.21

p ( r ) = , 6 1 8 . 6 1 -q C r /l. 04 ) + 1 3 . GO

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.071 Mpc Z = 0 .0 2 6

Table 4.4.22. (b) Cluster Parameters for Galaxy Cluster 22.

Using the cluster center as determined by the dispersion ellipse analysis, we count 221 galaxies within 20 rings of width 2.0 arcminutes and to the limiting mag­ nitude my = 19.0. The stripcounts for this cluster burst out of range because of the large counting radius and increased number of galaxies counted in both orthogonal directions. The quadrant counts are erratic and display several significant peaks. More importantly, the cluster surface density appears to show a general trend of increasing surface density with increasing radial distance.

With the exception of troughs in the data, in particular, those seen at radial distances of r = 8.1 and r = 16.9 arcminutes, the isothermal fit approximates the data. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 355 §4.4 GALAXY CLUSTER 023 20 38 34 - 3 5 24

CLUSTER RING C0UNT5 TTH' : ERST N0RTH ■■■ NEST = == 20 MIN =

;

& 1

== ERST S 8U T H W EST =

= E B S T l £ S T =

II CLUSTER SURFACE DENSITY

5 5 0 . — 1 MM B IN S == f 4 5 .

4 0 .

3 5 . S a 3 0 . I 2 5 . Î 2 0 . s 1 5 .

10.

5 . 0 . II flNNaUS NUMBER 12 ARCMIN WIDTH)

= ERST S iU T H I lesT = Figure 4.4.23. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 356 §4.4

GALAXY CLUSTER 023 20 38 34 -3 5 24

(INC TOTAL OUAORANl■ COUNTS COUNTING «SERVED LOG(RAD) LOG(DEN)

JMBER COUNT NW NE SE SW RADIUS DENSITY

(RRCMIN) (GAL/SQDEG)

1 2 1 1 0 0 1.259 723.00 0.10001 2.85914

2 19 4 6 8 1 2.815 2289.51 0.44949 3.35974

3 29 5 12 G 8 4.539 2096.71 0.65698 3.32154

4 39 8 12 11 8 6.295 2014.08 0.79898 3.30408

5 41 7 10 13 11 8.061 1646.84 0.90640 3.21655

6 45 18 8 910 9.8:3 1478.87 0.99267 3.16993

7 45 11 11 12 11 11.607 1251.35 1.06472 3.03738

8 43 9 13 8 13 13.383 1036.30 1.12655 3.01549

9 53 18 13 11 11 15.160 1127.03 1.18069 3.05194

10 16 3 6 2 5 16.937 304.42 1.22885 2.48348

11 2 0 0 0 2 18.716 34.43 1.27220 1.53692

12 0 0 0 0 0 20.494 0.00 1.31163 0.00000

13 0 0 0 0 0 22.273 0.00 1.34778 0.00000

TOTAL NUMBER OF GALAXIES COUNTED = 334 MAGNITUDE CUTOFF, MV z 19.0

CLUSTER CENTER AT XO = 105.191 YO = -22.456

RING WIDTH (ARCMIN) z 2.0

Table 4.4.23. (a) Ring-Count Data for Galaxy Cluster 2S. Isotbermal Analysis 357 §4.4

GALAXY CLUSTER 023 20 38 34 - 3 5 24

ISOTHERMAL FIT p(r) = aq(r//5) + 7

cn CD O

o CO

Û_ cn

CC Π1 0 ' CD

CORE RADIUS: Rc=3/S~ 0.178 Mpc

RADIAL DISTANCE (ARCMINUTES!

Figure 4.4.23. feJ Isothermal Fit for Galaxy Cluster 2S. Isotbermal Analysis 358 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 023 20 38 34 -35 24

p(r) - a q(r//S) + y

a - 1808. 25 ±243. 74 /S - 1 .0 4 ± 0 .0 1 y -= 11.95±0.28

p ( r ) = 2160.93-qCr/l.05 ) + 1 2 . 3 5 rn

CORE RADIUS: REDSHIFT; Rc=3/S~ 0.178 Mpc Z = 0.065

Table 4.4.23. (b) Cluster Parameters for Galazy Cluster S3.

Using the cluster center as determined by the dispersion ellipse analysis, we count 334 galaxies within 11 rings of width 2.0 arcminutes and to the limiting magnitude rrii, = 19.0. This dense cluster displays a curious bifurcation of the data about the cluster center as determined by the dispersion ellipse analysis. The feature is seen both in the East-West and North-South data and is confirmed in the quadrant counts which show a strong avoidance for the cluster center in virtually all quadrants. The quadrant counts also show a tendency for counts to increase radially with distance with peaks in the first quadrant distribution found at rings 6 and 9. The cluster surface density also increases at a decreasing rate with increasing radial distance.

The low central density is seen to effect the isothermal fit, however the data appears to be modeled better at larger radii. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotberm al Analysis 359 §4.4 GALAXY CLUSTER 024 20 48 41 - 5 2 08

CLUSTER RING C0ÜN7S = = E R S T mmm N0RTH mi WEST =

II == 20 MIN =

/vfil E M a I i

II

= ' ERST WEST —

CLuoTcrr 3Tm r c b u n t d

== ERST ■ n N0RTH « I W EST — CLUSTER SURFACE DENSITY II B IN S — 5 0 . I 45. 40. 35. s I 30. 25. g i 2 0. 15. 10.

5 .

0 .

II flWULUS NUMBER 12 RRCMIN WIDTH)

= : EBST I SOUTH H I WEST = Figure 4.4.24. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. s 5

Isothermal Analysis 360 §4 4

GALAXY CLUSTER 024 20 48 41 -52 OS

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOGIRAD) LOG(DEN)

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMIN! (GAL/SQDEG)

1 4 0 0 3 1 1.259 1446.01 0.10001 3.16017

2 8 2 0 8 0 2.815 954.00 0.44949 2.98408

3 7 1 4 2 0 4.539 506.10 0.65698 2.70424

4 11 3 1 4 3 6.295 568.07 0.79898 2.75440

5 11 3 5 1 2 8.061 441.84 0.90640 2.64526

G 7 1 0 5 1 9.833 230.05 0.99257 2.35182

7 13 5 3 4 1 11.607 361.50 1.08472 2.55811

8 9 3 2 3 1 13.383 216.90 1.12655 2.33626

9 15 4 2 4 5 15.160 318.97 1.18069 2.50375

10 9 3 3 2 1 16.937 171.24 1.22885 2.23360

11 6 1 4 1 0 18.716 103.29 1.27220 2.01404

12 15 3 5 2 5 20.494 235.76 1.31153 2.37247

13 12 1 0 6 5 22.273 173.52 1.34778 2.23935

14 15 3 4 3 5 24.052 200.83 1.38115 2.30284

15 8 2 0 3 3 2S.83i 99.72 1.41215 1.99880

16 14 1 4 6 3 27.611 163.26 1.44108 2.21288

17 12 4 5 1 2 29.390 131.45 1.46820 2.11678

18 2 1 0 0 1 31.170 20.66 1.49374 1.31507

19 1 1 0 0 0 32.950 9.77 1.51785 0.98991

20 0 0 0 0 0 34.730 0.00 1.54070 0.00000

TOTAL NUMBER OF GALAXIES COUNTED = 179 MAGNITUDE CUTOFF. HV = 19.0

CLUSTER CENTER AT XO = 95.831 YO = -115.415

RING WIDTH (ARCMIN) = 2.0

T able 4.4.24. (a) Ring-Count Data for Galaxy Cluster S4- Isothermal Analysis 361 §4.4

GALAXY CLUSTER 0 2 4 20 48 41 - 5 2 08

ISOTHERMAL FIT p(r) = a-q(r//3) + y

O CD g cn

c r CD

CORE RADIUS; Rc = 3jS~ 0.100 Mpc

10° RADIAL DISTANCE (ARCHINDIES)

Figure 4.4.24. (e) Isothermal Fit for Galaxy Cluster 24- Isothermal Analysis 362 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 024 20 46 41 -52 08

p(r) - a q(r//S) + y

a - . 9 6 ± 3 4 0 . 4 3 /S - 1.05±0.17 11.68±3.43

p(r) = 1053.68-q(r/l.03 ) + 12.20

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.100 Mpc Z - - 0.037

Table 4.4.24. (b) Cluster Parameters for Galaxy Cluster 2\.

Using the cluster center as determined by the dispersion ellipse analysis, we count 179 galaxies within 19 rings of width 2.0 arcminutes and to the limiting magnitude m-u — 19.0. We note a wide variance in both the east-West and North- South strip count data with slight concentrations Eastward of center along the absissa and Northward along the ordinant. Several peaks are noticed in the quadrant counts, in particular the first quadrant maximum near ring 7. The cluster surface density shows several peaks and troughs but no really significant deviations.

The isothermal fit to the data achieves some success, but appears somewhat high in the sense of enveloping the data peaks, perhaps being influenced by the apparently high central density as well as the wild variations seen at relatively large radial distances ftom the cluster center. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 363 §4.4 GALAXY CLUSTER 025 21 13 10 - 5 9 36

CLUSTER RING COUNTS : E R S T MMM N0RTH — WEST '

2 0 M IN = I

E I E

II

= = E R S T W EST = z

CLUSTER STRIP COUNTS ■ ERST ■■■ N0RTM ■■■ Æ5T

CLUSTER SURFACE DENSITY B IN S =

S

2 S . B E

K RNMJLUS NIMBER 12 ARCMIN WIDTH)

= ERST Figure 4.4.25. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 364 §4.4

GALAXY CLUSTER 025 21 13 10 -5 9 SB

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAO) LOG(DEN)

NUMBER COUNT NW NE SE SU RADIUS DENSITY lARCHIN) IGAL/SQDEGl

I 1 0 1 0 0 1.259 361.50 0.10001 2.55811

2 9 2 G 1 0 2.815 1084.50 0.44949 3.03523

3 IS 4 3 7 1 4.539 1084.50 0.65698 3.03523

4 14 1 4 5 4 6.295 723.00 0.79898 2.85914

5 13 1 4 5 3 8.081 522.17 0.90640 2.71781

6 11 1 2 2 G 9.833 361.50 0.99267 2.55811

7 22 4 5 6 7 11.607 611.77 1.06472 2.78659

8 22 5 G 5 6 13.383 530.20 1.12655 2.72444

9 13 2 2 7 2 15.160 276.44 1.18069 2.44160

10 18 2 3 10 3 16.937 342.48 1.22885 2.53453

11 12 5 3 2 2 18.716 206.57 1.27220 2.31507

12 12 G 1 3 2 20.494 188.61 1.31163 2.27556

13 19 1 10 3 5 22.273 274.74 1.34778 2.43892

14 21 5 G 5 5 24.052 281.17 1.38115 2.44897

15 12 4 2 G 0 25.831 149.59 1.41215 2.17489

16 15 8 3 2 2 27.611 174.92 1.44108 2.24284

17 21 4 4 4 9 29.390 230.05 1.46820 2.36182

18 11 2 1 4 4 31.170 113.61 1.49374 2.05543

19 8 6 2 0 0 32.950 78.16 1.51785 1.89300

20 2 2 0 0 0 34.730 18.54 1.54070 1.26808

T0TRL NUMBER OF GALAXIES COUNTED = 271 MAGNITUDE CUTOFF, MV = 19.0 CLUSTER CENTER AT XO = 131.705 YO = 18.574

RING WIDTH CARCMIN) = 2.0

Table 4.4.25. (a) Ring-Gount Data for Galaxy Gluster 25. Isotbermal Analysis 365 §4.4

GALAXY CLUSTER 0 2 5 21 13 10 - 5 9 36 1 0 ^ ------1— I— I— I— 1 I I 11------1— I— I— I— I I I 11 ISOTHERMAL FIT p(r) = a-q(r//S) + 7

1 0 ^ CD

c r 0=3 0 1 ÛT LlJ CL

1 ,0 ' CD

CORE RADIUS: Rc=3jS~ 0.115 Mpc

I I I I I iJil I > > > I 1 I » 1 I I I 1 I ! 10 ' 10 " 10° 10* 10“" RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.25. fej Isothermal Fit for Galaxy Cluster 25. Isotbermal Analysis 366 §4.4

CLUSTER PARAMETERS ______GALAXY CLUSTER 025 21 13 10 -59 36

pCr) - a q(r// 8 ) + y

a - 525.08 ±293.09 /S - 1.05±0.15 y - 11.80±3.I2

p(r) = 964. 43-qCr/l. 04 ) + 12.63

CORE RADIUS: REDSHIFT: Rc=3/S~ 0 .1 1 5 M pc Z = 0 .0 4 2

Table 4.4.25. (b) Cltister Parameters for Galaxy Cluster 25.

Using the cluster center as determined by the dispersion ellipse analysis, we count 271 galaxies within 20 rings of width 2.0 arcminutes and to the limiting mag­ nitude = 19.0. The cluster strip counts show a rather symmetric spread about the cluster center along the East-West absissa and a slight Northward increase along the North-South ordinate. We find several peaks amongst the quadrant counts, the largest occuring in the third quadrant near ring 10. We notice a general avoidance of the cluster center. This efifect is also seen in the cluster surface density distri­ bution which otherwise shows several major peaks and troughs above some mean value.

The isothermal fit is no doubt influenced by the paucity of data near the clus­ ter center, but the rest of the observed data appears to be well discribed by the isothermal model. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 367 §4.4 GALAXY CLUSTER 026 21 22 58 ■35 00

CLUSTER RING C0UNTS — ERST —* N0RTH Ma WEST =

: 2 0 M IN =

n/,

J . '

r == ERST WEST

CLuoTcn OTnir cbunto — EAST » MBRTH «■ «ST :

CLUSTER SURFACE DENSITY = 1 MM B I N S 5 0 .

4 5 . 40.

3 5 .

3 0 .

2 5 . 2 0 .

1 5 . 10.

5 . 0 .

ftfWXUS NWeER 12 RRCMIN WIDTH)

= EAST ua SflUTH MI WEST — Figure 4.4.26. {aj Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 368 §4.4

GALAXY CLUSTER 026 21 22 58 -3 5 00

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOGIRAD) LOGIDEN)

JMBER COUNT NW NE SE sw RADIUS DENSITY

(RRCMIN) (GAL/SODEG)

1 1 0 0 1 0 1.259 361.50 0.10001 2.55811

2 13 2 3 4 4 2.815 1566.51 0.44949 3.19493

3 26 12 6 4 4 4.539 1879.81 0.65698 3.27411

4 20 12 1 5 2 6.295 1032.86 0.79898 3.01404

5 30 8 10 8 4 8.061 1205.00 0.90640 3.08099

6 27 11 5 9 2 9.833 887.32 0.99287 2.94308

7 42 13 4 15 10 11.607 1167.93 1.06472 3.06742

8 40 16 10 10 4 13.383 964.00 1.12655 2.98408

9 32 5 8 10 9 15.160 680.47 1.18069 2.63281

10 31 2 5 19 5 16.937 589.82 1.22885 2.77072

11 25 5 6 10 4 18.716 430.36 1.27220 2.63383

12 19 9 3 3 4 20.494 298.63 1.31163 2.47514

13 13 7 2 2 2 22.273 187.98 1.34778 2.27411

14 4 3 0 0 1 24.052 53.56 1.38115 1.72881

15 0 0 0 0 0 25.831 O.GO 1.41215 0.00000

16 0 0 0 0 0 27.611 0.00 1.44108 0.00000

17 0 0 0 0 0 29.390 0.00 1.45820 0.00030

TOTAL NUMBER OF GALAXIES COUNTED = 323 MAGNITUDE CUTOFF. MV = 19.0

CLUSTER CENTER AT XD = 144.719 YD = -1.784

RING WIDTH lARCMIN) = 2.0

Table 4.4.26. {aJ Ring-Count Data for Galaxy Cluster S6. Isotbermal Analysis 369 §4.4

GALAXY CLUSTER 026 21 22 58 -35 00 10 ISOTHERMAL FIT /o(r) = a-q(r//S) + 7

DUC3 Q Œ

en

CORE RADIUS: Rc=3/S~ 0.143 *h ^ Mpc

io‘ 10° 10 ' RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.26. {ej Isothermal Fit for Galaxy Cluster S6. Isotbermal Analysis 370 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 026 21 22 58 -35 00

p(r) - a q(r//S) + y

a - 957.43 ±395.58 /S - 1.06±0.11 T = 12.13±2.07

yo(r) = 1 5 4 5 . 6 8 - q ( r / 1. 05 ) + 1 2 .6 2

CORE RADIUS; REDSHIFT; Rc=3/S~ 0.143 Mpc Z = 0 .0 5 2

Table 4.4.26. [h) Cluster Parameters for Galaxy Cluster 26.

Using the cluster center as determined by the dispersion ellipse analysis, we count 323 galaxies within 14 rings of width 2.0 arcminutes and to the limiting magni­ tude m„ = 19.0. This fairly compact cluster shows a relatively uniform distribution along the East-West absissa while the North-South ordinate displays considerably more scatter. The quadrant counts show a strong avoidance of the cluster center with a strong peak shown in the first quadrant as a result of subclustering in that region. We find the cluster surface density rising fairly rapidly from the central void to a maximum near r = 11.6 arcminutes and then descending more slowly to the periphery of the cluster.

As a result of the relatively low central densities, the isothermal fit seeks to model the middle regions of the cluster where 10°’® < r < 10^’*. In this region we feel the isothermal model adequately describes the observations. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the X* minimization procedure. Isotbermal Analysis 371 §4.4 GALAXY CLUSTER 027 21 26 10 -5 1 04

rasTT CLUSTER RING C0UNT5 ERST N0RTH • » WEST %= ...... I...... 20 MIN =

S0UTH

CuuDTcn 3Tnir c b u n t o = EAST N0RTH &CST = w CLUSTER SURFACE DENSITY = 1 HM BINS == 5 0 . I 45. 4 0 . as. E 3 0 . B 2 5 . g E 20. IS, 10. 5. 0 . II fWMJLUS NWSER 12 RRCMIN WIDTH)

= EfiST ms S0ÜTH ■■■ WEST = Figure 4.4.27u (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 372 §4.4

GALAXY CLUSTER 027 21 26 10 -51 04

RING T0TAL QUADRANT C0UNTS COUNTING BSERVED LOGtRAD) LBGtOEN)

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(RRCMIN) (GflL/SQOEG)

1 9 2 3 3 1 1.259 3253.51 0.10001 3.51235

2 16 5 5 3 3 2.815 1928.01 0.44949 3.28511

3 10 2 1 3 4 4.539 723.00 0.65698 2.85914

4 19 5 6 4 4 6.295 981.22 0.79898 2.99177

5 19 3 10 3 3 8.061 763.17 0.90640 2.88262

6 13 3 5 2 3 9.833 427.23 0.99257 2.63066

7 21 7 2 6 6 11.607 583.96 1.06472 2.76639

8 18 1 3 4 10 13.383 433.80 1.12655 2.63729

9 25 3 5 9 8 15.160 531.62 1.18069 2.72560

10 18 4 4 5 5 16.937 342.48 1.22885 2.53463

11 20 4 5 7 4 18.716 344.29 1.27220 2.53592

12 19 3 7 4 5 20.494 298.63 1.31163 2.47514

13 6 3 2 0 1 22.273 86.76 1.34778 1.93832

14 8 3 5 0 0 24.052 107.11 1.38115 2.02984

15 0 0 0 0 0 25.831 0.00 1.41215 0.00000

16 0 0 0 0 0 27.611 0.00 1.44108 0.00000

17 0 0 0 0 0 29.390 0.00 1.46820 0.00300

TOTAL NUMBER OF GALAXIES COUNTED = 221 MAGNITUDE CUTOFF. MV = 19.0

CLUSTER CENTER AT XO = 33.381 YO = -57.179

RING WIDTH IWCMINI = 2.0

Table 4.4.27. (a) Ring-Count Data for Galaxy Cluster £7. Isothermal Analysis 373 §4.4

GALAXY CLUSTER 027 21 26 10 - 5 1 04 10 ' ISOTHERMAL FIT p(r) = a-q(r//S) + y

Ü 10' U LQjJ

CC ÜJ Q_ to

CORE RADIUS: Rc=3/S~ 0.129 *h ^ Mpc

10° 10 RROIfiL DISTANCE (ARCMINUTES)

Figure 4.4.27. feJ Isothermal Fit for Galaxy Glaster 21. Isothermal Analysis 374 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 027 21 26 10 - 5 1 0 4

pCr) - oc q(r//S) + y

a - 1472.53 ±388.72 /S - 1.02±0.01 y - n.40±0.40

p C r) = 2 0 6 Ü . 1 6 - q C r / l . 0 3 ) + 1 2 . 0 1 •C 5T FIT

CORE RADIUS; REDSHIFT: Rc=3/S~ 0.129 Mpc Z = 0 .0 4 6

Table 4.4.27. (b) Cluster Parameters for Galaxy Cluster S7.

Using the cluster center as determined by the dispersion ellipse analysis, we count 221 galaxies within 14 rings of width 2.0 arcminutes and to the limiting magnitude mi, = 19.0. This centrally condensed clusters shows a slight depression in the strip count data along the East-West absissa near the center of the cluster whereas the North-South ordinate merely displays a large scatter. The quadrant counts show a general tendency to increase their populations with radial distance from the center of the cluster and this same behavior is seen in the surface density distribution which displays a gradual increase in density radiallly away from the cluster center save for the dip at ring 6.

The high central density of this cluster dominates the ability of the isothermal model to fit the observations well, so as a result we see the fit riding as an envelope over the observed density distribution with better mapping only at the cluster periphery’. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the x* minimization procedure. Isotbermal Analysis 375 §4.4 GALAXY CLUSTER 028 21 29 13 - 3 5 23

rSBT CLUSTER RING C0UNTS = = e r s t mmm N0RTH HE5T

s = ZD M IN =

= = ERST S0U TH

ci_u3Tcn 3TR:r cbunto : ERST M WTM —m NEST =

CLUSTER SURFACE DENSITY = 1 m B IN S = I

3 5 . § I ! 2 5 . B I

I mWULUS NUMBER IZ RRC^IIN WIDTH:

EAST mmm S01/TH n m • C 5 T = Figure 4.4.28. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 376 §4.4

GALAXY CLUSTER 028 21 29 13 -3 5 23

(INC T0TAL QUADRANT C0UNTS COUNTING OBSERVED LOG(RAO) L0G(OEN)

JMBER C0UNT NW NE SE SW RADIUS DENSITY

(RRCMIN) (GAL/SODEG)

1 2 0 0 1 1 1.259 723.00 0.10001 2.85914

2 17 3 4 5 5 2.815 204B.51 0.44949 3.31144

3 23 5 7 5 6 4.539 1862.91 0.65698 3.22087

4 22 5 3 9 5 6.295 1136.15 0.79898 3.05543

5 28 5 7 5 11 8.061 1124.67 0.90640 3.05103

6 15 7 1 4 3 9.833 492.96 0.99267 2.69281

7 22 5 4 8 5 11.607 611.77 1.06472 2.78659

e 18 4 8 4 2 13.383 433.80 1.12655 2.63729

9 34 4 15 9 6 15.160 723.00 1.18069 2.85914

10 26 11 6 5 4 16.937 494.69 1.22885 2.69433

11 27 6 7 7 7 18.716 464.79 1.27220 2.66725

12 15 3 5 4 3 20.494 235.76 1.31163 2.37247

13 20 7 0 4 9 22.273 289.20 1.34778 2.46120

14 1 1 0 0 0 24.052 13.39 1.38115 1.12675

15 0 0 0 0 0 25.831 0.00 1.41215 0.00000

16 0 0 0 0 0 27.611 0.00 1.44108 0.00000

17 0 0 0 0 0 29.390 O.OD 1.45820 0.00000

T0TRL NUMBER 0F GALAXIES C0UNTED = 270 MAGNITUOE CUT0FF. MV = 19.0

CLUSTER CENTER AT XO = 75.807 YO = -19.961

RING WIOTH (ARCHIN) = 2.0

Table 4.4.28. (a) Ring-Count Data for Galazy Cluster £8. Isotberm al Analysis 377 §4.4

GALAXY CLUSTER 0 2 8 21 29 13 - 3 5 23

ISOTHERMAL FIT pir) = a-q(r//S) + y

y 10' L3 ë ÜJQl CE enC3

co ÜJ

I,,o

CORE RADIUS: Rc=3^~ 0.120 Mpc

10* 10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.28. (e) Isothermal Fit for Galazy Cluster 28. Isothermal Analysis 378 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 028 21 29 13 -35 23

pCr) - ot q(r//S) + y

a- 857.47 ±505.01 /S - 1.05±0.16 y - ll.B5±3.19

p(r) = 1613.81 -q(r/l.04 ) + 12.21

CORE RADIUS: REDSHIFT: Rc=3/S~ 0 .1 2 0 * h - ‘ M pc Z = 0 .0 4 4

Table 4.4.28. (b) Cluster Parameters for Galaxy Cluster S8.

Using the cluster center as determined by the dispersion ellipse analysis, we count 270 galaxies within 14 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. In this case we have a fairly centrally condensed cluster; the East-West strip counts along the absissa show a concentration East of center whereas along the North-South ordinate we find a concentration somewhat South of center. We see the same behavior displayed in the quadrant counts with an additional strong peak seen in the first and particularly in the second quadrant at ring 9. The cluster surface density distribution shows a paucity of counts near cluster center and a bifurcated distribution otherwise, with a minimum near ring 7.

The isothermal fit is somewhat effected by the low central projected density, but seems to otherwise approximate the observations, save for the bifurcated region of the distribution near {10°’® < r < 10^'^) where it overrides the data. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the X® minimization procedure. Isotbermal Analysis 379 §4.4 GALAXY CLUSTER 029 21 31 14 - 6 2 15

CLUSTER RING C0UNTS : E A S T mmm W R T H mu W EST = IHIIHIIIWIIIHIIII'IIIH 2 0 M IN = II I

:

:

s

II

— EAST ■■■ S0UTH I W EST =

CLUSTER S T R IP C0UNTS = E A S T

B IN S - I CLUSTER SURFACE DENSITY 5 0 .

s I I B i

10. I II flwiaus NUMBER 12 RRCMIN HIOTHl

= EA ST S B LAM I l E S T - Figure 4.4.29. faj Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 380 §4.4

GALAXY CLUSTER 029 21 31 14 -6 2 15

RING T0TAL QUADRANT C0UNTS COUNTING 0BSERVED L0G(RAD) LEGtOENl

NUMBER C0UNT NW NE SE SW RADIUS DENSITY

(RRCMIN) (GAL/SODEG)

1 0 0 0 0 0 1.259 0,00 0.10001 0.00000

2 8 3 0 2 3 2.815 964.00 0.44949 2.98408

3 13 3 4 3 3 4.539 939.90 0.65698 2.97308

4 16 3 9 3 1 6.295 826.29 0.79898 2.91713

5 14 3 1 4 6 8.061 562.34 0.90640 2.75000

6 26 7 5 9 5 9.833 854.46 0.99267 2.93169

7 13 4 3 2 4 11.607 361.50 1.05472 2.55811

8 19 8 3 5 3 13.383 457.90 1.12655 2.65077

9 18 5 2 7 4 15.160 382.77 1.18059 2.58293

10 19 8 2 5 4 16.937 361.50 1.22885 2.55811

11 21 3 6 8 4 18.716 361.50 1.27220 2.55811

12 16 6 3 5 2 20.494 251.48 1.31163 2.40050

13 22 7 5 8 2 22.273 318.12 1.34778 2.50259

14 11 4 2 0 5 24.052 147.28 1.38115 2.16814

15 19 6 4 3 6 25.831 236.85 1.41215 2.37447

16 23 8 2 4 9 27.611 268.21 1.44108 2.42848

17 12 7 2 2 1 29.390 131.45 1.46820 2.11878

18 7 2 4 1 0 31.170 72.30 1.49374 1.85914

19 8 3 1 4 0 32.950 78.16 1.51765 1.89300

20 7 1 0 3 3 34.730 64.88 1.54070 1.61214

T0TAL NUMBER 0F GALAXIES C0UNTED = 298 MAGNITUDE CUT0FF. MV = 19.0

CLUSTER CENTER AT XO = 8.471 YO = -118.667

RING WIDTH (ARCMIN) = 2.0

Table 4.4.29. (a) Ring-Count Data for Galazy Cluster 29. Isotbermal Analysis 381 §4.4

GALAXY CLUSTER 029 21 31 14 -62 15 10' ISOTHERMAL FIT p(r) = a-q(r//S) + 7

Ü 10^ O aÜJ CÜLU cr o to

ÜJCO

c r CD

CORE RADIUS:

Rc=3j8~ 0 .1 3 0 '•'h ^ Mpc

10' 1 0 ° 10' 10' RADIAL DISTANCE (ARCMINUTES!

Figure 4.4.29. (e) Isothermal Fit for Galaxy Cluster 29. Isotbermal Analysis 382 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 029 21 31 14 -62 15

p(r) - a q(r//S) + y

a- 698.17 ±474.22 /S - 1.05±0.18 y~ 11.62±3.51

p(r) = 1369.58-q(r/1.G3 ) + 11.95 ■ C S1 f l T

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.130 Mpc Z =0.048

Table 4.4.29. (b) Cluster Parameters for Galaxy Cluster 29.

Usiug the cluster center as determined by the dispersion ellipse analysis, we count 293 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. We find the East-West strip counts somewhat uniformly distributed on the absissa, but more widely scattered and with greater variance along the North-South ordinate. The quadrant count data shows a zone of avoidance at the calculated center of the cluster in all quadrants as well as a generally erratic appearance. The cluster surface density distribution shows a plateau-like shape cut with several minima located at ring 7 and ring 14.

The lack of counts near the center of the cluster forces a deep minima on the isothermal fit, so that point has been ignored in the analysis. The remaining observations are then fairly well modeled by the isothermal distribution with the exception of the tail of the observations that suffer a severe cutoff at the radial distance of r = 35 minutes of arc from the center of the cluster. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 383 §4.4 GALAXY CLUSTER 030 21 31 06 - 5 3 50

CLUSTER RING C0ÜNTS r r a o r r : ERST MW N0RTH mmm WEST

== 20 MIN = II

5

i 5

"..I.,,...... I,,

== ERST I S 0U TH mm W EST = =

CUUOTCrr OTTTZr c o u n t s ; ERST «M north mmm »CST =

!! CLUSTER SURFACE DENSITY I —i BINS == S E 25. Ë :E 1

II flNNULUS NUMBER 12 RRCMIN WIDTH)

: EAST w SOUTH ■■■ EEST — Figure 4.4.30. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 384 §4.4

GALAXY CLUSTER 030 21 31 06 -53 50

IING T0TRL QURORRNT C0UNTS COUNTING OBSERVED L0G(RRD) LBG(DEN)

JMBER C0UNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SODEG)

1 2 0 1 1 0 1.259 723.00 0.10001 2.85914

2 11 1 2 2 G 2 .8 1 5 1325.51 0.44949 3.12233

3 13 6 2 1 4 4 .5 3 9 9 3 9 .9 0 0 .6 5 6 9 8 2 .9 7 3 0 8

4 15 3 1 7 4 G. 295 774.65 0.79898 2.88910

5 14 3 2 6 3 8.061 562.34 0.90540 2.75000

6 23 6 4 7 G 9 .8 3 3 7 5 5 .8 7 0 .9 9 2 6 7 2 .8 7 8 4 5

7 8 2 1 3 2 11.607 2 2 2 .4 6 1 .0 6 4 7 2 2 .3 4 7 2 6

8 11 5 1 3 2 13.383 265.10 1 .1 2 6 5 5 2.42341

9 19 5 7 G 1 15.160 4 0 4 .0 3 1 .1 8 0 6 9 2.60641

10 15 3 5 3 4 1G.937 285.40 1 .2 2 8 8 5 2 .4 5 5 4 5

11 24 7 4 G 7 18.716 413.14 1.27220 2.61610

12 9 7 0 1 1 20 .4 9 4 1 4 1 .4 6 1.31163 2.15063

13 11 2 1 5 3 2 2 .2 7 3 1 5 9 .0 6 1.34778 2.20156

14 7 1 2 3 1 2 4 .0 5 2 9 3 .7 2 1 .3 8 1 1 5 1.97184

15 0 0 0 0 0 25.831 0 .0 0 1 .4 1 2 1 5 0.00000

16 0 0 0 0 0 27.611 0 .0 0 1 .4 4 1 0 8 0.00000

17 0 0 0 0 0 2 9 .3 9 0 0 .0 0 1 .4 6 8 2 0 0.00000

T0TRL NUMBER 0F GALAXIES C0UNTEO = 182 MAGNITUDE CUT0FF. MV = 1 9 .0

CLUSTER CENTER AT XO = -2 8 .7 5 5 YO = 6 4 .5 1 9

RING WIDTH (RRCMIN) = 2 .0

Table 4.4.80. faj Ring-Count Data for Galaxy Cluster SO. Isotbermal Analysis 385 §4.4

GALAXY CLUSTER 0 3 0 21 31 06 -53 50 10' ISOTHERMAL FIT /D(r) = a-q(r//S) + 7

O cc e x o CO

CO

CORE RADIUS;

Rc=3^~ 0.136 *h ^ Mpc

10'

RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.30. {eJ Isothermal Fit for Galaxy Cluster SO. Isothermal Analysis 386 §4 4

CLUSTER PARAMETERS ______GALAXY CLUSTER 030 21 31 06 -53 50

p(.r) - cx q(r//S) + y

a - 587. 05 ±347.23 /S - 1.05±D.16 7 - 11.61±3.24

/0 (r) = 1G94.55-q(r/l .04 ) + 12.15

CORE RADIUS: REDSHIFT; Rc=3/S~ 0.136 *h-i Mpc Z = 0 .0 5 0

Table 4.4.30. (b) Cluster Parameters for Galaxy Cluster SO.

Using the cluster center as determined by the dispersion ellipse analysis, we count 182 galaxies within 14 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. The cluster strip counts show a slight enhancement along the East-West absissa to the West and likewise along the North-South ordinate to the North, with the latter distribution showing slightly more variance. The quadrant counts show very few counts near the cluster center with the distribution rising and falling radiallly away from cluster center. The general cluster surface density distribution shows a deep central minimum, a slow rise to a maximum at ring 6, a dramatic fall and then a repeat of the same behavior to the cluster periphery giving a zonal type of population surface density.

The meager central density as well as the depression at r = 11.6 arcmin effect the isothermal fitting, yet it appears as if the model accomodates the observed data reasonably with possible exception of the region of sharp cutoff located at the cluster periphery. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the "best fit” determined from the minimization procedure. Isothermal Analysis 387 §4.4 GALAXY CLUSTER 031 21 32 18 - 5 2 44

CLUSTER RING C0UNTS ; ERST ■— N0RTH WEST :

cs 20 MIN =

A S aJT H

ct-uoTCPç DTnir cbuntd EAST M N0RTH mm. »CST “

II CLUSTER SURFACE DENSITY =1 W BINS =

5 ! i : c É

li fiN N a U S NUMBER 12 BRCMIN WIDTH)

= E B S T SKJTM tC S T = : Figure 4.4.81. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 388 §4.4

GALAXY CLUSTER 031 21 32 18 -52 49

RING TOTAL OUAORANT COUNTS COUNTING OBSERVED LOG(RAO) LOG(DEN)

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 0 0 0 0 0 1.259 0.00 0.10001 0.00000

2 4 1 1 1 1 2 .8 1 5 482.00 0.44949 2.68305

3 7 3 0 0 4 4 .5 3 9 506.10 0.55698 2.70424

4 15 3 5 1 6 6 .2 9 5 774.65 0.79898 2.88910

5 6 0 1 3 2 8.061 2 4 1 .0 0 0 .9 0 6 4 0 2.38202

6 14 3 5 3 3 9.833 460.09 0 .9 9 2 6 7 2.66285

7 10 2 3 3 2 11.607 278.08 1.06472 2.44417

8 17 8 1 4 4 13.383 409.70 1.12655 2.61247

9 15 2 3 7 3 15.160 3 1 8 .9 7 1.18069 2.50375

10 15 6 4 2 3 16.937 2 8 5 .4 0 1.22885 2.45545

11 11 1 6 2 2 18.716 189.36 1.27220 2.27728

12 17 5 4 5 3 20 .4 9 4 267.20 1.31163 2.42683

13 15 2 4 3 6 22 .2 7 3 2 1 6 .9 0 1.34778 2.33626

14 5 0 1 2 2 24.0 5 2 6 6 .9 4 1 .3 8 1 1 5 1.82572

15 0 0 0 0 0 25.831 0 .0 0 1 .4 1 2 1 5 0.00000

16 0 0 0 0 0 27.611 0.00 1.44108 0.00000

17 0 0 0 0 0 29.390 0.00 1.46820 0.00000

18 0 0 0 0 0 31.170 0.00 1.49374 0.0 0 0 0 0

TOTAL NUMBER OF GALAXIES COUNTED = 151 MAGNITUDE CUTOFF. MV = 19.0

CLUSTER CENTER AT xo = -3 9 .2 6 6 YD = 123.490

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.31. (a) Eing-Count Data for Galaxy Cluster SI. Isothermal Analysis 389

GALAXY CLUSTER 031 21 32 18 -52 44

ISOTHERMAL FIT p(r) = a-q(r//S) + 7

^ 1 0 CD 5 Πa 00

cn

X CE Π10' CD

CORE RADIUS;

Rc=3jS~ 0.119 *h ^ Mpc

RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.81. fej Isothermal Fit for Galaxy Cluster SI. Isotbermal Analysis 390 §4^

CLUSTER PARAMETERS ______GALAXY CLUSTER 031 21 32 18 -52 44

pCr) - £x q(r//S) + 7

a - 446.80 ±265.69 /S - l.G5±0.18 7 - 11.61±3.55

yO(r) = 829. 25-q(r/l .03 ) + 11.97

CORE RADIUS; REDSHIFT: Rc=3/S~ 0.119 *li-i Mpc Z = 0 .0 4 4

Table 4.4.31. fbj Cluster Parameters for Galaxy Cluster SI.

Using the cluster center as determined by the dispersion ellipse analysis, we count 151 galaxies within 14 rings of width 2.0 arcminutes and to the limiting mag­ nitude rriy = 19.0. From the cluster strip counts we notice that this scattered,, sparsely populated cluster shows a slight density enhancement West of cluster cen­ ter along the East-West absissa; the distribution along the North-South ordinate appears erratic and displays a wide variance. The quadrant counts show a zone of avoidance near the cluster center with a generally erratic appearance. Likewise,the cluster surface density distribution displays a seies of peaks and troughs of various widths before a sharp cutoff after ring 12.

The lack of appreciable surface density near the ceneter of the cluster as well as the peripheral cutoff makes the isothermal fit difficult to model, but we approach some level of approximation of the observations near the middle ranges of the cluster. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 391 S44 GALAXY CLUSTER 032 21 41 46 - 5 1 44

CLUSTER RING COUNTS == ERST mm. north mmu W EST :

== 20 MIN = IÎ I

s

:

I II

= = ERST SOUTH

CLUSTER STRIP C0UNTS : ERST WRTH M« tCST

CLUSTER SURFACE DENSITY e — 1 MM BINS = 50. I

3 5 . 5

f 3 0 .

e c r i

0.

L R fM JLUS NWBER 12 RRCMIN WIDTH)

O«^N(n«*mwr>coo)o«^csn«*m(0r^cD7^Q = ERST ■■■ SOUTH Figure 4.4.32. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 392 §4.4

GALAXY CLUSTER 032 21 41 46 -51 44

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) L0C1OEN)

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GRL/SQOEG)

1 2 0 2 0 0 1.259 723.00 0.10001 2.85914

2 5 2 0 0 3 2 .8 1 5 6 0 2 .5 0 0 .4 4 9 4 9 2 .7 7 9 9 6

3 6 0 2 1 3 4.539 433.80 0.65698 2.63729

4 4 0 0 2 2 6 .2 9 5 2 0 6 .5 7 0.79898 2.31507

5 10 0 2 5 3 8.061 401.67 0.90640 2.60387

6 13 3 2 5 3 9.833 427.23 0 .9 9 2 6 7 2 .6 3 0 6 6

7 13 2 1 5 5 11.607 3 6 1 .5 0 1 .0 6 4 7 2 2.55811

6 8 1 1 4 2 13.383 192.80 1.12655 2.28511

9 12 2 6 2 2 15.160 255.18 1.18069 2.4 0 6 8 4

10 18 2 3 6 5 1 6.937 3 4 2 .4 8 1.2 2 8 8 5 2.5 3 4 6 3

11 20 6 4 6 4 1 8.716 3 4 4 .2 9 1.27220 2.53692

12 12 4 3 2 3 20.494 188.61 1.31163 2.27556

13 IS 9 4 2 1 22.273 231.36 1.34778 2.35429

14 12 4 3 1 4 2 4 .0 5 2 160.67 1.38115 2.20593

15 11 6 2 0 3 25.831 1 3 7 .1 2 1 .4 1 2 1 5 2 .1 3 7 1 0

16 5 1 0 2 2 27.611 58.31 1.44108 1.76572

17 13 3 6 2 2 2 9 .3 9 0 142.41 1.46820 2. 15354

18 8 2 0 0 6 31.170 82.63 1.49374 1.91713

19 3 0 0 2 1 32.950 29.31 1.51785 1.46703

20 2 0 0 1 1 34.730 18.54 1.54070 1.26808

TOTAL NUMBER OF GALAXIES COUNTED = 197 MAGNITUDE CUTOFF. MV = 1 9 .0

CLUSTER CENTER AT XO = -9 6 .5 5 3 YO = -93.917

RING WIDTH (RRCMIN) = 2 .0

Table 4.4.32. faj Ring-Gount Data for Galaxy Cluster S2. Isothermal Analysis 393 &L4

GALAXY CLUSTER 032 21 41 46 -51 44

ISOTHERMAL FIT p(r) = a-q(r/)S) + y

ODl

at: ZDŒ a CD tr LlJ O- cn UJ ŒX CE CD

CORE RADIUS:

Rc=3j8~ 0.117 Mpc

10' 10° 10' RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.32. (e) Isothermal Fit for Galaxy Cluster S2. Isothermal Analysis 394 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 032 21 41 46 -51 44

p(r) - a-q

oc- 380.87 ±201.58 /S - 1.05±0.17 y - 11.90±3.34

p(r) = 671,46-q(r/1.04 ) + 12.69 0E 3 T F IT

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.117 Mpc Z = 0 .0 4 3

Table 4.4.32. (b) Cluster Parameters for Galaxy Cluster S2.

Using the cluster center as determined by the dispersion ellipse analysis, we count 193 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. We find the East-West strip counts slightly enhanced both East and West of the cluster center whereas the North-South ordinate shows an excess North of center as well as a relatively large variance. The quadrant counts show a meager population close to the cluster center but then a rise that is obsers'ed in all directions. There is a lagre peak in the distribution at about ring 13 in the first quadrant. The cluster surface density distribution shows an an erratic rise to a maximum at a radial distance of about r = 18.7 arcminutes, after which the distribution falls, does a quick rise and falls again.

We find the isothermal fit modeling the observational data fairly well with exceptions at the deep data troughs like that seen at radial distance r = 13.4 arcminutes. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isothermal Aualysis 395 §4.4 GALAXY CLUSTER 033 21 42 51 - 5 7 29

CLUSTER RING C0UNTS ; ERST mmm N0RTH WEST = . . == 20 MIN = : I s I *

II inuim tiiiiiim tim iui» iitiii*i»iiÜM iiniiU = E R S T I S0U TH I WEST =

CLUSTER STRIP C0UNTS : e r s t mmm «RTH ICST = .III tn m III! M l ttiii I n il iim iiii u ti I ti 111 II CLUSTER SURFACE DENSITY II =1 B I N S = so.

4 5 .

4 0 .

35. S ! 30. i 25. Ë i 20 . 15. 10.

5 . 0. II ANNULUS N im R (2 RRCMIN WIDTH)

r= EAST n i S0ÜTH *■* WEST = Figure 4.4.33. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 396 §4.4

GALAXY CLUSTER 033 21 42 51 -57 29

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) LOG(DEN)

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 12 2 4 2 4 1.259 4338.D2 0 .10001 3.63729

2 21 6 5 6 4 2 .8 1 5 2530.51 0.44949 3.40321

3 19 6 6 4 3 4 .5 3 9 1373.71 0 .6 5 6 9 8 3.13789

4 41 8 9 13 11 6.295 2117.37 0 .7 9 8 9 8 3.32580

5 26 7 4 10 5 8.061 1044.34 0 .9 0 6 4 0 3.01884

G 30 6 8 8 6 9 .8 3 3 985.91 0.99267 2.99384

7 48 9 13 17 9 11.607 1334.77 1.06472 3.12S41

a 38 8 5 18 7 13.383 915.80 1.12655 2.96180

s 45 15 10 13 7 15.160 956.92 1.18069 2.98087

10 40 10 12 11 7 16.937 76 1 .0 6 1 .22885 2.83142

11 30 14 3 8 5 18.716 516.43 1.27220 2.71301

12 37 12 11 9 5 20.494 581.55 1.31163 2.76458

13 45 22 10 8 5 22.273 650.70 1.34778 2.81338

14 30 11 4 8 7 2 4 .0 5 2 4 0 1 .6 7 1.38115 2.60387

15 32 15 3 7 7 25.831 398.90 1.41215 2.60086

16 40 16 5 10 9 27.611 466.45 1.44108 2.66881

17 26 4 2 12 8 29.390 284.82 1.46820 2.45457

18 10 3 0 3 4 31.170 103.29 1.49374 2.01404

19 4 0 0 1 3 32.950 39.08 1.51785 1.59197

20 0 0000 34.730 D.DO 1.54070 0.00000

T0TRL NUMBER OF GALAXIES COUNTED = 574 MAGNITUDE CUTOFF. MV = 1 9 .0

CLUSTER CENTER AT XO = -7 4 .2 1 5 YO = 134.600

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.88. (a) Ring-Count Data for Galaxy Cluster SS. Isotbermal Analysis 397 §4.4

GALAXY CLUSTER 033 21 42 51 -57 30

ISOTHERMAL FIT p(r) = a-q(r//S) + 7

Ü 1 0 ^ O a

0 01

a . tn

CORE RADIUS;

R c= 3 )g- 0.114 Mpc

10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.33. feJ Isothermal Fit for Galaxy Cluster SS. Isotbermal Analysis 398 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 033 21 42 51 - 5 7 30

p(r) - a q(r//S) + y

a - 2389.51 ±516.81 /S - 1.02±0.01 y - 11.77±0.40

p(r) = 3 1 5 7 . 3 5 -q(r/l .0 3 ) + 1 2 .3 7 mCST FIT *

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.114 *h.“^ Mpc Z = 0 .0 4 2

Table 4.4.33. (bj Cluster Parameters for Galaxy Cluster SS.

Using the cluster center as determined by the dispersion ellipse analysis, we count 574 galaxies within 19 rings of width 2.0 arcminutes and to the limiting magnitude rriv = 19.0. We find the East-West strip count distribution fairly smooth and without any extraordinary maxima or minima; the North-South distribution on ther other hand displays a large excess near the cluster center and a rather large variance. The former suggests a linear feature running East-West along the cluster somewhat South of center. The cluster surface density increases with increasing radial distance to a maximum near ring 8 after which it suffers a slow decline. We see this behavior in the quadrant counts as well.

The isothermal fit to the observed data appears to model the cluster density better in the outerlying regions of the cluster than where we have significant dips in the observations. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit" determined from the minimization procedure. Isotbermal Analysis 399 §4.4 GALAXY CLUSTER 034 21 43 46 - 4 4 06

CLUSTER RING C0UNTS ERST mmm N 0R TH W EST =

= 2D MIN =r II I

:

:

I

= = E A S T WEST —

CLU3TCn 3TRir C 0 U N T 3 ERST ••• N0RTM «»• leST ==

CLUSTER SURFACE DENSITY 1! = 1 HI B I N S — 50.

4 5 .

4 0 .

3 5 . S

Î 3 0 .

2 5 . E 20. s a 1 5 . É 10.

5 . 0.

= ERST ■■■ S0UTR mmm W EST > = Figure 4.4.34. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 400 §4.4

GRLBXY CLUSTER 034 21 43 46 -44 06

RING T0TAL QUADRANT COUNTS COUNTING OBSERVED L0G(RAD) LOG(DENI

NUMBER C0UNT NW NE SE SW RADIUS DENSITY

(RRCMIN) (GAL/SQDEG)

1 2 0 0 1 1 1.259 723.00 D.10001 2.85914

2 8 1 3 1 3 2 .8 1 5 9 6 4 .0 0 0.44949 2.98408

3 18 2 5 7 4 4 .5 3 9 1301.41 0 .6 5 6 9 6 3 .1 1 4 4 1

4 26 9 9 6 2 6.295 1342.72 0 .7 9 8 9 8 3 .1 2 7 9 9

5 24 5 6 6 7 8.061 964.00 0.90640 2.98408

6 27 7 9 8 3 9 .8 3 3 8 8 7 .3 2 0 .9 9 2 5 7 2 .9 4 8 0 8

7 21 5 2 5 9 1 1 .6 0 7 5 8 3 .9 6 1.06472 2.76639

B 25 11 5 2 7 13.383 602.50 1 .12655 2 .7 7 9 9 5

9 20 3 4 5 8 15.160 425.30 1.18069 2 .6 2 8 5 9

10 18 7 6 3 2 16.937 342.48 1.22885 2 .5 3 4 5 3

11 35 10 9 12 4 18.716 602.50 1.27220 2 .7 7 9 9 6

12 19 9 2 3 5 20.494 298.63 1 .3 I I6 3 2 .4 7 5 1 4

13 22 10 4 6 2 22.273 318.12 1.34778 2.50259

H 35 7 5 17 8 24.052 468.61 1.38115 2 .6 7 0 8 1

15 24 5 6 6 7 25.831 299.17 1.41215 2.47592

IB 22 5 5 8 4 2 7 .6 1 1 256.55 1.44108 2 .4 0 9 1 7

17 26 ID 3 8 5 29.390 284.82 1 .46820 2 .4 5 4 5 7

18 12 2 6 1 3 31.170 123.94 1.49374 2 .0 9 3 2 2

19 0 0 0 0 0 3 2 .9 5 0 0 .0 0 1.51785 0.00000

20 0 0 0 0 0 3 4 .7 3 0 0 .0 0 1.54070 0 .0 0 0 0 0

T0TRL NUMBER 0F GALAXIES C0UNTED = 384 MAGNITUDE CUT0FF. MV = 1 9 .0

CLUSTER CENTER AT XO = 119.835 YO = 51.560

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.34. (a) Ring-Count Data Jor Galaxy Cluster S4> Isotbermal Analysis 401 §4.4

GALAXY CLUSTER 034 21 43 46 - 4 4 06

ISOTHERMAL FIT pir) = aq(r//S) + y

CK: =3cr g cn

X cr OCE

CORE RADIUS;

Rc=3/?~ 0.131 Mpc

10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.34. (e) Isothermal Fit for Galaxy Cluster S4- Isothermal Analysis 402 §4^

CLUSTER PARAMETERS GALAXY CLUSTER 034 21 43 46 -44 06

p(r) - a-q(r// 5 ) + y

a - 704.08 ±416.38 /S - 1.05±0.16 y - 11.9G±3.09

p(r) = 1329. 19-q(r/l .04 ) + 12.84

CORE RADIUS: REDSHIFT: R c= 3 /9 ~ 0.131 * h - i Mpc Z = 0 .0 4 8

Table 4.4.34. (b) Cluster Parameters for Galaxy Cluster S4.

Using the cluster center as determined by the dispersion ellipse analysis, we count 384 galaxies within 18 rings of width 2.0 arcminutes and to the limiting magnitude m.y = 19.0. We find fairly large disperions in both the East-West and North-South components of the strip counts with a slight enhancement South of the cluster center where we see an obvious concentration of galaxies. As shown by the quadrant counts, however, the center of the cluster is nearly devoid of galaxies. We also see that the first quadrant represents the most populous region of the cluster. The cluster surface density rises rapidly as we move from the cluster center to a maximum after which it falls and rises sharply once more through two peaks and then reaches the cluster periphery.

The isothermal fit to this data overshoots near the cluster center but more adequately represents the observations beyond the middle of the cluster. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the X® minimization procedure. Isotbermal Analysis 403 §4.4 GALAXY CLUSTER 035 21 44 41 - 4 6 13

CLUSTER RING C0UNT5 s : e r s t mmm NORTH WEST =

=: 20 MIN = i s A/I

:

K 1 II

= = E R S T S0JTH '

CLU3Ttr^ 3 T n ir CBUNT3

; e r s t —« NBRTH «ST ==

CLUSTER SURFACE DENSITY t = 1 MM BINS = E I

SS. 5 I I 25. Ê s

:

— ERST S 0 U T H • • • Figure 4.4.35. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (dj Cluster Surface Density. Isothermal Analysis 404 §4.4

GALAXY CLUSTER 035 2144 41 -46 13

RING T0TAL QUADRANT C0UNTS COUNTING OBSERVED L0G(RAO) LOG(DEN)

NUMBER C0UNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 8 4 2 2 0 1.259 2892.01 0.10001 3.45120

2 8 4 3 0 2 2 .8 1 5 1084.50 0.44949 3.0 3 5 2 3

3 19 2 6 9 2 4.539 1373.71 0.65698 3 .1 3 7 8 9

4 22 2 2 13 5 6 .2 9 5 1136.15 0 .79898 3 .0 5 5 4 3

5 18 5 3 6 4 8.061 723.00 0.90640 2.85914

6 13 0 4 S 4 9.833 427.23 0.99267 2 .6 3 0 5 6

7 14 0 5 3 5 1 1 .6 0 7 389.31 1.06472 2 .5 9 0 2 9

8 22 8 5 7 2 1 3 .3 8 3 5 3 0 .2 0 1.12655 2.72444

9 16 4 5 1 6 15.160 340.24 1.18069 2.53178

10 24 7 9 3 5 1 6 .9 3 7 4 5 6 .6 3 1.22885 2 .6 5 9 5 7

11 25 3 7 2 13 18.718 430.36 1.27220 2.63383

12 34 8 5 5 16 2 0 .4 9 4 5 3 4 .3 9 1.31163 2.72786

13 36 9 11 8 8 2 2 .2 7 3 520.56 1.34778 2 .7 1 6 4 7

.14 21 6 8 3 4 24.052 281.17 1.38115 2 .4 4 8 9 7

15 21 6 1 4 10 25.831 261.78 1.41215 2 .4 1 7 9 3

16 19 10 4 2 3 2 7 .6 1 1 2 2 1 .5 7 1.44108 2 .3 4 5 5 0

17 16 0 6 4 4 2 9 .3 9 0 175.27 1.46820 2 .2 4 3 7 2

18 12 0 2 9 1 3 1 .1 7 0 123.94 1.49374 2 .0 9 3 2 2

19 4 0 2 2 0 3 2 .9 5 0 39.08 1.51785 1.59197

20 1 0 0 1 0 3 4 .7 3 0 9.27 1.54070 0 .9 5 7 0 5

TOTAL NUMBER 0F GALAXIES COUNTED = 354 MAGNITUDE CUT0FF. MV = 1 9 .0

CLUSTER CENTER AT XO = 107.000 YO = -61.752

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.85. (a) Ring-Count Data for Galaxy Cluster S5. Isothermal Analysis 405 §4^

GALAXY CLUSTER 0 3 5 21 44 41 - 4 6 13 ]0' ISOTHERMAL FIT p(r) = aq(r//5) + y

Ü 10^ O UJo

CO

X c r

CORE RADIUS: Rc=3/?~ 0.116 Mpc

10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.35. (e) Isothermal Fit for Galaxy Cluster S5. Isothermal Analysis 406 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 035 21 44 41 -46 13

p(r) - a-q(r//S) + -y

a - 976. A5 ±659. 11 /S - 1.05 ±0.17 -y - 11.73±3.38

p(r) = 1951.54-q(r/l.03 ) + 12.36

CORE RADIUS: REDSHIFT: R c= 3/S ~ 0.116 Mpc Z = 0 .0 4 3

Table 4.4.35. fbj Cluster Parameters Jor Galaxy Cluster S5.

Using the cluster center as determined by the dispersion ellipse analysis, we count 354 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude rtiy = 19.0. The cluster strip counts reveal a slight enhancement West of center along the East-West absissa as well as another along the North-South ordinate somewhat South of center. Both of these are regions of subclustering in the body of the main cluster. These are also evident in the quadrant counts as peaks in the third and fourth quadrants. The cluster surface density distribution reveals these features as peaks above the general radial rise in density away fron the cluster center.

The isothermal analysis has to contend with the high central density of this cluster as well as the two subclusterings. As a result, it tends to overshoot the observations near the center of the cluster and find a better fit at the cluster pe­ riphery'. The results of the analysis are seen in the table above which gh’es the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 407 §4.4 GALAXY CLUSTER 036 21 50 32 - 5 8 04

CLUSTER RING C0ÜNTS = = ERST B M N0RÎH w WEST : ...... == 20 MIN = i:

A ! 1 « • fl K tf M « m « i i

i:

A ERST S0UTH mmm WEST =

CLU3TCR OTHir C0UNT3 : E R S T m m N 0RTH mm W EST =

II CLUSTER SURFACE DENSITY

— 1 MM BINS ==

S I I 2 5 . B i 3 ë

II AfWULUS NUMBER 1 2 RRCMIN WIDTH)

o«^(v)D«'i/)cor^oo)O->(sjtnv*Ln(0r*‘(DOo

: ERST m S0U1H « I NEST = Figure 4.4.36. faj Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. EA6

Isotbermal Analysis 408 §4.4

GALAXY CLUSTER 036 21 50 32 -5 8 04

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) LOG(DEN)

UMBER COUNT NW NE SE SW RADIUS DENSITY

(RRCMIN) (GAL/SQDEG)

1 12 0 6 3 3 1.259 4338.02 0.10001 3.63729

2 23 6 8 3 6 2 .8 1 5 2771.51 0.44949 3.44272

3 27 5 7 8 7 4.539 1952.11 0.65698 3 .2 9 0 5 0

4 43 12 7 13 11 6.295 2220.65 0.79898 3.34648

5 28 9 7 8 4 8 .0 6 1 1124.67 0.90640 3.05103

6 26 7 6 7 6 9 .8 3 3 8 5 4 .4 6 0.9 9 2 6 7 2 .9 3 1 6 9

7 40 13 12 4 11 1 1 .6 0 7 1112.31 1.06472 3 .0 4 6 2 3

8 43 9 14 12 8 1 3 .3 8 3 1036.30 1.12655 3.01549

9 24 3 8 8 5 15.160 510.35 1.18069 2 .7 0 7 8 7

10 15 7 0 5 3 1 6 .9 3 7 2 8 5 .4 0 1.22885 2.45545

11 12 2 0 2 8 1 8 .7 1 6 2 0 6 .5 7 1.27220 2 .3 1 5 0 7

12 2 0 0 1 1 20.494 31.43 1.31163 1.49741

13 0 0 0 0 0 2 2 .2 7 3 0.00 1.34778 O.OCDDO

14 0 0 0 0 0 24.052 0.00 1.38115 0.00000

TOTAL NUMBER OF GALAXIES COUNTED = 295 MAGNITUDE CUTOFF, MV = 1 9 .0

CLUSTER CENTER AT XO = - 1 2 7 .5 3 4 YO = 102.014

RING WIDTH (ARCMIN) = 2 .0

Table 4.4.36. (a) Ring-Count Data for Qalazy Cluster S6. Isothermal Analysis 409

GALAXY CLUSTER 036 21 50 32 -58 04

ISOTHERMAL FIT p(r) = aq(r//S) + 7

Ü 1 0 ^ CÛ LU

CL O CO

X CE CJ

CORE RADIUS: Rc=3y?~ 0.135 Mpc

io‘ 10° 10’ RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.36. (ej Isothermal Fit for Galaxy Cluster S6. Isotbermal Analysis 410 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 036 21 50 32 - 5 8 04

/7(r) - a q(r//S) + y

a - 2707.31 ±398.52 /S - l . O S i O . Q O y - 11.60±0.24

p(r) = 3244.86-q(r/l . 03 ) + 11 . 93 •E S T F IT

CORE RADIUS: REDSHIFT: Rc=3;S~ 0.135 Mpc Z = 0 .0 5 0

Table 4.4.36. (b) Cluster Parameters jor Galaxy Cluster S6.

Using the cluster center as determined by the dispersion ellipse analysis, we count 295 galaxies within 12 rings of width 2.0 arcminutes and to the limiting mag­ nitude ruv = 19.0. The strip counts reveal what the eye beholds as a highly centrally condensed compact cluster. The East-West distribution is fairly symmetric about the center of the cluster, whereas we find a slight concentration South of center along the North-South absissa. The quadrant counts show the main central concentration as coming from the second and fourth quadrants and some effects of subclustering as evidenced by several sharp peaks in the distributions. The cluster surface density map shows a steep rise from center which later rounds off and terminates at the cluster periphery. Two peaks are seen to dominate the distribution.

The isothermal fit envelopes the observational data and is again dominated by the high density peaks. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isothermal Analysis 411 §4.4 GALAXY CLUSTER 037 21 55 17 - 6 0 35

CLUSTER RING C0UNTS rm n = = ERST mmm WRTH w WEST

z = 2 0 MIN =

S0JTH

CLUDTCn OTTTir C0UNTO

E A S T m m NRTH »■ WEST :

CLUSTER SURFACE PENSITY II B IN S = II i 50. -Ï I I I I I I I I I I 1 45. 40. 35. S E s 30. s * 25. B : 20. : s 35. 10. 5. g 3 0. II II AWULUS NUMBER (2 ARCMIN WIDTH)

ERST WEST = Figure 4.4.S7. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 412 §4.4

GALAXY CLUSTER 037 21 55 17 -6 0 35

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAO) LOGIDEN)

NUMBER COUNT NW NE SE SU RADIUS DENSITY

(ARCMIN) (GAL/SQDEG) 1 4 0 1 2 1 1 . 2 5 9 1 4 4 6 .0 1 0.10001 3.16017 2 2 9 11 4 4 10 2.815 3494.51 0.44949 3.54339 3 IB G 4 1 7 4.539 1301.41 0.65698 3.11441 4 2 6 1 0 0 4 1 2 6 . 2 9 5 1 3 4 2 .7 2 0.79898 3.12799 5 3 0 5 8 G 11 8 .0 6 1 1205.00 0.90540 3.08099 6 3 0 3 6 8 13 9.833 985.91 0 .9 9 2 6 7 2 .9 9 3 8 4 7 2 6 5 3 10 8 1 1 .6 0 7 723.00 1.06472 2.85914

e IB 2 5 4 5 1 3 .3 8 3 385.60 1.12655 2.58614

g 2 8 11 5 5 7 15.160 595.41 1.18069 2.77482

10 2 3 9 3 7 4 1 6 .9 3 7 4 3 7 .6 1 1 .2 2 8 6 5 2.64108 11 3 9 8 9 18 4 18.716 . 671.36 1.27220 2 .8 2 6 9 6 12 4 8 13 15 8 12 2 0 .4 9 4 7 5 4 .4 4 1.31163 2.87762 13 4 7 14 16 12 5 22.273 679.62 1 .3 4 7 7 8 2 .8 3 2 2 7 14 5 4 11 21 18 4 2 4 .0 5 2 723.00 1.38115 2 .8 5 9 1 4 15 44 6 2 5 10 3 25.831 548.48 1.41215 2.73916 16 2 0 7 0 G 7 2 7 .6 1 1 2 3 3 . 2 3 1.44108 2.36778 17 1 0 5 0 1 4 29.390 109.55 1.46820 2.03950

16 1 3 4 0 0 9 3 1 .1 7 0 134.27 1.49374 2.12799 19 7 0 0 0 7 3 2 .9 5 0 6 8 . 3 9 1 .5 1 7 8 5 1.83501 2 0 0 0 0 0 0 3 4 .7 3 0 0.00 1 .5 4 0 7 0 0.00030

T0TAL NUMBER OF GALAXIES COUNTED = 512 MAGNITUDE CUTOFF. HV = 19 .0

CLUSTER CENTER AT XO = 98.536 YO = -32.630

RING WIDTH 1ARCMIN] = 2.0

Table 4.4.87. faj Ring-Count Data for Galaxy Cluster 57. Isothermal Analysis 413 §44

GALAXY CLUSTER 037 21 55 17 -60 35

ISOTHERMAL FIT yo(r) = a-q(r//S) + 7

g g

Œ ZD C3 CO Û:

ccX ΠCD

CORE RADIUS; Rc=3/S~ 0.130 Mpc

10' 10° 10' RADIAL DISTANCE lARCMINUTES)

Figure 4.4.37. fej Isothermal Fit for Galaxy Cluster 57. Isothermal Analysis 414 §4.4

CLUSTER PARAMETERS ______GALAXY CLUSTER 037 21 55 17 -60 35 ______

p (r) - a qCr/yS) + y

a- 1546.91 ±456.11 /S •= 1 .0 2 ± 0 .0 1 7 = 11.58±0.50

p(r) = 2251.82-qCr/1.04 ) + 12.35 •tST riT

CORE RADIUS; RED SHIFT: Rc=3/S~ 0.130 Mpc Z = 0.048

Table 4.4.37. (b) Cluster Parameters for Galaxy Cluster 81.

Using the cluster center as determined by the dispersion ellipse analysis, we count 512 galaxies within 19 rings of width 2.0 arcminutes and to the limiting mag­ nitude m„ = 19.0. This centrally and peripherally condensed cluster shows a fairly symmetric distribution about the East-West absissa with exception at the Eastward tail of the mapping; likewise along the North-South ordinate we see concentrations both North and South of center. We see the effects of sub clustering in the quadrant counts with the more central condensation arising from the fourth quadrant contri­ bution and the unusual arc of galaxies at the periphery of the cluster arising from contributions from the second and third quadrants. This effect is also seen in the cluster surface density distribution with its exaggerated groupings at the extremes of the cluster.

We find the isothermal fit to model the observations poorly mainly because of the consentrations in the data. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermaî Analysis 415 §4.4 GALAXY CLUSTER 038 21 58 09 - 6 0 11

CLUSTER RING COUNTS =: ERST mmm N0RTH m n WEST =

~ 20 MIN 1 i: :i s 8 M , 1 •A 1 « • • m n M • ■ ■ s

- i : i J1 /k. i: i 8 8 li

= ERST SOflH i WEST = n « U * K %

CI-U3TCTT OTTTir C0UNT3 sz ERST —» HBRTn mam ftCST =

B CLUSTER SURFACE DENSITY s=l MM BINS == 50. S I 45. 40. 35. 5 I 30. n 25. f 2 0 . IS. i 10. T 5. 0. c

= EnST wm SauTH ■» ICST — Figure 4.4.88. (a) ClusteT Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 416 §4.4

GALAXY CLUSTER 038 21 58 09 -6 0 11

;iNG TBTAL QUAORANT COUNTS COUNTING OBSERVED LOGIRAO) L0G1DEN)

JHBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 16 2 13 1 0 1.259 5784.02 0.10001 3.76223 2 22 1 5 9 7 2.815 2651.01 0.44949 3.42341

3 32 7 7 15 3 4.539 2313.61 0.65698 3.36429

4 24 5 5 7 7 G. 295 1239.43 0.79898 3.09322 5 23 6 6 5 G 8.061 923.84 0.90640 2.96550 G 24 5 2 g 8 9.833 788.73 0.99267 2.89693 7 27 6 5 10 G 11.607 750.81 1.06472 2.87553 8 38 17 5 11 5 13.383 915.60 1.12655 2.96180

9 30 7 8 11 4 15.160 637.94 1.18069 2.80478

10 24 ID 1 9 4 16.937 456.63 1.22885 2.65957

11 13 3 0 4 6 18.716 223.79 1.27220 2.34983

12 19 8 2 3 G 20.494 298.63 1.31163 2.47514

13 17 5 9 3 0 22.273 245,82 1.34778 2.39052

14 3 0 3 G 0 24.052 40.17 1.38115 1.60387

15 0 0 0 0 0 25.831 0.00 1.41215 0.00000

16 0 0 0 0 0 27.611 0.00 1.44108 0.00000

TOTAL NUMBER 0F GALAXIES C0ÜNTED = 312 MAGNITUDE CUT0FF, MV = 19.0

CLUSTER CENTER AT XO = 80.599 YO = -10.760

RING WIDTH (ARCMIN) = 2.0

Table 4.4.S8. (a) Ring-Count Data for Galaxy Cluster S8. Isotbermaî Analysis 417 §4 4

GALAXY CLUSTER 038 21 58 06 -60 11

ISOTHERMAL FIT pCr) = a-q(r//S) + y

ë 10 o LÜ O LU û:: Œ O

CH

e n

X ΠO

CORE RADIUS; Rc=3)S~ 0.175 *h 1 Mpc

RflDIRL DISTANCE (ARCMINUTES)

Figure 4.4.38. (e) Isothermal Fit for Galaxy Cluster S8. Isothermal Analysis 418 544

CLUSTER PARAMETERS GALAXY CLUSTER 0 3 8 21 5 6 08 - 6 0 11

p(r) - a-q

a - 3173. 93 ±287.48 /S - 1.02 ±0.01 y - 11.73±G.16

pCr) = 3487. 59-q(r/1. 03 ) + 11.90

CORE RADIUS; REDSHIFT: Rc=3/S~ 0.175 Mpc Z = 0 .0 6 5

Table 4.4.38. (b) Cluster Parameters for Galaxy Cluster 38.

Using the cluster center as determined by the dispersion ellipse analysis, we count 312 galaxies within 14 rings of width 2.0 arcminutes and to the limiting mag­ nitude = 19.0. The cluster strip counts reveal a strong concentration Eastward of cluster center along the East-West absissa. To the eye this appears as a some­ what linear concentration running North-South from a region just South-East of the cluster center to the cluster periphery. The quadrant counts show the effects of subclustering as evidenced by the extraordinarj' concentration in the fourth quad­ rant. The cluster surface density distribution also shows these effects as a gross increase in density near the cluster periphery.

We find the isothermal fit greatly effected by the concentrations noted above so that the fit tends to overide the observations and settle on the peaks of the density distribution. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the ’’best fit” determined from the minimization procedure. Isotbermaî Analysis 419 §4.4 GALAXY CLUSTER 039 22 01 11 - 5 8 18

CLUSTER RING COUNTS = E R S T m m M R T H mmm N E S T :

= 2 0 MIN =

== ERST ■■ S0LTTH mmm WEST = • ««••BUM

CLU3Tcrc s i r i r cbunts

EAST » NBRTH m i » £ 5 T &=

CLUSTER SURFACE DENSITY 8 B IN S J B

as. S

I 3 0 . S I = . s I 10 . Ü 1 5 .

li

Figure 4.4.39. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 420 §4.4

GALAXY CLUSTER 039 22 0! 11 -5 8 18

RING TBTAL QUADRANT COUNTS COUNTING 0BSERVEO L0CIRAOI LBGIDEN)

NUMBER CBUNT NW NE 5E SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 5 0 0 2 3 1.259 1807.51 0.10001 3.25708

2 10 0 2 3 5 2.815 1205.00 0.44949 3.08099

3 9 3 2 1 3 4.539 650.70 0.65698 2.81338 4 e 4 0 2 2 6.295 413.14 0.79898 2.6161D

5 12 4 0 2 6 8.061 482.00 0.90640 2.68305 6 3 1 2 0 0 9.833 98.59 0.99267 1.99394 7 17 5 4 2 6 11.607 472.73 1.06472 2.67462 e 18 4 5 8 1 13.383 433.80 1.12655 2.63729

9 16 5 3 6 2 15.160 340.24 1.18069 2.53178

10 26 11 7 5 3 16.937 494.69 1.22885 2.69433

11 25 9 7 6 3 18.716 430.36 1.27220 2.63383 12 25 9 4 9 3 20.494 392.94 1.31163 2.59432 13 27 9 4 9 5 22.273 390.42 1.34778 2.59153

14 32 9 3 9 11 24.052 428.45 1.38115 2.63190

15 32 12 6 9 5 25.831 398.90 1.41215 2.60086 16 25 8 5 2 10 27.611 291.53 1.44108 2.46469

17 27 10 8 5 4 29.390 295.77 1.46820 2.47096 18 6 1 2 3 0 31.170 61.97 1.49374 1.79219 19 6 0 2 3 1 32.950 58.62 1.51785 1.75806

20 2 0 0 2 0 34.730 18.54 1.54070 1.25833

TBTAL NUMBER BF GALAXIES COUNTED = 331 MAGNITUDE CUT0FF. MV = 19.0

CLUSTER CENTER AT XO = 63.530 YO = 90.895

RING WIDTH lARCMIN) = 2.0

Table 4.4.89. (a) Ring-Count Data for Galaxy Cluster S9. Isotberma.1 Analysis 421 §4.4

GALAXY CLUSTER 039 22 01 11 -58 18 10' ISOTHERMAL FIT p(.r) = a-q(r//S) + y

a i CD Q

CL C3 CD g CO

CORE RADIUS; Rc=3/S~ 0.116 *h ^ Mpc

10' 10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.89. (e) Isothermal Fit for Galaxy Cluster S9. Isothermal Analysis 422 S4.4

CLUSTER PARAMETERS GALAXY CLUSTER 039 22 01 11 - 5 8 18

p(r) - a-q(r//S) + y

a - 685.34 ±437.50 /S - 1.05±0.17 y -= ll.B3±3.33

p ( r ) = aOT fIT 1 3 3 5 .3 4 - q •*’ C r /l.03 ) + 1 2 . 6 9

CORE RADIUS: REDSHIFT: Rc=3/8~ 0.116 Mpc Z = 0 .0 4 3

Table 4.4.89. fbj Cluster Parameters for Galaxy Cluster S9.

Using the cluster center as determined by the dispersion elhpse analysis, we count 331 galaxies within 20 rings of width 2.0 arcminutes and to the limiting mag­ nitude = 19.0. This widely scattered aggregate of galaxies forms a loose cluster with few dense concentrations. The strip counts show considerable scatter espe­ cially along the North-South ordinate where we do see slight density enhancements both North and South of cluster center. The quadrant counts reveal concentrations in the third and in particular in the first quadrants. The cluster surface density distribution shows a sharp drop within the slow rise in density directed radially from the cluster center. This radical drop located at ring 6 greatly contributes to the inability of the isothermal model to describe this cluster.

Although the isothermal fit manages to describe some of the obsen'ations, it has great difficulty modeling the cluster as a whole. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotherm al Analysis 423 §4.4 GALAXY CLUSTER 040 22 01 07 - 5 0 18

CLUSTER RING C0UNTS : EAST NBRTH WEST =

2 0 MIN =

i l - i A v

S0ÜTH

CLUSTER STRIP [BUNTS EAST m n N0FTM u s IC S T ~ CLUSTER SURFACE DENSITY B IN S ”

f i E i

s M U .U S NUmEA (2 RRCHIN WIDTH)

ERST M « S8UTH Figure 4.4.40. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 424 §4.4

GALAXY CLUSTER 040 22 01 07 -5 0 IB

RING TBTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) LOGIDEN)

NUMBER CBUNT NW NE SE SU RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 4 0 1 0 3 1.259 1446.01 O.lODDl 3 .16D17

2 14 3 1 3 7 2.815 1687.01 0.44949 3.22712

3 9 3 1 2 3 4.539 650.70 0.65698 2.81338

4 11 2 4 1 4 6.295 568.07 0.79898 2.75440

5 9 1 3 1 4 8.061 361.50 0.9DB4D 2.55811

6 13 5 0 4 4 9.833 427.23 0.99267 2.63066

7 9 2 2 4 1 11.607 250.27 1.06472 2.39841

8 10 1 4 3 2 13.383 241.00 1.12GS5 2.38202

S 12 3 2 2 5 15.160 255.18 1.18069 2.40684

10 13 3 1 2 7 16.937 247.34 1.22885 2.39330

11 16 4 5 4 3 18.716 275.43 1.27220 2.44001

12 12 3 3 2 4 20.494 188.61 1.31163 2.27556

13 19 3 10 3 3 22.273 274.74 1.34778 2.43892

14 41 9 20 8 4 24.052 548.95 1.38115 2.73953

15 10 3 2 3 2 25.831 124.66 1.41215 2.09571

16 24 10 7 4 3 27.611 279.87 1.44108 2.44696

17 IB 5 3 5 5 29.390 197.18 1.46820 2.29487

IB 23 3 3 8 9 31.170 237.56 1.49374 2.37577

19 14 6 0 3 5 32.950 136.78 1.51785 2. 13604

20 3 0 0 0 3 34.730 27.81 1.54070 1. 44417

TBTAL NUMBER BF GALAXIES CflUNTEO = 284 MAGNITUDE CUTOFF. MV = 19.0 CLUSTER CENTER AT XO = -8.125 YO = -14.404

RING HIOTH (ARCMIN) = 2.0

Table 4.4.40. ^aj Ring-Count Data for Galaxy Cluster 40. Isothermal Analysis 425 UA

GALAXY CLUSTER 040 22 01 07 -50 18 10' ISOTHERMAL FIT pir) = aq(r//5) + 7

a 10' O o ÜJ c r

cn LU X ΠΠ10^ O

CORE RADIUS: Rc=3iS~ 0.113 Mpc

io ‘ 10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.40. (e) Isothermal Fit for Galaxy Cluster J^O. Isothermal Analysis 426 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 040 22 01 07 - 5 0 18

p(r) - a q(r//S) + y

a - 666.48 ±426.80 /S - 1.05±Q.17 y ■= U .7 2 ± 3 .4 3

p(r) = 1274.42-qCr/l.GS ) + 1 2 . 2 6 •C S7 r i T

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.113 Mpc Z = 0 .0 4 2

Table 4.4.40. fbJ Cluster Parameters for Galaxy Cluster 40.

Using the cluster center as determined by the dispersion ellipse analysis, we count 284 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. The cluster strip counts show fairly wide dispersion in both directions and display the obvious central concentration located marginally South of the cluster center as well as the slight condensation North-East of center. The quadrant counts confirm the observation in particular in the second quadrant where the dominant peak locates the previously mentioned concentration. Similar behavior is seen in the cluster density distribution which displays a virtual plateau near the cluster center and then departs rapidly near the peripheral concentrations.

The non-uniform cluster surface density lessens the ability of the isothermal fit to model the observational data. This is particularly evident in the plateau regions of the distribution. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. isotbennal Analysis 427 §4.4 GALAXY CLUSTER 041 22 19 59 - 5 5 23

CLUSTER RING C0UNTS : ERST — N0RTH u u WEST =

= 2 0 H IN = II Is

E

i II

= = E R S T

CLU3TCR 3TITir C0UNT3

EAST NBRTH ••• ICST =

CLUSTER SURFACE DENSITY II =1 m BINS — E so. I

35.

2 S . B E

= EAST WEST — Figure 4.4.41. Cluster Ring Counts, (h) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surjace Density. Isothermal Analysis 428 §4.4

GALAXY CLUSTER 041 22 19 59 -5 5 23

RING T0THL QUADRANT COUNTS COUNTING OBSERVED LOG (RAD) LBGIOEN)

NUMBER CBUNT NW NE SE SW RADIUS DENSITY (ARCMIN) IGAL/SQOEG)

1 1 0 1 0 0 1.259 361.50 0.10001 2.55811

2 4 0 1 3 0 2.815 482.00 0.44949 2.68305

3 6 1 1 4 0 4.539 433.80 0.65698 2.63729

4 17 0 1 14 2 6.295 877.93 0.79898 2.94346

5 14 3 2 6 3 8.061 562.34 0.90640 2.75000

6 20 3 6 8 3 9.833 657.28 0.99267 2.81775

7 10 0 2 5 3 11.607 278.08 1.06472 2.44417

e 30 7 4 13 6 13.383 723.00 1.12655 2.85914 9 16 0 5 5 6 15.160 340.24 1.18059 2.53178 10 17 3 6 2 6 16.937 323.45 1.22685 2.50931 11 24 8 1 8 7 18.716 413.14 1.27220 2.61610 12 29 6 5 4 14 20.494 455.81 1.31163 2.65878 13 14 1 6 5 2 22.273 202.44 1.34778 2.30630

14 22 7 2 9 4 24.052 294.56 1.38115 2.46917

15 20 5 6 6 3 25.831 249.31 1.41215 2.39674

16 30 13 2 11 4 27.611 349.84 1.44108 2.54387

17 29 9 0 13 7 29.390 317.68 1.46820 2.50199

18 13 5 0 8 0 31.170 134.27 1.49374 2.12799

19 7 3 0 3 1 32.950 68.39 1.51785 1.83501

20 8 4 0 4 0 34.730 74.15 1.54070 1.87014

T0TAL NUMBER BF GALAXIES COUNTED = 348 MAGNITUDE CUT0FF. MV = 19.0

CLUSTER CENTER AT XO = 101.125 YO = -22.117

RING WIDTH 1ARCMIN) = 2.0

Table 4.4.41. (a) Ring-Count Data, Jot Galaxy Glueter 4I. Isotbermaî Analysis 429 §4.4

GALAXY CLUSTER 041 22 19 59 -50 23

ISOTHERMAL FIT pir) = a-q(r//S) + 7

Ü 10 CD UJ Q ÜJ Œ O CO

Q_ cn

X ΠΠ10' CD

CORE RADIUS:

Rc=3jS~ 0.109 Mpc

10° 10' RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.41. (e) Isothermal Fit for Galaxy Cluster ^1. Isotbermaî Analysis 430 §4.4

CLUSTER PARAMETERS ______GALAXY CLUSTER 0 4 1 2 2 19 5 9 - 5 0 2 3 ______

p(r) - oc q(r//S) + y

a - 430.40 ±219.66 /S - 1 .0 5 ± 0 .1 5 y~ 12.35± 3.03

p(r) = 642.22-q(r/1.04 ) + 13.12 ■ D T FIT

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.109 »h-i Mpc Z = 0 .0 4 0

Table 4.4.41. (b) Cluster Parameters for Galaxy Cluster 41-

Using the cluster center as determined by the dispersion ellipse analysis, we count 348 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. The cluster strip counts reveal a slight concentration East of center along the East-West absissa and likewise another somewhat South of center along the North-South ordinate. This corresponds to what is seen as a small group of galaxies South-East of cluster center. The quadrant counts reveal a paucity of galaxies at or near the cluster center noticed in all quadrants, and several peaks which correspoond to the aforementioned group and other enhancements near the cluster periphery. The surface density distribution shows several peaks and valleys and in particular the lack of membership near the center of the cluster.

The isothermal fit seems to model the middle portions of the cluster adequately but runs into difficulty at the cluster center, as we might have anticipated, and at the cluster periphery. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Jsotbermal Analysis 431 §4.4 GALAXY CLUSTER 042 22 21 26 - 5 6 38

CLUSTER RING C0UNTS = = EAST — . NBRTH . . . WEST winHin m iin»iiwin n iiniiim im ii»iifWNH = 2 0 MIN = I: il kaJ • iA « I «(OisKtftta

■.t.iil.imimlmmi. == ERST

CLU3TDT 3TrÇir C0UNT3 ERST ■■■ NBRTH &€ST =

CLUSTER SURFACE DENSITY = 1 MM BINS = s

3 5 . § pT!

II

OMrgm^iPoo)o-"r<4fnvin(cr*‘CCOO = EAST Figure 4.4.42. (a) Cluster Ring Counts, (b) Quadrant Counts, (e) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 432 §4.4

GALAXY CLUSTER 042 22 21 26 -5 6 38

RING TBTAL QUAORANT CBUNTS CBUNTING BBSERVEO LBG(RAO) LBGIOEN)

NUMBER CBUNT NW NE SE SW RAOIUS DENSITY (ARCHINl (GAL/SQDEG)

1 2 0 0 1 1 1.259 723.00 0.10001 2.85914

2 3 2 0 1 0 2.815 361.50 0.44949 2.55811

3 11 6 0 3 2 4.539 795.30 0.65698 2.90053 4 19 3 1 7 8 6.295 981.22 0.79898 2.99177 5 19 2 I 7 9 8.061 763.17 0.90640 2.88262

6 16 1 2 5 8 9.833 525.82 0.99267 2.72084

7 11 2 6 3 0 11.607 305.89 1.06472 2.48556

8 17 3 8 2 4 13.383 409.70 1.12555 2.61247

g 20 5 7 6 2 15.160 425.30 1.18069 2.62869

10 20 3 9 4 4 16.937 380.53 1.22885 2.58039

11 29 2 18 8 1 18.716 499.22 1.27220 2.69829

12 35 1 20 6 8 20.494 550.11 1.31163 2.74045

13 28 4 16 3 5 22.273 404.88 1.34778 2.60733

14 29 6 11 6 6 24.052 388.28 1.38115 2.58914

15 18 9 1 5 3 25.831 224.38 1.41215 2.35098

16 16 10 0 3 3 27.611 186.58 1.44108 2.27087

17 21 6 0 10 5 29.390 230.05 1.46820 2.36182

18 4 1 0 0 3 31.170 41.31 1.49374 1.61610

19 5 1 0 2 2 32.950 48.85 1.51785 1.68883

20 4 0 0 0 4 34.730 37.08 1.54070 1.55911

TBTAL NUMBER BF GALAXIES C0UNTED = 327 MAGNITUDE CUT0FF. MV = 19 0

CLUSTER CENTER AT XO = 87.461 YO = -88.514

RING WIDTH (ARCMIN) = 2.0

Table 4.4.42. (a) Ring-Count Data for Galaxy Cluster ^2. Isotbermaî Analysis 433 §4.4

GALAXY CLUSTER 042 22 21 26 -56 38

ISOTHERMAL FIT p(r) = a-q(r//S) + y

UJ

Œ

cn

c r Π10' o

CORE RADIUS;

Rc=3)S~ 0.116 Mpc

RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.42. {e) Isothermal Fit for Galaxy Cluster J^2. Isothermal Analysis 434 §4.4

CLUSTER PARAMETERS ______GALAXY CLUSTER 042 22 21 26 -56 38

p(r) - a q(r//S) + y

a - 519.80 ±286.90 /S - 1.05±0.1B y ~ 12.11±3.1G

p(r) = 728. 31 -q(r/l .03 ) + 12.42

CORE RADIUS; REDSHIFT; Rc=3/S~ 0.116 M pc Z = 0 .0 4 3

Table 4.4.42. (b) Cluster Parameters for Galaxy Cluster 4S.

Using the cluster center as determined by the dispersion ellipse analysis, we count 327 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. The strip counts quantify what is apparent to the eye: a concentration East of the cluster center along the East-West absissa locates an ap­ parent subcluster North-East of the center of the cluster; likewise, an enhancement to the South of center along the North-South ordinate reveals another concentra­ tion just South of center. The quadrant counts show much the same, especially with the dramatic peak seen in the second quadrant between rings 10 and 12 that corresponds to the subclustering found North-East of the cluster center. The clus­ ter surface density distribution is enhanced by the subclusters to give significantly large and wide peaks in the mapping.

The peaks and valleys of the observed surface density distribution do not allow the isothermal fit to model the data very well. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isothermal Analysis 435 §4.4 GALAXY CLUSTER 043 22 22 36 - 5 6 06

CLUSTER RING CBUNTS : EBST NBRTH NEST = INp t m iH H 111W111 H == 20 MIN =

iniiniiImMUJihuMUiJniynuImniiiüiiiiiiniliinmtJmmmloiminUBU

= = ERST « ■ « S0UTH ■■■ WEST =

ci_u3Tcrr arn rr c b u n t d ERST NBRTH IC S T =

: CLUSTER SURFACE DENSITY = 1 MM BINS := £ 5 0 . 3 I 5 4 5 .

4 0 . S 3 5 . Ç : 3 0 .

2 5 . a I I 2 0 . 1 5 . 1 1 0 .

g 5 .

1 0 . 0 1! BIfAJLUS NUWER 12 RRCMIN WIDTH I

: EBST Figure 4.4.48. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 436 §4.4

GALAXY CLUSTER 093 22 22 36 -5 6 06

ÎING TOTAL OUADRANI■ COUNTS COUNTING OBSERVED LOGIRAO) LOG (DEN) JMBER C0UNT NW NE SE sw RADIUS DENSITY (ARCMINl (GAL/SQOEG)

1 2 0 1 0 1 1.259 723.00 0.10001 2.B59I4

2 15 1 3 8 3 2.815 1807.51 0.44949 3.25708

3 17 3 2 11 1 4.539 1229.10 0.65698 3.08959

4 20 7 3 8 2 6.295 1032.86 0.79898 3.01404 5 19 3 7 7 2 8.061 763.17 0.90640 2.88262

6 30 9 5 7 9 9.833 985.91 0.99267 2.99384

7 33 6 7 12 6 11.607 917.66 1.06472 2.96268

8 28 7 7 6 8 13.383 674.80 1.12655 2.82918

9 32 S 4 13 6 15.160 680.47 1.18069 2.83281

10 30 5 8 10 7 16.937 570.79 1.22885 2.75648

11 34 4 11 12 7 18.716 585.29 1.27220 2.76737

12 30 4 13 7 6 20.494 471.52 1.31163 2.67350

13 17 8 4 0 5 22.273 245.82 1.34778 2.39062

14 6 5 0 0 1 24.052 80.33 1.38115 1.90490

15 0 0 0 0 0 25.831 0.00 1.41215 0.00000

16 0 0 0 0 0 27.611 0.00 1.44108 0.00000

T0TAL NUMBER 0F GALAXIES COUNTED = 313 MAGNITUDE CUT0FF. MV = 19.0

CLUSTER CENTER AT XO = 79.768 YO = -59.436 RING WIDTH (ARCMINl = 2.0

Table 4.4.43. faj Ring-Count Data for Galaxy Cluster J^S. Isothermal Analysis 437 §4.4

GALAXY CLUSTER 043 22 22 36 - 5 6 06

ISOTHERMAL FIT /o(r) = oc-q(r//S) + y

H 10 a o UJ g a c n

CO

c r Π10' o

CORE RADIUS:

Rc=3/S~ 0.117 Mpc

RADIAL DISTANCE (RRCMINUTES)

Figure 4.4.43. (e) Igothermal Fit for Galaxy Cluster Isothermal Analysis 438 §4.4

CLUSTER PARAMETERS ______GALAXY CLUSTER 0 4 3 2 2 2 2 3 6 - 5 6 0 6

p (r) - ex q(r//S) + y

a- 806. 33 ±492.59 /S -• 1. 05±0.16 -y = 11.77±3.12

p(r) = 1541. 59-qCr/l. 04 ) + 12.55

CORE RADIUS: REDSHIFT; Rc=3/S~ 0.117 Mpc Z = 0 .0 4 3

Table 4.4.48. (b) Cluster Parameters for Galaxy Cluster J^S.

Using the cluster center as determined by the dispersion ellipse analysis, we count 313 galaxies within 14 rings of width 2.0 arcminutes and to the limiting mag­ nitude nzv = 19.0. The cluster strip counts reveal several instances of subclustering: The East-West absissa shows a concentration East of center while the North-South ordinate decribes one South of center. These correspond to what we see as a farly strong condensation South South-East of center. The quadrant counts show similar behavior as well as a paucity of cluster members at the center. In addition, the cluster surface density distribution reflects all of the above findings and shows the presence of two wide peaks in the general rise of density radially from the cluster center.

The isothermal fit appears to model the data well with the exception of the lack of contribution to the general density near the cluster center. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the X® minimization procedure. IsotbermaJ Analysis 439 §44 GALAXY CLUSTER 044 22 24 46 - 3 0 51

CLUSTER RING C0UNTS rovn non = = ERST mmm N0RTH u a WEST =

== 20 MIN =

MJ S0ÜTH m aa

CLUSTCr 3TRir C0UNT3

: ERST a * a N0RTH * * a >CST =

CLUSTER SURFACE DENSITY t! B IN S = 5 0 .

4 5 .

4 0 . S 3 5 .

E 3 0 . 2 5 . g : 2 0 . 1 5 .

3 0 .

5 . 0.

II ANNULUS NWEER 12 ARCHIN WIDTH)

0^tM rn«’incor>a3ato«>(^(*^«*m(jor*‘ (D7)a * = ERST >C5T ~ Figure 4.4.44. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 440 §4.4

GALAXY CLUSTER 044 22 24 46 -3 0 51

RING TOTAL QUAORANT COUNTS COUNTING OBSERVED LOG(RAD) LBG(DEN)

NUMBER COUNT NW NE SE SU RADIUS DENSITY

(ARCHIN) (GAL/SQOEG)

1 2 0 1 1 0 1.259 723.00 0.10001 2.85914

2 6 D 3 3 0 2.815 723.00 0.44949 2.85914

3 10 0 4 6 0 4.539 723.00 0.6569B 2.85914

4 15 4 4 G 1 6.295 774.65 0.7989B 2.88910

5 14 5 3 4 2 8.061 562.34 0.90640 2.75000

6 11 1 5 5 0 9.833 361.50 0.99267 2.55811

7 14 4 3 5 2 11.607 3B9.31 1.06472 2.59029

8 7 1 3 3 0 13.383 168.70 1.12655 2.22712

6 12 2 5 3 2 15.150 255.18 1.18069 2.40684

10 17 1 1 4 11 16.937 323.45 1.22885 2.50981

11 9 3 3 0 3 18.716 154.93 1.27220 2.19013

12 13 3 2 3 5 20.494 204.33 1.31163 2.31033

13 31 3 7 13 8 22.273 448.26 1.34778 2.65153

14 10 4 1 3 2 24.052 133.89 1.38115 2.12675

15 22 2 6 6 8 25.831 274.24 1.41215 2.43613

16 13 1 4 6 2 27.611 151.60 1.44108 2.18069

17 11 2 4 0 5 29.390 120.50 1.46820 2.08099

18 6 3 3 0 0 31.170 61.97 1.49374 1.79219

19 3 2 1 0 0 32.950 29.31 1.51785 1.46703

20 0 0 0 0 0 34.730 0.00 1.54070 0.00000

TOTAL NUMBER OF GALAXIES C0UNTEO = 228 MAGNITUDE CUTOFF. MV = 19 0

CLUSTER CENTER AT XO = 143.511 YO = -45.125

RING WIOTH (ARCHIN) = 2.0

Table 4.4.44. {aj Einff-Count Data for Galaxy Cluster Isotbermal Analysis 441 §4.4

GALAXY CLUSTER 044 22 24 46 - 3 0 52 10' ISOTHERMAL FIT yO(r) = a-q(r//S) + 7

Ü 1Q3 § ÜJ Œct: C3 CO

UJ

CO

X (X CDΠ10^

CORE RADIUS;

Rc=3jS- 0.103 Mpc

10' 10° io‘ RADIAL DISTANCE (RRCMINUTES)

Figure 4.4.44. (e) Isothermal Fit for Oalaxy Cluster 44- Isotbermal Analysis 442 § 4 . 4

CLUSTER PARAMETERS GALAXY CLUSTER 0 4 4 22 24 4 6 -3 0 52

p(r) - £x q(r//S) -t- y

a- 476.60 ±266.70 /S - 1.05 ±0.16 y- 11.79±3.24

p(r) = 867. 02-q(r/l .04 ) + 12.52

CORE RADIUS: REDSHIFT: Rc=3/S~ 0 .1 0 3 M pc Z = 0 .0 3 8

Table 4.4.44. fbj Cluster Parameters for Galaxy Cluster ^4-

Using the cluster center as determined by the dispersion ellipse analysis, we count 226 galaxies within 19 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. We notice a slight enhancement along the East-West absissa slightly East of the cluster center and a general large variance along the North- South ordinate. The quadrant counts suggest a paucity of galaxies near the cluster center in particular in the first and fourth quadrants, to the W^est, and a relatively large contribution to the South-East mostly from the third quadrant. The cluster surface density distribution shows a ragged plateau with a large peak located at the cluster periphery near ring 13.

We find the isothermal analysis to adequately model the observ'ations fairly well with perhaps the exception of the region near the center of the cluster and the trough near ring 11. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 443 §4.4 GALAXY CLUSTER 045 23 16 35 - 4 2 22

CLUSTER RING C0UNTS s= ERST M N0RTH w WEST :

== 20 MIN =

fi

£ I ;i

== ERST

CLUSTER STRIP C0UNTS z= ERST w N0RTH — m (CST == CLUSTER SURFACE DENSITY B = I! 5 0 .

4 5 .

4 0 .

3 5 . S E 3 0 . I 2 5 . { 2 0 . 1 5 . nn 10.

5 .

0 . e

t i S0UTH — m Figure 4.4.45. faj Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 444 § 4 . 4

GALAXY CLUSTER 045 23 16 35 -42 22

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) L0GIOEN)

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCHIN) (GAL/SQOEG)

1 5 2 2 0 1 1.259 1807.51 0.10001 3.25708

2 11 3305 2,815 1325.51 0.44949 3 .1 2 2 3 8

3 14 4 2 2 6 4 .5 3 9 1012.20 0.65698 3.00527

4 21 3 11 5 2 6.295 1084.50 0.79898 3 .0 3 5 2 3

5 22 7 7 4 4 8.061 883.67 0.90640 2.94629

6 20 9 5 2 4 9.833 657.28 0.99267 2.8 1 7 7 5

7 17 3 7 3 4 11.607 472.73 1.06472 2.67462

8 23 8 5 3 7 13.383 554.30 1.12655 2.74375

9 13 1 0 7 5 15.160 276.44 1.18069 2 .4 4 1 6 0

10 22 1 10 4 7 16.937 418.58 1.22885 2.62178

11 29 5 4 8 12 18.716 499.22 1.27220 2 .6 9 8 2 9

12 24 4 12 0 8 20.494 377.22 1.31163 2.5 7 6 5 9

13 19 3 6 3 7 22.273 274.74 1.34778 2.43892

14 25 0 14 3 8 24.052 334.72 1.38115 2.52 4 6 9

15 37 5 24 3 5 25.831 461.23 1.41215 2.66391

16 27 5 10 5 7 27.611 314.88 1.44108 2.49811

17 29 2 8 6 13 29.390 317.68 1.46820 2.5 0 1 9 9

18 19 2 8 6 3 31.170 196.24 1.49374 2.29280

19 33 5 8 10 10 32.950 322.42 1.51785 2 .5 0 8 4 2

20 30 9 7 7 7 34.730 278.08 1.54070 2.44 4 1 7

TOTAL NUMBER OF GALAXIES COUNTED = 585 MAGNITUDE CUTOFF, MV = 19.0

CLUSTER CENTER AT XO = 75.547 YO = -126.152

RING WIDTH (ARCHIN) = 2 .0

Table 4.4.45. (a) Ring-Count Data for Galaxy Cluster 45. Isotbermal Analysis 445 §4.4

GALAXY CLUSTER 045 23 16 35 - 4 2 22

ISOTHERMAL FIT p(r) = aq(r//S) + y

UJ g o

c n ΠLDΠ10'

CORE RADIUS: Rc=3iS~ 0.081 Mpc

RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.45. fej Isothermal Fit for Galaxy Cluster 45. Isotbermal Analysis 4 4 6 § 4 . 4

CLUSTER PARAMETERS GALAXY CLUSTER 045 23 16 35 -42 22

p(r) - ot-q(r//S) + y

a - 830. 83 ±538. 15 /S - 1.05±G.17 y~ U . 8 5 ± 3 . 3 3

p ( r ) = 1612.29- q ( r / l .0 3 ) + 12.60

CORE RADIUS: REDSHIFT: Rc=3/3~ 0.081 *h-i Mpc Z = 0 .0 3 0

Table 4.4.45. (b) Cluster Parameters for Galazy Cluster ^5.

Using the cluster center as determined by the dispersion ellipse analysis, we count 401 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. The cluster strip counts show several concentrations: we note one East of the cluster center along the East-West absissa and another to the far West of center corresponding to a subgroup of galaxies located at the South-West periphery of the cluster; likewise, we see several concentrations along the North- South ordinate. These features are also found in the quadrant counts in particular, for example, at the large peak seen in the second quadrant. The cluster surface density shows a gradual, albeit ragged, rise in density radially outward from the cluster center.

The isothermal fit appears to model the observational data rather well with the possible exception of the region near the cluster periphery where some of the more concentrated subclustering is found. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Aaalysis 447 GALAXY CLUSTER 046 23 27 36 - 3 9 36

CLUSTER RING C0ÜNTS : e a s t m m N0RTH WEST = . = 2 0 M IN = II I

:

I II A N h E fiS T S 8U T H ' WEST =

C C U S T C fT O T H t r C 0 U N T ? = ERST tM N0RTN «u NEST =

CLUSTER SURFACE DENSITY

g 5 0 .

I 3 ( 5 . «.

3 5 . 5

I S 3 0 . I I E 20.

1 5 . 10.

5 . I 0. II RWU.US NUWER 12 PRCMIN NIDTHl

= ERST 3HJTH 1 tC S T = Figure 4.4.46. faJ Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 448 §4.4

GALAXY CLUSTER 046 23 27 36 -39 36

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOGIRAD) LOG IDEN)

JMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMINl (GAL/SQOEG)

1 7 1 3 G 3 1.259 2530.51 0.10001 3.40321

2 8 3 2 2 1 2 .815 964.00 0.44949 2.98408

3 12 0 2 5 5 4.539 867.60 0.65698 2.93832

4 10 3 2 0 5 6.295 516.43 0.79898 2.71301

5 14 2 4 5 3 8.061 562.34 0.90640 2 .75000

6 14 2 6 3 3 9.833 460.09 0.99267 2.66285

7 17 9 4 1 3 11.607 472.73 1.06472 2.67462

6 15 4 3 5 3 13.383 361.50 1.12655 2.55811

9 16 5 4 2 5 15.160 340.24 1.18069 2.53178

10 12 1 5 3 3 16.937 228.32 1.22885 2.35854

11 4 2 1 0 1 18.716 68.86 1.27220 1.83795

12 5 0 3 2 0 20.494 78.59 1.31163 1.89535

13 0 0 0 0 0 22.273 0.00 1.34778 0.00000

14 0 0 0 0 0 24.052 0.00 1.38115 0.00000

TOTAL NUMBER OF GALAXIES COUNTED = 134 MAGNITUDE CUTOFF. MV = 19.0

CLUSTER CENTER AT XO = -3 4 .3 5 8 YO = 24.253

RING mOTH I ARCMINl = 2 .0

Table 4.4.46. (a) Ring-Count Data for Galaxy Cluster Isotbermal Analysis 449 §4.4

GALAXY CLUSTER 046 23 27 36 - 3 9 37 10 ISOTHERMAL FIT pCr) = a-q(r/^) + y

a 10' O oUJ OfUJ CE O CO

a.UJ cn

X CE CDΠ10'

CORE RADIUS: Rc=3;S~ 0.132 Mpc

10' 10° 10 ' RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.46. (e) hothermal Fit for Galaxy Cluster 46. Isotbermal Analysis 450 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 0 4 6 2 3 2 7 3 6 - 3 9 37

p(r) - a-q(r//S) + y

a - 779.97 ±492.73 /S - 1.05 ±0.18 y - 11.63±3.54

y O (r) = 149^. 8 6 -qCr/1. 03 ) + 11.96 « C 3 7 r i T *

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.132 Mpc Z = 0 .0 4 9

Table 4.4.46. (b) Cluster Parameters for Oalaxy Cluster

Using the cluster center as determined by the dispersion ellipse analysis, we count 134 galaxies within 12 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. We find the strip counts somewhat concentrated East of cluster center along the East-West absissa as well as South of center along the North-South ordinate where we appear to have several concentrations of galaxies. Likewise the quadrant counts tend to have their peaks at locations where there is a local excess of galaxies. Finally, the cluster surface density shows a gradual rise in population with increasing radial distance away from center reaching a maximum near ring 7 after which it tapers off.

The isothermal fit is severely effected by the high central density calculated for this cluster which is well over twice as great as that in the adjacent annulus. As a result the fit rides higher above the observations then one might want in order to provide an acceptable model. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. IsotbermaJ Analysis 451 §4.4 GALAXY CLUSTER 047 23 34 24 - 6 9 34

CLUSTER RING C0UNTS = ERST tm m N0RTH ■■■ WEST =

= 20 MIN =

:

I

i X :

== EAST

CI_U3TCF\ 3 T m r CBUNT3 ; EAST N0RTH «S T =

w CLUSTER SURFACE DENSITY I BINS

95. S

I 25. g Î i i

II BNNULUS NUMBER 12 RRCMIN WIDTH)

o«MC4n«'i/>co9>o = ERST « StUTH KST = Figure 4.4.47. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 452 §4.4

GALAXY CLUSTER 047 23 34 24 -69 34

RING T0TAL OUADRANI C0UNTS C0UNTING 0BSERVED L0GtRAD) L0GIDEN)

JMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMINl (GAL/SQDEGl

1 2 0 0 1 1 1.259 72 3 .0 0 O.lOODl 2.85914

2 3 1011 2.815 361.50 0.44949 2.55811

3 10 3 3 2 2 4 .5 3 9 7 2 3 .0 0 0.65698 2.85914

4 B 1 3 0 4 6.295 413.14 0.79898 2.61610

5 10 1 2 2 5 8.061 4 01.67 0.90640 2.60387

6 16 0 7 8 1 9 .8 3 3 5 2 5 .8 2 0.99267 2.72084

7 15 2 6 3 4 11.607 417.12 1.06472 2.62026

e 15 4 5 5 1 13.383 361.50 1.12655 2.55811

9 19 4 6 2 7 15.160 40 4 .0 3 1.18069 2.60641

10 14 5 2 5 2 16.937 266.37 1.22885 2.42548

11 22 6 3 8 5 18.716 378.72 1.27220 2.57831

12 11 4 0 4 3 20.494 172.89 1.31163 2.23778

13 3 0 0 2 1 22.273 43.38 1.34778 1.63729

14 1 0 0 1 0 24.052 13.39 1.38115 1.12675

15 0 0 0 0 0 25.831 0.00 1.41215 0.00000

16 0 0 0 0 0 27.611 0.00 1.44108 0.00000

TOTAL NUMBER 0F GALAXIES C0UNTED = 149 MAGNITUDE CUTOFF, MV = 19.0

CLUSTER CENTER AT XO = -3 8.221 YO = 25.705

RING WIDTH (ARCHIN) = 2 .0

Table 4.4.47. faj Ring-Gount Data for Galazy Cluster 47. Isothermal Analysis 453 §4.4

GALAXY CLUSTER 047 23 34 24 -6 9 35 10' ISOTHERMAL FIT pir) = oc-q(r//S) + y

û:LU ce Q en

X o

CORE RADIUS; Rc=3jS~ 0.155 *h ^ Mpc

10° 10' RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.47. (e) Isothermal Fit for Galaxy Cluster ^7. Isotbermal Analysis 454 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 0 4 7 2 3 3 4 2 4 - 6 9 3 5

pCr) - a q(r//S) + y

a 408.53±214.93 /S - 1.05±0.16 -y - 11.80±3.20

p(r) = 730.15-qCr/l.04 ) + 12.59 «ES: r n

CORE RADIUS: REDSHIFT; Rc=3/S~ 0.155 Mpc Z = 0 .0 5 7

Table 4.4.47. ('fty Cluster Parameters for Galaxy Cluster fT.

Using the cluster center as determined by the dispersion ellipse analysis, we count 149 galaxies within 13 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. The cluster strip counts display a slight enhancement of numbers of galaxies to the East of cluster center along the East-West absissa. The North-South ordinate shows a large variance and a high centrally located concen­ tration. The quadrant counts reveal a relatively low central density and several regions of higher density indicating a low level of subclustering. The cluster surface density shows a steady growth radially from cluster center but with several peaks and troughs in the data.

The isothermal fit appears pulled down by the low surface density and as a result fails to model well the tail of the distribution. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isotbermal Analysis 455 §4.4 GALAXY CLUSTER 048 23 38 42 - 3 0 30

CLUSTER RING C0UNTS = ERST m u N0RTH mmm WEST =

K 20 MIN = I 3

I

= - ERST S0OTH

CLUSTER STRIP C0UNT5 : ERST n a N0RTH mmm (CST ==

CLUSTER SURFACE DENSITY D = J BINS = I S

I 1

K

= : ERST mmm SOUTH mmm Figure 4.4.48. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isothermal Analysis 456 §4.4

GALAXY CLUSTER 048 23 38 42 -30 30

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RADI L0G1OENJ

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMINl (GAL/SODEGl

1 1 0 0 0 1 1.259 351.50 0.10001 2.55811

2 6 1 5 0 0 2 .8 1 5 7 2 3 .0 0 0.44949 2.85914

3 4 0 1 3 0 4.539 289.20 0.55698 2.46120

4 10 3 2 0 5 6.295 515.43 0.79898 2.71301

5 19 4 6 3 6 8.061 7 5 3.17 0.90840 2.88282

6 13 0 6 7 0 9.833 427.23 0.99267 2.63085

7 21 5 10 0 6 11.607 583.96 1.06472 2.76539

8 19 2 6 6 5 13.383 457.90 1.12855 2.56077

9 17 4 3 5 5 15.150 361.50 1.18059 2.55811

10 18 2 2 11 3 15.937 342.48 1.22885 2.53463

11 11 3 0 5 3 18.716 189.36 1.27220 2.27728

12 15 7 1 5 2 20.494 2 3 5 .7 5 1.31163 2.37247

13 10 6 1 2 1 22.273 144.50 1.34778 2.16017

14 22 12 2 4 4 24.052 294.55 1.38115 2.46917

15 13 2 7 3 1 25.831 152.05 1.41215 2.20956

15 11 1 3 3 4 27.611 128.27 1.44108 2.10814

17 12 2 2 3 5 29.390 131.45 1.46820 2.11878

18 12 4 3 2 3 31.170 123.94 1.49374 2.09322

19 9 1 2 1 5 32.950 8 7 .93 1.51785 1.94415

20 6 3 1 1 1 34.730 55.62 1.54070 1.74520

TOTAL NUMBER OF GALAXIES COUNTED = 249 MAGNITUDE CUTOFF. MV = 19 0

CLUSTER CENTER AT XO = 88.526 YD = -26.589

RING WIOTH (ARCMINl = 2 .0

Table 4.4.48. (a) Ring-Count Data for Galaxy Cluster 48. Isotbermal Analysis 457 §4.4

GALAXY CLUSTER 048 23 38 42 - 3 0 30 10’ 1------P ■“ !------n r“PT' I I I I I I T"l I I I I I I l TT“ ISOTHERMAL FIT p(.r) = o(-q(r//S) + y

ü 10^ o

g g cn o r g cn

X cr g 10^ c n \

CORE RADIUS:

Rc=3/?~ 0.119 Mpc

I - I - I 11111

10 10“ 10* 10^ RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.48. (e) Isothermal Fit for Galaxy Cluster 48. Isotbermal Analysis 458 §4.4

CLUSTER PARAMETERS ______GALAXY CLUSTER 0 4 8 2 3 3 8 42 - 3 0 3 0

p(r) - a q(r//S) + y

a - 408.86±207.68 /S - 1.05±0.15 y ~ 1 2 . 1 2 ± 3 . G 7

p(T') = 529.94 *q(r/l. 03 ) + 12.29

CORE RADIUS: REDSHIFT: Rc=3yS~ 0.119 Mpc Z = 0 .0 4 4

Table 4.4.48. (b) Cluster Parameters for Galaxy Cluster f 8 .

Using the cluster center as determined by the dispersion ellipse analysis, we count 249 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude m„ = 19.0. The cluster strip counts display several concentrations: along the East-West absissa we see and Eastward enchancement of galaxy counts; likewise several significant peaks are present in the North-South counts along the ordinate where we find a central concentration dominating the distribution. It is in these locations where we find instances of subclustering. The quadrant counts show a very low central density and several peaks confirming the presence and location of small groups of galaxies. The cluster surface density rises and falls raggedly with increasing distance from the center of the cluster.

The isothermal fit appears somewhat dragged down due to the paucity of galax­ ies in ring 3 and hence poorly models the observed surface density distribution. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the x® minimization procedure. Isotbermal Analysis 459 §4.4 GALAXY CLUSTER 049 23 44 55 - 2 8 24

CLUSTEB RING.COUNTS : ERST NEST If

SK ' J y i

>««asuMaaB iiaitiouMitiss

= EAST CLUSTER,^%^I^0UNT5

= 1 MM B IN S = CLUSTER SURFACE DENSITY

5

2 5 . @

i

I g

— EfiST u < S0UTH » i WEST == Figure 4.4.49. faj Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotbermal Analysis 460 §4.4

GALAXY CLUSTER 099 23 99 55 -28 29

RING T0TAL QUADRANT C0UNTS COUNTING OBSERVED L0G(RAD) LBGIOEN)

NUMBER C0UNT NW NE SE SW RADIUS DENSITY

(ARCMINl (GAL/SQOEGI

1 14 6 3 2 3 1.259 5061.02 0.10001 3.70929

2 15 4 3 5 3 2.815 1807.51 0.99999 3.25708

3 19 8 2 4 5 4 .5 3 9 1373.71 0.65698 3.13789

4 23 8 5 7 3 6 .2 9 5 1187.79 0.79898 3.07979

5 19 7 9 3 5 8.061 763.17 0.90690 2.85ZÔ2

6 29 6 7 6 10 9.833 953.05 0.99267 2.97912

7 32 9 5 7 11 11.607 889.85 1.06972 2.99932

8 92 21 8 7 8 13.383 1012.20 1.12655 3.00527

9 30 10 5 7 8 15.160 637.99 1.18069 2.80978

10 23 8 2 9 11 16.937 937.61 1.22885 2.64108

11 96 10 9 15 17 18.716 791.86 1.27220 2.89865

12 34 9 9 6 10 20.999 539.39 1.31163 2.72786

13 30 6 7 11 6 22.273 933.80 1.39778 2.63729

19 29 13 8 9 4 29.052 388.28 1.38115 2.58919

15 32 16 2 6 8 25.831 398.90 1.91215 2.60086

16 45 15 13 10 7 27.611 529.76 1.99108 2.71996

17 33 15 7 9 7 29.390 361.50 1.96820 2.55811

18 28 8 6 8 6 31.170 289.20 1.99379 2.96120

19 43 6 12 19 11 32.950 920.12 1.51785 2.62338

20 29 7 8 9 5 39.730 268.81 1.59070 2.92999

T0TAL NUMBER 0F GALAXIES C0UNTED = 1190 MAGNITUDE CUT0FF. MV = 19.0

CLUSTER CENTER AT XO = 15.979 YO = 85.995

RING WIDTH (ARCMINl = 2 .0

Table 4.4.49. (a) Ring-Count Data for Galazy Cluster 49. Isothermal Analysis 461 §4.4

GALAXY CLUSTER 049 23 44 55 - 2 8 25 10' ISOTHERMAL FIT p(r) = aq(r//S) + 7

a 10^ U OLU LU g

en LU cr CJ

CORE RADIUS:

Rc=3)S~ 0.062 *h ^ Mpc

io‘ 10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.49. fej Isothermal Fit for Galaxy Cluster ^9. Isothermal Analysis 462 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 049 23 44 55 -28 25

p(r) - a q(r//S) + y

a - 2283.79 ±442.64 /S - 1.02 ±0.00 y - 11.89±G.38

p(r) = 2928.43-qCr/l. 03 ) + 12.44

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.062 Mpc Z = 0 .0 2 3

Table 4.4.49. (b) Cluster Parameters for Galaxy Cluster

Using the cluster center as determined by the dispersion ellipse analysis, we count 595 galaxies within 20 rings of width 2.0 arcminutes and to the limiting mag­ nitude r»v = 19.0. The strip counts for this large and diverse cluster display central concentrations both along the East-West absissa and North-South ordinate as well. This feature is also displayed in the quadrant counts which show a high central density in addition to the presence and location of several instances of subcluster­ ing. The general cluster surface density distribution increases slowly with increasing radial distance and shows numberous peaks and troughs in the observational data.

The isothermal fit appears to model the periphery of the cluster adequately, but fails somewhat in the near-central regions. This may be due to the high central density compared to the surrounding values. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. Isothermal Analysis 463 §4.4 GALAXY CLUSTER 050 23 59 06 - 4 4 07

CLUSTER RING C0UNTS : ERST wmm N0RTM mmm WEST

s= 20 MIN =

: ;

S0UTH WEST =

CLUSTER STRIP C0UNTS EAST N0RTH " ICST =

CLUSTER SURFACE DENSITY : B IN S = 50.

45.

40. 35. S 30. I 25. g i 2 0 . 15. 10. 5 . 0 .

I BNNULUS NUMBER 12 RRCHIN WIDTH)

EAST Figure 4.4.50. (a) Cluster Ring Counts, (b) Quadrant Counts, (c) Cluster Strip-Counts and (d) Cluster Surface Density. Isotberma.1 Analysis 464 §4.4

GALAXY CLUSTER 050 23 59 05 -44 07

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RADI LOG (DENI

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(flRCMIN) (GAL/SQDEG)

1 7 1 0 5 1 1.259 253D.51 0.10001 3.40321

2 9 1 1 1 6 2.815 1084.50 0.44949 3.03523

3 7 2 0 3 2 4 .5 3 9 506.10 0.65698 2.70424

4 18 1 2 G 9 6.295 929.57 0.79898 2.96828

5 21 4 5 3 9 8.061 843.50 0 .90640 2 .92509

6 19 2 1 6 10 9 .8 3 3 624.41 0.99267 2.79547

7 22 3 6 8 5 11.607 611.77 1.06472 2.78659

8 17 2 8 5 2 13.383 409.70 1.12655 2.61247

9 19 1 5 6 7 15.160 404.03 1.18069 2.60641

10 26 4 8 11 3 16.937 494.69 1.22885 2.69433

11 18 4 9 4 1 18.716 309.86 1.27220 2.49116

12 19 1 8 7 3 20.494 298.63 1.31163 2.47514

13 16 4 6 3 3 22.273 231.36 1.34778 2.35429

14 11 3 3 2 3 2 4 .0 5 2 147.28 1.38115 2.16814

15 14 7 1 1 5 25.831 174.52 1.41215 2.2 4 1 8 4

16 36 10 6 8 12 27.611 419.81 1.44108 2.62305

17 28 7 7 7 7 2 9 .3 9 0 306.73 1.46820 2.48575

18 8 2 1 1 4 3 1 .1 7 0 82.63 1.49374 1.91713

19 10 6 0 1 3 32.950 97.70 1.51785 1.98991

20 5 0 0 2 3 34.730 46.35 1.54070 1.66502

T0TPL NUMBER OF GALAXIES COUNTED = 334 MAGNITUDE CUTOFF. MV = 19 0

CLUSTER CENTER AT XO = -1 0 4 .7 9 4 YO = 47.058

RING WIDTH IPRCMIN) = 2 .0

Table 4.4.50. (a) Ring-Count Data for Galaxy Cluster 50. Isothermal Analysis 465 §4.4

GALAXY CLUSTER 050 23 59 06 - 4 4 07 10' ISOTHERMAL FIT pir) = CL-qir/^) + y

Ü 103 O OÜJ

acn

cn

CORE RADIUS; Rc=3jS- 0.103 Mpc

10' 10° RADIAL DISTANCE (ARCMINUTES)

Figure 4.4.50. (e) Isothermal Fit for Galaxy Cluster 50. Isothermal Analysis 466 §4.4

CLUSTER PARAMETERS GALAXY CLUSTER 0 5 0 2 3 5 9 0 6 - 4 4 07

p

a - 831.68 ±553.8<1 /S - 1.05±0.17 y - 11.82±3.43

yO(r) = 1631. 48-qCr/l. 03 ) + 12.47

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.103 Mpc Z = 0 .0 3 8

Table 4.4.50. (b) Cluster Parameters for Galaxy Cluster 50.

Using the cluster center as determined by the dispersion ellipse analysis, we count 330 galaxies within 20 rings of width 2.0 arcminutes and to the limiting mag­ nitude my = 19.0. The cluster strip counts show several instances of subclustering as is evidenced by the wide peaks seen along the East-West absissa, both East and West of center as well as by similar concentrations along the North-South ordinate, in particular South of center. The quadrant counts reveal a low central condensa­ tion but a number of concentrations particularly in quadrants two and three that correspond to small groups of galaxies. The cluster surface density rises quickly ra­ dially away from the center to a rough plateau, sinks and then peaks at the cluster periphery.

The resulting isothermal fit appears to model the observations well with the exception of the trough near ring 3 and the peripheral peak. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit”” determined from the minimization procedure. CHAPTER V

THE ABELL CLUSTERS

But as each revolution of thought has contained some kernel of surviving truth, to we may hope that our present representation of the universe contains something that will last, notwithstanding its faulty expression. - Arthur Stanley Eddington, 1914

In this chapter we provide a condensed version of cluster descriptions and subsequent isothermal analysis of several Abell Clusters found by Abell (1957) in his survery of the distribution of rich clusters of galaxies. The present description serves as an interface between our current work and that which has gone before, not only to restudy previous efforts but to compare and extend the expanding body of information with earlier studies. We trust that these first steps will continue the work of Abell and eventually lead to the large Southern effort that he planned and organized as an all-sky completion of his work carried out in the Northern hemisphere.

467 The Abell Clusters 468 §5.1

5.1 Description and Isothermal Analysis of 5 Abell Clusters

In this section we present a uniform Description and Isothermal Analysis of five Abell clusters of galaxies. Rather than publish the data in numerical form, we choose a graphical and tabular format for ease of comparison between cluster and cluster. The sample is magnitude-limited and uniform to = 19.0. As in the previous cases, we provide a general description of the individual clusters, with relevant commentary, as well as the results of an isothermal analysis performed on each. The Abell Clusters 469 §5.1 GALAXY CLUSTER ABELL 0428 03 13 53 - 1 9 17

SURFACE DENSITY OISTRIBUTI0N •0. CLUSTER MEMBERSHIP AND M0RPH0L0GY

ft. ; u . Ï

17.

e.i E

u .

u . èüîî! X£GENDi B0=E = •♦ : B « * T 6 fi= • i

EAST m S = i ¥ ¥ ? ?

CLUSTER MAGNITUDE DISTRIBUTI0N P0SITI0N ANGLE OISTRIBUTIGN 100.

80.

80. 20. E 19-G 70. 18. K

cwm tot jEnw

S . 80. S

20.

10.

DCTfl (DEGREES) r> r» (c lo tn tn S 8 Figure 5.1.01 (a) Cluster Morphology, (b) Surface Density Distribution, (e) Magnitude Distribution and (d) Position Angle Distribution. The Abell Clusters 470 §5.1

CaW T auSTER RBOL 0128 03 13 S3 -19 I MJIXY [LUSTER «BELL 0128 03 13 S3 -19 I CFLRXT [LUSTER BBELL 0128 03 13 53 -19 I I

3 3

f 4 f * t t t t t f ^

GALAXY CLUSTER ABELL 0 4 2 8 0 3 13 5 3 - 1 9 17

FIELD S47 ES0/SERÛ PLATE J636S

X Y RA DEC L B z n s s o i (19501 119501 (19501 059. 504 039.261 3 13 53.4 -19 17 44.3 003 42 13.2 -55 54 0.7 0.051

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 50 MAJOR AXIS 10.44 SAMPLE POPULATION 130

S0 20 MINOR AXIS 9.84 C0RE POPULATION 46 s 56 ECCENTRICITY 0.33 LIMITING MAGNITUDE 19.0

SB 3 P0SN. ANGLE -0. 17

P 1

Figure 5.1.01 (e,f,g) Cluster Morphological Population Distributions. Table 5.1.01 (a) Cluster Population Description.

Galaxy Cluster Abell 0428: OS IS 5S -19 17. The cluster is located in the North-East quadrant of ESO/SERC Field 547. Within a diameter of 45mm as determined by mio we count 207 galaxies in this cluster and 130 to a limiting magnitude of mum = 19.0. The cluster is classified Abell tj'pe RI because of its near lack of spherical symmetrj' and presence of several concentrations indicating sub clustering.

We count 38 galaxies brighter than Mi) 4- 2 and thus classify the cluster as T ie Abell Clusters 471 §5.1 having an Abell richness of 0. We suggest a B — M type III classification for the cluster which has no dominant galaxies in the field. For m i,m i, and mio we give 14.9, 15.4 and 15.9, respectively. The value of mio implies a redshift of O.OGl.

The cluster appears somewhat elongated and has several noticable concentra­ tions, notably that immediately North of center and that South-West of center, which are the densest and a number of less dense groups scattered throughout mainly the second and third quadrants of the cluster.

The cluster magnitude distribution appears somewhat bifurcated rising slowly from the brightest galaxies to a small peak near = 17.0 then falling to a trough a magnitude later only to rise again to another peak near = 18.5 after which it falls rapidly to the magnitude limit. The position angle distribution is scattered, but suggests an excess in the n u m b ers of bright galaxies oriented West of North.

The elliptical galaxies in the cluster appear to be somewhat more concentrated towards the center of the cluster. The spirals appear to be loosely scattered through­ out the cluster, but also somewhat concentrated in the central regions. We find the {E : SO : 5) ratio to be (i.O : 0.4 : 1.2) indicating nearly twenty percent more spirals in this cluster than ellipticals. The core population comprises nearly 35% of the sample enclosed in 0.11 square degrees. This gives a core surface density of 407 gala>des per square degree on the sky.

We note several pairs of close or superposed pairs of galaxies in this cluster such as the early and late pair of ellipticals at z = 51.9, y = 31.8; and the superposed pair of lenticulars at z = 74.1,y = 44.8. We also point out the presence of an peculiar galaxy with the appearance of an amorphous mass with multiple concentrations located at z = 59.5, y = 36.8. T ie Abell Clusters 472 §5.1 GALAXY CLUSTER ABELL 0428 03 13 53 - 1 9 17

CLUSTER RING C0UNTS r= e r s t » N0RTH mmm WEST :

= 2 D M IN =

| W t= ERST m m S a U T H W EST =

CUUDTCn - OTfT I r C0UNT3 E R S T m m W R T H m m W EST =

CLUSTER SURFACE DENSITY B I N S =

S I : E

Ë 3 11 g

0'**Nn^tf>cot^CDO)0««c4(no*i/)Eor«cocTo : ERST ■» sarTH I t C S T = Figure 5.1.01. fhj Cluster Ring Counts, (i) Quadrant Counts, (i) Cluster Strip-Counts and (k) Cluster Surface Density. T ie Abell Clusters 473 §5.1

GALAXY CLUSTER ABELL 0428 03 13 53 -1 9 17

RING T0TAL QUADRANT C0UNTS C0UNTING 0BSERVED L0G(RRD) L0GIDEN)

NUMBER C0UNT NW NE SE SW RADIUS DENSITY

(ARCMINl IGAL/SQOEGl

1 2 0 1 0 1 1.259 723.00 0.10001 2.83914

2 11 2 5 2 2 2.815 1325.51 0.44949 3.12238

3 11 4 5 1 1 4.539 795.30 0.55698 2.90053

4 8 2 2 0 4 6.295 413.14 0.79898 2.61610

5 6 1 1 0 4 8.061 241.00 0.90640 2.33202

6 13 2 2 5 4 9.633 427.23 0.99267 2.63036

7 10 3 3 2 2 11.607 278.08 1.06472 2.44417

8 10 2 3 4 1 13.383 241.00 1.12655 2.38202

9 11 1 1 5 4 15.160 233.91 1.18069 2.35905

10 10 3 0 2 5 16.937 190.26 1.22885 2.27936

11 17 4 4 5 4 18.716 292.64 1.27220 2.45634

12 13 2 5 5 1 20.494 204.33 1.31163 2.31033

13 3 3 0 0 0 22.273 43.38 1.34778 1.63729

14 4 2 2 0 0 24.052 53.56 1.38115 1.72381

15 1 1 0 0 0 25.831 12.47 1.41215 1.09371

16 0 0 0 0 0 27.611 0.00 1.44108 0.00000

17 0 0 0 0 0 29.390 0.00 1.46520 0.00000

T0TAL NUMBER 0F GALAXIES C0UNTEO = 130 MAGNITUDE CUT0FF. MV = 19 0

CLUSTER CENTER AT XO = -59.504 YO = 39.252

RING WIDTH lARCHINl = 2.0

Table 5.1.01. (b) Ring-Count Data for Abel Cluster O4S8. The Abell Clusters 474 §5.1

GALAXY CLUSTER ABELL 0428 03 13 53 -19 17 10' ISOTHERMAL FIT p(r) = a-q(r/^) + y

in

CO

X

CORE RADIUS;

Rc=3jS~ 0.162 *h ^ Mpc

10° RADIAL DISTANCE (ARCMINUTES)

Figure 5.1.01. (I) Isothermal Fit Jar Abell Cluster 0428. T ie Abell Clusters 475 §5.1

CLUSTER PARAMETERS GALAXY CLUSTER ABELL 0 4 2 8 0 3 13 5 3 - 1 9 17

p(r) - a q(r//S) + y

a - 499. 15 ±289.99 /S - 1.05±0.17 7 - 11.53±3.33

p(r) = 928. 14-qCr/1. 03 ) + 11.94 ■ST FIT '*■

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.162 *h-i Mpc Z = 0 .0 6 0

Table 5.1.01. (c) Cluster Parameters for Abell Cluster 0428.

Using the cluster center as determined by the dispersion ellipse analysis, we count 130 galaxies within 15 rings of width 2.0 arcminutes and to the limiting mag­ nitude = 19.0. The cluster strip counts show several instances of subclustering as is evidenced by the slight enhancement Eastward of center along the East-West absissa as well as North of center along the North-South ordinate. The quad­ rant counts show the lack of central condensation except in the second and fourth quadrants where we see slight galaxy concentrations. The cluster surface density distribution shows an erratic rise and fall of density radially away from the center of the cluster; two peaks are seen, one at ring 6 and the other at ring 11.

The resulting isothermal fit appears to model the observations fairly with the exception of the peak near ring 3. This surface density enhancement seems to bias the fit to higher values along the ordinate. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. T ie Abell Clusters 476 §5.1 GALAXY CLUSTER ABELL 0514 04 45 54 - 2 0 33

SURFACE DENSITY DISTRIBUTI0N CLUSTER MEMBERSHIP AND M0RPH0L0GY to.

II. O e E •1 i #

-II. (

-42.

•44.

EGEND

-7 1 . gO“ ♦

uitiiimiiiliiiminliiiimiiliiimiiilinyiiiiliimuiiliiiMiUiliiimuilii EA S T m 4 C S T lt^888 = S8SSS

CLUSTER MAGNITUDE DISTRIBUTI0N P0SITI0N ANGLE DISTRIBUTION 100.

BO.

80. IS. h 70.

IS.

13. ■" - 12. E - 11. *?- 3 in. S 1 90.

2 0 . to.

0. E - TlCTfi lOEOREESI W JBCNITOg R%GE , 0*0eooeeeeeoeeoooo r- CD to tn in «■ g S P s s Figure 5.1.02 (a) Cluster Morphology, (b) Surface Density Distribution. (c) Magnitude Distribution and (d) Position Angle Distribution. The Abell Clusters 477 §5.1

CfiLfiXY CLUSTER ABELL 0514 M 45 54 -20 3 CALRXT CLUSTER ABELL 0514 04 45 54 -20 3 GALAXY CLUSTER ABELL 0514 04 45 54 -20

i i

GALAXY CLUSTER ABELL 0514 04 45 54 -20 33

FIELD 552 ESa/SERC PLATE JES2S

X Y RA DEC L B z I1950J 119501 (19501 (19501 103.854 -029.613 4 45 5 4.7 -20 33 40.5 219 28 43.9 -35 56 19.1 0. 051

M0RPH0L0GY DISPERSION E L L IP S E CLUSTER MEMBERS

E 101 MAJOR A XIS 10.02 SAMPLE POPULATION 2 7 9

80 32 MINOR A X IS 7 .6 4 CORE POPULATION 102

S 141 ECCENTRICITY 0 .6 5 LIMITING MAGNITUDE 19.0

SB 4 P0SN. ANGLE 25 .7 6

P 1

Figure 5.1.02 (e,f,g) Cluster Morphological Population Distributions. Table 5.1.02 (a) Cluster Population Description.

Galaxy Cluster Abell 0514: 04 45 55 -20 34. The cluster is located in the South-East quadrant of ESO/SERC Field 552. Within a diameter of 45mm as determined by mio we count 329 galaxies in this cluster and 279 to a limiting magnitude of mum = 19.0. The cluster is classified Abell tj'pe RI because of its lack of spherical symmetry and presence of several concentrations indicating sub clustering.

We count 120 galaxies brighter than mj + 2 and thus classify the cluster as The Abell Clusters 478 §5.1 having an Abell richness of 2. We suggest & B — M tj'pe II-III classification for the cluster which has as its brightest galaxies those intermediate in appearance between giant ellipticals and merely normal bright ellipticals. For m i, 1 7 1 3 , and mio we give 13.5,15.3 and 15.5, respectively. The value of mio implies a redshift of 0.051.

The cluster appears quite elongated and has several noticable concentrations, notably that immediately North of center and that South-East of center, which are the densest and a number of less dense groups scattered throughout mainly the third and first quadrants of the cluster, the former being the most dominant. The cluster magnitude distribution appears somewhat bifurcated rising with an almost exponential rise from the brightest galaxies to a large peak near m„ = 16.5 then falling to a trough a magnitude and a half later only to rise rapidly to another peak between m„ = 18.5 and the magnitude limit. This phenomenon may be interpreted as the possible superposition of two clusters. The position angle distribution is scattered, but suggests an excess in the numbers of bright galaxies oriented West of North in particular at the Western pole somewhat aligned with the major axis of the dispersion ellipse.

We note the condensation of elliptical galaxies in the South-East portion of the cluster, near the center. The spirals appear to be loosely scattered throughout the cluster but there appears to be a major concentration of them near the center. We find the (E : SO : S) ratio to be (l.O : 0.3 : 1.4) indicating nearly forty percent more spirals in this cluster than ellipticals. The core population comprises nearly 37% of the sample enclosed in 0.08 square degrees. This gives a core surface density of 1 2 1 0 galaxies per square degree on the sky.

We notice several interesting superpositions in the cluster; even the brightest galaxy in the cluster, located at r = —108.2, p = —26.7, appears to be superposed with a to the North-East. Another pair is seen at z = —124.8, y = The Abell Clusters 479 §5.1

—22.7 consisting of a lenticular and an elliptical and a pair with an early and late elliptical at z = —99.2, y = —29.8. Several barred spiral galaxies are seen with ring-like structures and ”s-shaped” features such as seen at z = —113.6, y = —34.9. T ie Abell Clusters 480 §5.1 GALAXY CLUSTER ABELL 0514 04 45 54 - 2 0 33

CLUSTER RING C0ÜNTS := EBST B H0RTH B NEST =

= 20 MIN = II I

I

II

— EfiST I S0UTH I WEST z=

Ci-uOTCrr o rn ir c b u n t o : EAST B WRTH B ICST =

II II CLUSTER SURFACE DENSITY = 1 Itt BINS = £ 5 0 . «.

4 0 . as. 5 E i 3 0 . s 2 5 . E 2 0 . IS. 10. 5. 0.

II (NtHJlUS NIM EP 12 BRCMIN WIDTH)

0»*f'*ro*"uicDf*-(DCTO — r^f’i«rLntor*'CDOTO EAST ICST = Figure 5.1.02. (h) Cluster Ring Counts, (i) Quadrant Counts, (j) Cluster Strip-Counts and (k) Cluster Surface Density. T ie Abell Clusters 481 §5.1

GALAXY CLUSTER ABELL 0514 04 45 54 -2 0 33

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) LBG(DEN)

JMBER COUNT NW NE SE 5W RADIUS DENSITY

(ARCMINl tGAL/SQDEG)

1 15 5 5 1 4 1.259 5422.52 0.10001 3.73420

2 12 2 7 2 1 2.815 1446.01 0.44949 3.16017

3 26 5 7 10 4 4.539 1879.81 0.65698 3.27411

4 23 4 4 12 3 6.295 1187.79 0.79898 3.07474

5 20 4 4 7 5 8.061 803.34 0.90640 2.90493

6 33 12 5 g 7 9.833 1084.50 0.99267 3.03523

7 33 8 9 8 8 11.607 917.66 1.06472 2.95258

8 34 7 9 13 5 13.383 819.40 1.12655 2.91350

9 19 4 2 4 9 15.160 404.03 1.18069 2.60541

10 23 10 2 8 3 16.937 437.61 1.22885 2.64108

11 22 5 3 11 3 18.716 378.72 1.27220 2.57831

12 7 1 4 2 0 20.494 110.02 1.31163 2.04148

13 7 5 2 0 0 22.273 101.22 1.34778 2.00527

14 4 3 1 0 0 24.052 53.56 1.38115 1.72331

15 1 1 0 0 0 25.831 12.47 1.41215 1.09371

IB 0 0 0 0 0 27.611 0.00 1.44108 0.00000

TOTAL NUMBER OF GALAXIES COUNTED = 279 MAGNITUDE CUTOFF. MV = 19.0

CLUSTER CENTER AT XO = 103.B54 YO = -29.613

RING WIDTH IARCMINl = 2.0

Table 5.1.02. (b) Ring-Count Data for Abel Cluster 0514. T ie Abell Clusters 482 §5.1

GALAXY CLUSTER ABELL 0514 04 45 55 -20 34 10 ISOTHERMAL FIT fi(r) = a-q(r/yS) + 7

X CE

CORE RADIUS:

Rc=3jS~ 0.137 Mpc

10* 1 0 ° RADIAL DISTANCE (ARCMINUTES!

Figure 5.1.02. (I) Isothermal Fit for Abell Cluster 0514. T ie Abell Clusters 483 §5.1

CLUSTER PARAMETERS GALAXY CLUSTER ABELL 0 5 1 4 0 4 4 5 5 5 - 2 0 3 4

p

a - 2677.51 ±277.30 /S - 1 .0 3 ± 0 .0 0 y ~ 1 1 .7 9 ± 0 .1 9

p ir) = 2999.70 -qCr/l .03 ) + 12.01 '■ 0 7 ri7

CORE RADIUS; REDSHIFT; Rc=3/S~ 0.137 Mpc 2 =0.051

Table 5.1.02. (c) Cluster Parameters for Abell Cluster 0514-

Using the cluster center as determined by the dispersion ellipse analysis, we count 279 galaxies within 15 rings of width 2.0 arcminutes and to the limiting mag­ nitude ruv = 19.0. The cluster strip counts show several instances of subclustering as is evidenced by the great enhancement Eastward of center along the East-West absissa as well as South of center along the North-South ordinate. The quadrant counts show a strong contribution from the rhird quadrant at the location of the densest concentration of galaxies in the cluster. As a result, the cluster surafce den­ sity rises quickly as we move radially away from the cluster center. The distibution reaches a peak at Ring 8 and then drops away.

The resulting isothermal fit appears to model the observations poorly due to the excessively large value of the central density. This strongly motivates the fit to higher values along the ordinate forcing it to envelope the observations rather than pass through them. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the x* minimization procedure. T ie Abell Clusters 484 §5.1 GALAXY CLUSTER ABELL 0533 04 58 57 - 2 2 38

CLUSTER MEMBERSHIP AND M0RPH0L0GY SURFACE DENSITY DISTRIBUTION -too.

• t t c .

•uo. i I •ISO.

• I tt.

-I». Ï i f

•IH. 5 0 = - s = *

iC S T ? = ?

CLUSTER MAGNITUDE DISTRIBUTI0N P05ITI0N ANGLE DI5TRIBUTIBN 100. zs.

so.

60.

15. 13. •"

90. 6. S ZO. 10. 'JV

TÆTA (DEGREES) o » o » o o n o u> o D LOL/iLDvvnincNjrj 2 à B R B S B R S 8 S P Figure 5.1.03 (a) Cluster Morphology, (b) Surface Density Distribution, (c) Magnitude Distribution and (d) Position Angle Distribution. T ie Abell Clusters 485 §5.1

CHJ5CY CLUSTER B glL 0533 C« SB 57 -22 3 CPLRXT [LUSTER ABELL 0533 M 58 57 -22 3 CALRXT CLUSTER ABELL 0533 CH 55 57 -22 I I

i

ELLIPTICAL GALAXIES GALAXIES

# * * f * * < * * f ' i t t 'f 4 4 i 4

GALAXY CLUSTER ABELL 0533 04 58 57 -22 38

FIELD 5 5 2 ESO/SERC PLATE J5 B0 S

X Y RA DEC L B z 119501 119501 [19501 (19501 058.668 -141.297 4 SB 57.5 -22 35 55.6 223 5 35.7 -33 45 27.2 0.042

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 13 3 MAJ0R AXIS 14.32 SAMPLE POPULATION 3 2 4

5 0 4 8 MIN0R AXIS 12.61 CORE POPULATION 9 0

S 1 3 3 ECCENTRICITY 0.47 LIMITING MAGNITUDE 19.0

SB 7 P0SN. ANGLE 5 9 .7 2

P 3

Figure 5.1.OS (e,f,g) Cluster Morphological Population Distributions. Table 5.1.03 (a) Cluster Population Description.

Galaxy Cluster Abell 0533: 04 58 57 -22 38. The cluster is located in the South-East quadrant of ESO/SERC Field 552. Within a diameter of 60mm as determined by mio we count 430 galaxies in this cluster and 324 to a limiting magnitude of mum = 19.0. The cluster is classified Abell tj’pe RI because of its lack of spherical symmetry and presence of several concentrations indicating subclustering.

We count 120 galaxies brighter than + 2 and thus classify the cluster as T ie Abell Clusters 486 §5.1 having an Abell richness of 2. We suggest a. B — M type HI classification for the cluster which has no dominant galaxies that could be considered giant ellipticals or larger. For m i,m s, and mio we give 14.3, 14.4 and 15.1, respectively. The value of mio implies a redshift of 0.042.

The cluster appears somewhat elongated and has several noticable concentra­ tions, notably that immediately East of center and that North-West of center, which are the densest and a number of less dense groups scattered throughout mainly the first and fourth quadrants of the cluster, the former being the most dominant. The cluster magnitude distribution rises gently from the brightest galaxies to a plateau centered at m„ = 16.0 then rises sharply to a set of peaks spanning one and a half magnitudes to the sample limit with a large dip occurring at m„ = 18.0. The position angle distribution is scattered, but with several peaks, the largest run­ ning North-South and another two, almost symmetric to the latter, running East of North and West of North, respectively.

We note the relatively scattered appearance of the distribution of elliptical galaxies, but with concentrations on the first and fouth quadrants. The spirals are likewise distributed, but with the heaviest concentration located in the first quadrant. We find the {E : SO : S) ratio to be (1.0 : 0.4 : l.l) indicating nearly ten percent more spirals in this cluster than ellipticals. The core population comprises nearly 28% of the sample enclosed in 0.20 square degrees. This gives a core surface density of 453 galaxies per square degree on the sky.

We notice several interesting superpositions in the cluster: for instance a bright pair of ellipticals composed of an early and late member are seen at z = 49.8, y = —136.4; and a pair of bright superposed spirals are located at z = 40.7, y = —135.2. This cluster also seems fairly rich in spiral-type galaxies possessing ring-like struc­ tures such as the ones seen at z = 78.7, y = —122.7 and z = 52.4, j/ = —147.6. We T ie Abell Clusters 487 §5.1 also make note of an unusual object, seen edge-on, with what appear to be broken ansae located at z = 74.0, y = —164.1. Several very extended low surface brightness objects are also noticed in the field at z = 39.9, y = —147.9 and z = 37.2, y = —15G.0 and are likely to be foreground galaxies superposed on the cluster. The Abell Clusters 488 §5.1 GALAXY CLUSTER ABELL 0533 04 58 57 - 2 2 38

CLUSTER RING C0ÜNT5 == ERST —' N0RTH na WEST m u i yn iy i iiifyniwfu wyfwww! cz 20 MIN =

ERST ! SOUTH I W EST =

cuuD Tcn OTf^ir c b u n t o EAST ra WRTH «mm (EST

CLUSTER SURFACE DENSITY II =1 m BINS =

95 . 5 E B Ç S 1

II

= EBST Figure 5.1.03. {hj Cluster Ring Counts, (i) Quadrant Counts, (j) Cluster Strip-Counts and (k) Cluster Surface Density. The Abell Clusters 489 §5.1

GALAXY CLUSTER ABELL 0533 04 58 57 -2 2 38

RING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) LOG(DEN)

NUMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 4 0 2 2 0 1.259 1446.01 0.10001 3.16017

2 B 2 5 1 0 2.815 964.00 0.44949 2.98408

3 10 2 3 2 3 4.539 723.00 0.65698 2.85914

4 18 2 8 5 3 6.295 929.57 0.79898 2.96828

5 15 5 6 2 2 8.061 602.50 0.90640 2.77996

6 8 1 3 1 3 9.833 262.91 0.99267 2.41981

7 17 7 2 3 5 11.807 472.73 1.06472 2.67452

8 24 7 6 6 5 13.383 578.40 1.12555 2.76223

9 25 7 8 6 5 15.160 552.88 1.18069 2.74263

10 26 13 5 5 3 16.937 494.69 1.22885 2.69433

11 30 12 6 9 3 18.716 516.43 1.27220 2.71301

12 28 9 6 6 7 20.494 440.09 1.31163 2.64354

13 21 6 2 4 9 22.273 303.66 1.34778 2.48239

14 27 9 6 3 9 24.052 361.50 1.38115 2.55811

15 25 10 2 8 5 25.831 311.64 1.41215 2.49355

16 25 4 5 12 4 27.611 291.53 1.44108 2.45469

17 7 1 2 4 0 29.390 76.68 1.46820 1.85459

IB 5 0 3 2 0 31.170 51.64 1.49374 1.71301

19 0 0 D 0 0 32.950 0.00 1.51785 0.00030

20 0 0 D D 0 34.730 0.00 1.54070 Ü.COOOÜ

TOTAL NUMBER OF GALAXIES COUNTED = 324 MAGNITUDE CUTOFF. MV = 19 0

CLUSTER CENTER AT XO = -59.211 YO = -142.605

RING WIDTH (ARCMIN) = 2.0

Table 5.1.03. (b) Ring-Count Data for Abel Cluster 05SS. The Abell Clusters 490 §5.1

GALAXY CLUSTER ABELL 0533 04 58 57 -2 2 39

ISOTHERMAL FIT p(r) = a-q(r//?) + y

tn

c n

tt oΠ10'

CORE RADIUS; Rc=3)S~0.114 Mpc

RADIAL DISTANCE (HRCMINUTES)

Figure 5.1.03. (I) hothermal Fit Jot Abell Cluster 05SS. T ie Abell Clusters 491 §5.1

CLUSTER PARAMETERS GALAXY CLUSTER ABELL 0 5 3 3 0 4 5 8 5 7 - 2 2 39

p(r) - oc-qCr//S) + y

O - 663.69±413.02 - 1.05±0. 17 y - ll.88i3.34

pCr) = 1259. 85-q(r/l .04 ) + 12.65

CORE RADIUS: REDSHIFT: Rc=3f- 0.114 Mpc Z = 0 .0 4 2

Table 5.1.08. (c) Cluster Parameters for Abell Cluster 05SS.

Using the cluster center as determined by the dispersion ellipse analysis, we count 324 galaxies within 18 rings of width 2.0 arcminutes and to the limiting mag­ nitude mv = 19.0. The cluster strip counts show several instances of subclustering as is evidenced by the peaks found both East and West of center along the East-West absissa as well as those found, particularly South of center, along the North-South ordinant. The quadrant counts show these effects, especially in the first quadrant near Ring 10. The cluster surface densitj’ shows a ramp-like rise radially away from center with two troughs in the distribution at Rings 6 and 13.

The resulting isothermal fit appears to model the observations fairly due to the continually high values of the peripheral density. Since the latter appears to be caused by subclustering one might expect a better fit if those concentrations were absent from the distribution. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the x* minimization procedure. Tie Abell Clusters 492 §5.1 GALAXY CLUSTER ABELL 1736 13 24 41 - 2 6 57

CLUSTER HEHB^RShjIP_ AND M0RPH0L0GY SURFACE DENSITY DISTRIBÜTI0N

.>..l;H;Vr:»:4.l.<..4,l 1^1:1 I 4.1.1"' | .'I 1 I IJ I

o X=> ’A ^

• '■> ' • “ IBGEOT) : k E S0= *. 1 ^ : r ^ j g s = * SB—

ERST m HIST

CLUSTER MAGNITUDE DISTRIBUTI0N P05ITI0N ANGLE DI5TRIBUTIBN 100. 300.

60,

BO.

70. 70. I

30.

20. 2 0 . g

10.

0 . THETA IDECREESl tpCNHi^ i/) o m o tf) o neevoBoooeo 07CDor*-r*œcDuiu7ww*Bi»ncNjpg ggP88@R82«2 8 2 5 2 2 Figure 5.1.04 (a) Cluster Morphology, (b) Surface Density Distribution, (c) Magnitude Distribution and (d) Position Angle Distribution. T ie Abell Clusters 493 §5.1

CPLRXY CLUSTER ABELL 1736 13 24 41 -25 3 ■a. CtRXY CLUSTER ABELL II 1736.mw— 13 24 41 -25 3 .m GALAXY ...... CLUSTER ABELL ■■i^i^.i.... 1735 13 24 41 -26 9 I A

# •

R AL G AL AX I S G A L A X IE S S P IR A L G A L A X IE SS0 a e r m l o i

GALAXY CLUSTER ABELL 1736 13 24 41 -26 57

F i a H 509 ES0/SERC P^ATE J23S7

X Y RA DEC L B z I19SSI (19501 (19501 (19501 113.207 -103.482 13 24 40.7 -26 57 22.2 312 42 35.0 34 58 18.9 0.028

MORPHOLOGY DISPERSION ELLIPSE CLUSTER MEMBERS

E 3 0 8 MAJOR AXIS 2 0 .4 7 SAMPLE POPULATION 7 2 5

8 0 90 MINOR AXIS 17.03 CORE POPULATION 297

S 2 8 7 ECCENTRICITY 0.55 LIMITING MAGNITUDE 19.0

SB 2 7 P 0S N . ANGLE 6 1 .2 3

P 14

Figure 5.1.04 (e,f,g) Cltister Morphological Population Distributions. Table 5.1.04 (a) Cluster Population Description.

Galaxy Cluster Abell 1736: 18 24 41 -26 57. The cluster is located in the South-West quadrant of ESO/SERC Field 509. Within a diameter of 90mm as determined by mio we count 886 galaxies in this cluster and 726 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type I because of its lack of spherical symmetrj' and presence of several concentrations indicating subclustering. We do note, however, its high central density of galaxies.

We count 92 galaxies brighter than mj + 2 and thus classify the cluster as T ie Abell Clusters 494 §5.1 having an Abell richness of 2. We suggest a B — M type III classiication for the cluster which has no dominant galaxies that could be considered giant ellipticals or larger, although the brightest galaxy in the field is seen to possess a corona. For nil,m s, and mio we give 13.2,13.5 and 14.3, respectively. The value of mio implies a redshift of 0.028.

The cluster appears somewhat elongated and has several noticable concentra­ tions, notably that immediately North North-West of center and that South-East of center, which are the densest and a number of less dense groups scattered through­ out mainly the first quadrant of the cluster. The most dominant subgroup shows a complicated structure filled with dense groups of galaxies.

The cluster magnitude distribution tends to be somewhat serpentine, rising quickly from the brightest galaxies to about m„ = 17.0 where it tapers oS". The bulk of the population can be found in this region. The position angle distribution is scattered and jagged appearing, but with several peaks, the largest seen running North-South.

We note the relatively scattered appearance of the distribution of elliptical galaxies, and their central concentration with an apparent condensation in the first quadrant. The spirals appear to be more loosely scattered with a slight concentra­ tion in the third quadrant, South-East of center. We find the [E : SO : S) ratio to be (1.0 : 0.3 : 1.1) indicating nearly ten percent more spirals in this cluster than ellipticals. The core population comprises nearly 41% of the sample enclosed in 0.38 square degrees. This gives a core surface density of 774 galaxies per square degree on the sky.

This rich and diverse cluster contains many noteworthy species of galaxies: several are noticed to possess coronae as the object located at x = —103.3, y = T ie Abell Clusters 495 §5.1

—144.1; we notice superposed pairs of galaxies, either ellipticals such as those found at z = —106.6, p = —97.3 or spirals like are seen at z = —115.7, y = —142.3; and we see a very close pair of barred-spiral galaxies at z = —156.257, y = —99.2 and, remarkably, another located at z = —88.4, y = —123.5.

A curious superposed triplet of elliptical galaxies are seen at z = —131.1, y = —75.1. Finally, the peculiars can be typified by the unusual object seen at z = —93.3, y — —94.3. The Abell Clusters 496 §5.1 GALAXY CLUSTER ABELL 1736 13 24 41 - 2 6 57

CLUSTER RING C0UNTS c z e r s t an N 0 R T H m a W EST :

= ZD MIN = II I

5 E

§ z II

== ERST WEST =

CLUSTER STRIP C0UNTS ERST NBRTM a m W EST = = FWinTTTTTTTTTTTTTTTTTnn rrn j II = 1 W BINS = CLUSTER SURFACE DENSITY 5 0 .

4 5 .

4 0 . 35. S E 3 0 . I 2 5 . E 20 . 1 5 . 10.

5 . 0.

II AfMJLUS NUtCER 12 ARCMIN WIDTH)

warm S 0 U T H n « W EST = Figure 5.1.04. (h) Cluster Ring Counts, (i) Quadrant Counts, (j) Cluster Strip-Counts and (k) Cluster Surface Density. The Abell Clusters 497 §5.1

GALAXY CLUSTER ABELL 1736 13 24 41 -26 57

RING T0TAL QUADRANT C0ÜNTS COUNTING OBSERVED LOG(RAO) L(3GlDEt;)

NUMBER C0UNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 8 3 1 1 1 1.259 2159.01 0.10001 3.33626

2 13 2 3 4 4 2.815 1556.51 0.44949 3.19493

3 22 10 4 3 5 4.539 1590.61 0.65698 3.20156

4 37 20 5 5 7 6.295 1910.79 0.79898 3.28121

5 34 11 5 13 5 8.061 1365.67 0.90640 3.13535

6 36 16 7 8 5 9.833 1183.10 0.99267 3.07302

7 31 6 7 11 7 11.607 862.04 1.06472 2.93553

8 39 7 7 16 9 13.383 939.90 1.12655 2.97303

g 32 6 4 15 7 15.160 660.47 1.18069 2.83281

10 35 8 2 17 8 16.937 665.92 1.22885 2.82342

11 22 9 4 2 7 18.716 378.72 1.27220 2.57831

12 30 8 4 6 12 20.494 471.52 1.31163 2.67350

13 32 7 8 9 8 22.273 462.72 1.34778 2.66532

14 24 8 5 4 7 24.052 321.33 1.38115 2.50696

15 28 4 5 9 10 25.831 349.04 1.41215 2.54287

16 22 5 4 9 4 27.611 256.55 1.44108 2.40917

17 26 10 1 4 11 29.390 284.82 1.46320 2.45457

18 43 10 12 17 4 31.170 444.13 1.49374 2.64751

19 31 10 7 6 8 32.950 302.88 1.51785 2.46127

20 23 8 7 7 1 34.730 213.19 1.54070 2.32677

T0TAL NUMBER 0F GALAXIES C0UNTEO = 726 MAGNITUDE CUT0FF. MV = 19.0

CLUSTER CENTER AT XO = 115.661 YO = -101.238

RING WIDTH (ARCMIN) = 2.0

Table 5.1.04. fbj Ring-Gount Data for Abell Cluster 17S6. The Abell Clusters 498 §5.1

GALAXY CLUSTER ABELL 1736 13 24 41 -26 57 10’ “ I I I I— I— I I 1 I n I ; I I III " T 1------1------1----- 1 i 1 1 ISOTHERMAL FIT pir) = a-qir/^) + y

10"

I

CDΠ10'

CORE RADIUS:

Rc=3)S~ 0.076 *h~^ Mpc

10^ I I I— I- 1 I I I 10- 10° 10* 10" RADIAL DISTANCE (ARCMINUTES)

Figure 5.1.04. (I) hothermal Fit for Abell Cluster 17S6. Tie Abell Clusters 499 §5.1

CLUSTER PARAMETERS GALAXY CLUSTER ABELL 1736 13 24 41 -26 57

p(r) - a q(r//S) + y

p(r) = 2239. 85-qCr/l. 04 ) + 12.62 •E 3T FIT

CORE RADIUS; REDSHIFT: Rc=3/S~ 0.076 *h-i Mpc Z = 0.026

Table 5.1.04. (c) Cluster Parameters for Abell Cluster 17S6.

Using the cluster center as determined by the dispersion ellipse analysis, we count 566 galaxies within 20 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. The cluster strip counts show the high central condensation of this cluster as a slight enhancement somewhat North of center along the North- South ordinate. The quadrant counts display the latter with significant peaks in the first and third quadrants. We also find a general rise in counts towards the periphery of the cluster. Thsi is corroborated by the cluster surface density plot which shows a rapid increase in density from cluster center to some maximum region afetr which it gradually tapers oflf to an irregular plateau having an exceptional peak at Ring IS.

The resulting isothermal fit appears to model the observations quite well except for the slight dip near the cluster center at radii 2.8 < r < 4.5 minutes of arc.

The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. T ie Abell Clusters 500 §5.1 GALAXY CLUSTER ABELL 2538 23 06 01 - 2 0 11

SURFACE DENSITY DISTRIBUTI0N CLUSTER MEMBERSHIP AND H0RPH0L0GY R.

M.

tt.

•IS. EH-n

l e g e n d ; E = • ■ BG 0=* i 5 3 = • :

EAST *£ST f ? ? 3 • a-MD

CLUSTER MAGNITUDE DISTRIBUTI0N P05ITI0N ANGLE DISTRIBUTION 100. 2 5 .

9 0 .

6 0 .

7 0 .

1 5 . ctunsrat zcrm 1 3 .

90.

2 0 .

10.

o ^NITUg RWK a««ooaoeeeE T>CTfi lOECREES) eoe 38P88@R82«2gR I ; Figure 5.1.05 faj Cluster Morphology, (b) Surface Density Distribution, (c) Magnitude Distribution and (d) Position Angle Distribution. T ie Abell Clusters 501 §5.1

CnjW T aUSTER flBOL 2538 23 06 01 -20 I CnLRXT aiSTER BBOL 2538 23 06 01 -20 I CBLnXY CLUSTER BBELL 253S 23 05 01 -2 0 I

i i

# * # f ♦ ♦ ♦ T- ♦ - 6 * < Ë 1 f f i S É * i t

GALAXY CLUSTER ABELL 2538 23 06 01 -20 1 1

FIELD EOt ESO/SERC PLR-■E J3B54

X Y RA DEC L 8 Z C1B50) tlBSOI 119501 (19501 0 0 1 . 925 -007.189 23 6 1.6 -20 10 47.3 345 42 35.0 -65 25 2.8 0 .0 5 0

M0RPH0L0GY DISPERSION ELLIPSE CLUSTER MEMBERS

E 107 MAJOR AXIS 9 .6 6 SAMPLE POPULATION 223

30 36 MINOR AXIS 8 .5 4 CORE POPULATION 91

S 82 ECCENTRICITY 0.47 LIMITING MAGNITUDE 1 9 .0

SB 3 P0SN. ANGLE 50.78

P 0

Figure 5.1.05 (ej\g) Cluster Morphological Population Distributions. Table 5.1.05 (a) Cluster Population Description.

Galaxy Cluster Abell 2528: 23 06 01 -20 11. The cluster is located in the South-East quadrant of ESO/SERC Field 604. Within a diameter of 45mm as determined by mio we count 291 galaxies in this cluster and 228 to a limiting magnitude of mum = 19.0. The cluster is classified Abell type R because of its spherical symmetry and high central condensation.

We count 112 galaxies brighter than +2 and thus classify the cluster as having an Abell richness of 2. We suggest a B — M type II-III classification for the The Abell Clusters 502 §5.1 cluster which has as its brightest galaxies those intermediate in appearance between the giant ellipticals and normal bright galaxies.. For m i,m 3 , and mio we give 15.3, 15.5 and 15.8, respectively. The value of mio implies a redshift of 0.060.

The cluster appears highly centrally condensed, with a dense group of galaxies lying just East of the center of the cluster. Another slightly concentrated region is found right at the geometric center of the cluster. Finally, a few subgroups are noticed to the South at the periphery of the cluster.

The cluster magnitude distribution rises gently from the brightest galaxies to a plateau beginning at about m„ = 17.0 and ending at the magnitude limit. The position angle distribution appears skewed in favor of orientations tending West of North with a higher number of measured angles in that region.

We note the central condensation of elliptical galaxies and their paucity in the Southernmost regions of the cluster. The spirals appear to be somewhat centrally condensed with a zone of avoidance in the fourth quadrant. We find the [E : SO :

S) ratio to be (1 . 0 ; 0.3 : 0 .8 ) indicating nearly twenty percent more ellipticals in this cluster than spirals. The core population comprises nearly 40% of the sample enclosed in 0.09 square degrees. This gives a core surface density of 1 0 0 1 galaxies per square degree on the sky.

We find several pairs of galaxies in this cluster: a typical pair consisting of an early and a late elliptical galax}' is seen at z = 2 .6 , y = —26.6; and a pair of spirals at z = —3 .6 , 1/ = -5.6. A curious small group of ellipticals, looking much like a chain, is seen at z = —2.9, y = —6.2. The Abell Clusters 503 §5.1 GALAXY CLUSTER ABELL 2538 23 06 01 - 2 0 11

CLUSTER RING C0UNT5 K ERST tm m N0RTH ■» WEST :

c= 20 MIN =

An Aji/f t « • « e w * # # *

: EBST S0LfTH 1 WEST = ■««h

CLUOTCn OTHir C0UNT3 : EAST m m MRTH mm |CST =

II CLUSTER SURFACE DENSITY I :] m BINS =

! I Ë I s i

ntfWLUS NUtBER 12 ARCMIN WIDTH:

: EAST — « SRJTH — IC ST = Figure 5.1.05. (h) Cluster Ring Counts, (i) Quadrant Counts, (j) Cluster Strip-Counts and (k) Cluster Surface Density. Tie Abell Clusters 504 §5.1

GALAXY CLUSTER ABELL 2538 23 06 01 -2 0 11

TING TOTAL QUADRANT COUNTS COUNTING OBSERVED LOG(RAD) LOG(OEN) JMBER COUNT NW NE SE SW RADIUS DENSITY

(ARCMIN) (GAL/SQDEG)

1 10 6 3 0 1 1.259 3615.01 0.10001 3.55811

2 26 8 5 1 12 2.815 3133.01 0.44949 3.49596

3 28 12 7 5 4 4.539 2024.41 0.65693 3.30630

4 15 7 3 2 3 6.295 774.65 0.79898 2.88910

5 11 2 3 2 4 8.061 441.84 0.90540 2.54526

6 18 8 5 2 3 9.833 591.55 0.99267 2.77199

7 12 5 2 5 0 11.607 333.69 1.05472 2.52335

6 21 7 4 6 4 13.383 506.10 1.12655 2.70424

9 17 8 2 5 2 15.160 361.50 1.18069 2.55811

10 21 3 5 7 6 16.937 399.55 1.22885 2.60158

11 26 5 5 7 9 18.716 447.57 1.27220 2.65086

12 17 4 5 7 1 20.494 267.20 1.31163 2.42683

13 6 5 0 0 1 22.273 86.76 1.34778 1.93832

14 0 0 0 0 0 24.052 0.00 1.38115 0.00020

15 0 0 0 0 0 25.831 0.00 1.41215 0.00000

16 0 0 0 0 0 27.611 0.00 1.44108 0.00000

TOTAL NUMBER OF GALAXIES COUNTED = 228 MAGNITUDE CUTOFF. MV = 19.0

CLUSTER CENTER AT XO = 1.925 YO = -7.190

RING WIDTH IARCMIN) = 2.0

Table 5.1.05. (b) Ring-Count Data for Abel Cluster S5S8. Tie Abell Clusters 505 §5.1

GALAXY CLUSTER ABELL 2538 23 06 02 -20 11

ISOTHERMAL FIT p(r) = «-q(r//S) + 7

I

g

CORE RADIUS:

Rc=3jS~ 0.161 Mpc

10 10° RADIAL DISTANCE (ARCMINUTES)

Figure 5.1.05. (I) Isothermal Fit for Abell Cluster 25S8. The Abell Clusters 506 §5.1

CLUSTER PARAMETERS GALAXY CLUSTER ABELL 2536 23 06 02 -20 11

p(r) - a q(r//S) + y

a - 2115. 07 ±364.82 /S - 1.02±0.00 y - 11.39±0.25

p ( r ) = 2629.08-q(r/l.Q3 ) + 11.74

CORE RADIUS: REDSHIFT: Rc=3/S~ 0.161 Mpc Z = 0 .0 6 0

Table 5.1.05. fcj Cltister Parameters for Abell Cluster 25S8.

Using the cluster center as determined by the dispersion ellipse analysis, we count 228 galaxies within 13 rings of width 2.0 arcminutes and to the limiting magnitude = 19.0. The cluster strip counts show the high central condensation of this cluster as high peaks in both counting distributions. We notice a peak West of center along the East-West absissa as well as a density enhancement North of center at the periphery of the cluster along the North-South ordinate. The quadrant counts indicate the great contribution to the central density by all quadrants save the third; a majority of counts are found in the first. The cluster surface density is low near the center of trhe cluster and bounds rapidly towards a maximum by Ring 3 after which it drops through a ragged u-shaped trough to rise again at the cluster peripherj'.

The extreme high surface density of the central portions of the cluster seem to overwhelm the ability of the isothermal fit to model the observations and we see the fit as an envelope above the middle and peripheral portions of the cluster. The results of the analysis are seen in the table above which gives the calculated value of the cluster parameters and their variance as well as the “best fit” determined from the minimization procedure. C H A P T E R V I

CONCLUSION

But as for certain truth, no man has known it, nor will he know it; neither of the gods, nor yet of all the things of which I speak. A nd if by chance he were to utter the final truth, he would himself not know it; For all is but a woven web of guesses. - Xenophanes

Among the few secure conclusions one may draw from the analysis of the past legs of this journey is that the less one knows about the universe the easier it is to explain. In this respect, the study of the large scale structure of the universe does not differ from any other scientific subject m atter of lesser extent. Still, to the study of the ever-expanding universe, and in particular the study of these aggregates we call clusters of galaxies, we may apply with special appropriateness the saying, “The greater the sphere of our knowledge, the larger is the surface of its contact with the infinity of our ignorance.” The principal reason why this is so is amply documented

507 Conclusion 508 §6.0 in the successive phases of our penetration into the study of the structure of the universe and received its most timely expression at the dedication ceremonies of the Hale telescope in the words of Vannevar Bush: “ It is a great truth of science that every ending is a beginning, that each question answered leads to new problems to solve, that each opportunity grasped and utilized engenders fresh and greater opportunities.”

Indeed, the fresh and greater opportunities offered by our current study afford an embarrassment of riches. Any single aspect or area of concentration of the study of our data poses new problems when scrutinized in detail. Thus, this effort of data acquision and preliminary analysis can only serve as a beginning. In this light we present a catalogue of galaxy clusters and their parameters gleaned from our study.

In Table 6.0.1 we present the pertinent data from the measurement of 50 Bright Southern Clusters of Galaxies. The table includes a cluster identification number. Rectangular Coordinates on the ESO/SERC J plate for the cluster center, the ESO/SERC Field Number, Right Ascension and Declination for the epoch 1950 of the cluster center, redshift, Abell Richness and Type, Bautz-Morgan Classifica­ tion, the number of cluster members to m„ = 19.0 in the sample population and and estimate of the cluster core radius in M pc with h = 0.5. F ig u re 6.0.1 gives the epoch 1950 locations of the clusters on the celestial sphere using a Mollweide projection.

In succeeding sections we will point out particulars of our sample, paying close attention to similarities and differences between the clusters themselves, as well as making general comments on what can be said of clusters of galaxies in general. The latter we do with caution since the very acquistion of our sample is a consequence of the effects of selection. Conclusion 509 §6.0

BRIGHT S0UTHERN CLUSTERS 0F GALAXIES AND THEIR PARAMETERS

N X y FIELD RA DEC Z ABELL B-M POP R

(1950) (1950) R TY TYPE

01 005.543 -070.735 349 00 00 45.,6 -36 19 39.4 0.042 1 R l - I I 330 0. 228 02 035.621 -003.767 349 00 03 13.,9 -35 4 01.6 0.072 2 R II 265 0. 390

03 071.702 -039.543 349 00 06 49. ,1 -35 43 49.9 0.057 2 IR 11-I I I 265 0. 308

04 051.069 -119.610 149 00 07 28.,7 -57 14 52.8 0.044 1 IR I I I 153 0. 238

05 -107.031 024.617 194 00 18 08. ,3 -49 32 34.3 0.050 1 R II 214 0. 262

06 -015.272 094.597 350 00 22 49. ,7 -33 17 33.7 0.038 2 RI II 335 0. 205

07 -005.774 -082.259 196 01 29 33,,8 -51 32 55.7 0.040 0 RI I I I 289 0. 216

08 -043.427 -127.677 297 01 39 50. .0 -42 23 49.0 0.050 1 RI I - I l 214 0. 272

09 087.306 109.669 154 02 55 44..0 -52 56 09.1 0.049 2 III 355 0. 264

10 -103.879 -070.538 302 03 44 04..7 -41 21 11.8 0.050 2 RI 224 0. 268

11 101.219 054.375 302 04 04 04..0 -39 00 28.8 0.042 1 IR II 107 0. 228

12 -115.824 -001.271 253 05 24 00.,3 -45 01 46.1 0.051 0 1 III 115 0. 328

13 -083.921 004.016 087 06 21 39.,4 -64 56 34.9 0.038 0 R II - I I I 163 0. 206

14 -088.653 070.926 161 06 25 02.,5 -53 39 26.8 0.049 2 R I 232 0. 264

15 -076.713 032.793 161 06 26 25.,1 -54 22 29.4 0.048 2 R II 235 0. 260

16 146.553 065.348 442 12 51 41.,2 -28 44 33.4 0.048 2 RI II 348 0. 258

17 -095.233 -121.728 382 13 03 25.,3 -37 17 59.6 0.049 0 R II 181 0. 264

18 005.223 069.735 384 14 00 40.,6 -33 44 13.9 0.020 0 RI I 444 0. 108

19 102.148 117.241 384 14 09 17,.9 -32 50 02.6 0.044 1 I I I I 238 0. 238

20 102.819 053.059 384 14 09 28. ,3 -34 01 38.5 0.038 1 RI II 219 0. 204

21 -043.965 -081.811 447 14 30 26.,3 -31 32 40.5 0.054 0 RI II-III 150 0. 292

22 003.581 080.348 339 19 56 35,,4 -38 32 47.9 0.026 2 I I-II 458 0. .142

23 -105.191 -022.456 401 20 38 34 .4 -35 23 58.1 0.065 1 R I I I 334 0.,355

24 -095.831 -115.415 235 20 48 40,.7 -52 08 45.6 0.037 1 1 I I I 179 0.,200

25 -131.705 018.574 145 21 13 10,.0 -59 36 24.2 0.042 2 I II 271 0.,230

Table 6.0.1 fa.) Catalogue of Southern Galaxy Clusters Conclusion 5 1 0 §6.0

BRIGHT S0UTHERN CLUSTERS 0F GALAXIES AND THEIR PARAMETERS

N X FIELD RA DEC 2 ABELL 8-M POP R (19501 (19501 R TY TYPE

26 -144.719 -0 0 1 . 784 403 21 22 58. 0 -35 00 38. 8 0.052 2 RI I I I 323 0.285 27 -033.381 -057. 179 235 21 25 09 6 -51 04 18. 4 0.048 0 I III 221 0.258 28 -075.807 -019. 961 403 21 29 13 5 -35 22 50. 6 0.044 1 I II 270 0.240 29 -008.471 - lie . 667 145 21 31 14 2 -62 15 40. 3 0.048 2 R I 298 0.260 30 028.755 064. 519 188 21 31 05 9 -53 50 08. 2 0.050 1 I II 182 0.272 31 039.266 123. 490 188 21 32 18 2 -52 44 02. 1 0.044 1 1 III 151 0.238 32 096.553 -093. 917 235 21 41 45 5 -51 43 57. 4 0.043 2 I I-II 197 0.234 33 074.215 134. 600 145 21 42 50 8 -57 29 48. 5 0.042 2 R II 574 0.228 34 -119.835 051. 550 288 21 43 45 1 -44 05 15. 9 0.048 2 I II 384 0.262 35 -107.000 -051.752 288 21 44 40 5 -45 13 32. 3 0.043 2 R II - I I I 354 0.232 36 127.534 102. 014 145 21 50 32 0 -58 03 48. 4 0.050 2 R 11- I I I 295 0.270 37 -098.536 -032.630 145 21 55 17 4 -60 35 13. 4 0.048 2 R I I I 512 0.250 38 -080.549 -010.750 146 21 58 08 7 —60 11 45. 0 0.055 2 R I 312 0.350 39 -063.530 090. 895 146 22 01 11 1 -58 18 36. 8 0.043 1 1 I - I I 331 0.232 40 008.125 -014. 404 237 22 01 05 9 -50 18 11. 9 0.042 0 R I-II 284 0.225 41 -101.125 -022. 117 190 22 19 59 2 -50 23 08. 1 0.040 2 R II-III 348 0.218 42 -087.461 -088. 514 190 22 21 25 9 -56 38 22. 8 0.043 2 III-III 327 0.232 43 -079.768 -059.436 190 22 22 36 0 -56 05 57. 1 0.043 1 I III 313 0.234 44 -143.511 -045. 125 468 22 24 45 3 -30 51 42. 7 0.038 1 RI II 226 0.206 45 -075.547 -126. 152 347 23 16 35 3 -42 22 36. 6 0.030 2 1 III 585 0.162 46 038.794 021. 784 347 23 27 57 5 -39 37 05. 8 0.049 1 I I 134 0.254 47 038.221 025. 705 077 23 34 24 3 -69 34 43. 5 0.057 0 1 III 149 0.310 46 -086.526 -026.689 471 23 38 44 8 -30 30 04. 2 0.044 1 I I 249 0.238 49 -015.479 085. 995 471 23 44 55 4 -28 24 42. 6 0.023 1 R I - I I 1140 0.124 50 104.794 047. 058 292 23 59 05 8 -44 06 46. 5 0.038 0 III 334 0.206

Table 6.0.1 (b.) Catalogue of Southern Galaxy Clusters Conclusion 511 §6.0

CLUSTER LOCATIONS ON THE CELESTIAL SPHERE oh

t l

Figure 6.0.1 Galaxy Cluster Locations on the Celestial Sphere Conclusion 512 §6.1

6.1 Observational Features of Bright Southern Clusters of Galaxies

Of the galaxy clusters in our sample only a third of them can be considered Regular in the Abell sense; that is, having spherical symmetry and being highly centrally condensed. The remainder are either intermediate in class or are desig­ nated irregular. It would appear that, if this sample is typical of galaxy clusters, irregularity is the rule rather than the exception. However, of the 7 galaxy clusters that are unambiguously cD clusters we find 5 to be classed Regular so that, as far as our sample is concerned, the cD phenomenon is related to the symmetry of the cluster.

We note the suggestion of Peach (1969) that the brightest cluster member is formed in a special manner before the formation of the other cluster members. In addition, Tremaine and Richstone (1976) have cited that the statistical variation ff{m i — m 2 ) as compared to <7(mi) is evidence for the first-ranked cluster member’s being a special object. Further, Ostriker and Tremaine (1976) have advanced the idea that the first ranked cluster galaxy grows in luminosity by accretion of other bright cluster members. Now, whether the cD galaxies in these clusters are objects of formation or evolution, the case is clear that these galaxies are remarkable.

From the magnitude distributions of this group we find that the chance of the cD galaxies being a mere statistical fluctuation is negligible. On the other hand, if the giant cD galaxies have grown at the expense of other members of their parent clusters, then indeed they can be considered quite special. A more careful examination of the luminosity functions and morphological distributions may be able to distinguish between these two cases, but for the moment the inescapable conclusion is that the cD galaxies in our sample are “special objects.”

The uniqueness of the cD phenomenon has implications beyond formation or Conclusion 513 §6.1 evolution. The use of cD galaxies as a standard candle has been put forth by sev­ eral authors. For instance, Peebles (1968) has suggested that the apparently small dispersion of M i in his sample is solely due to the steep slope of the luminosity function. Without the construction of either Abell-type or Schechter-type Lumi­ nosity Functions, though, it would be difficult to derive a set of corrections to Mj based on M$, the bright-end turnover, as a standard candle, especially when one considers the unreliability of M* as pointed out by Dressier (1976). In our sample, for those few clusters with cD galaxies the redshift spread ranges from 0.02 to 0.06 while the of the cD galaxies ranges from 11.2 to 15.2. It must be left to future observations and computation of cluster luminosity functions to resolve the matter.

There are other “special” phenomena noticed in our sample. Throughout the clusters we have measured there appear to be galaxies in close proximity, that is, within two galaxy diameters of each other or actually superposed. The curious feature observed is that many of these are observed as pairs or binary systems with a typical combination consisting of an early and a late elliptical galaxy. Often, the earlier companion is seen to be the brighter member of the pair. The usual numbers of these pairs seen in any particular cluster are few but we call attention to the remarkable case of 39 pairs seen in Cluster 49 which represents some 7% of the cluster members. Likewise, Cluster 28 has 15 pairs, or 11% of the sample; and Cluster 23 has 16 pairs, or 9.5% of the cluster members being binary.

In addition, there are several cases of bright elliptical galaxies observed with halos in virtually every cluster. However, some of these are truely unusual in the sense that they are surrounded by a population of many faint attendants as if they were micro-clusters in their own right. Whether we are seeing super massive globular cluster type objects or very small elliptical galaxies imbedded in a giant elliptical galaxy’s halo remains to be seen. A prototypical example of this unusual phenomenon is seen in Cluster 21. Conclusion 514 §6.2

6.2 Cluster Parameters

Abell's Ricbness Parameter: The criterion for estimating the Richness of a cluster of galaxies as developed by Abell (1957) was based on the number of galaxies within a two magnitude interval of the third brightest cluster member. Richness, as defined by Abell, is a parameter that is used quite often as an indication of mass: MviTiai «Richness, or, better, of luminosity MfL

The tacit assumption contained in this definition is that there exists a uni­ versal Luminosity Function. Now a change in the slope of the bright end of the luminosity function from cluster to cluster could add or detract from a cluster’s richness even though its total population would be unchanged. This and the lack of precise photometric measurements to establish such a magnitude interval yield richness determinations that are by-and-large consistent, but occasionally give a poor estimation of the total cluster population. These limitations notwithstanding, we cannot overestimate the value of Abell’s method.

A natural richness criterion could be based on the total number of galaxies counted and complete to some faint limiting magnitude mum- In practice, however, this would be a difficult number to estimate. Nevertheless, the dispersion analysis can yield a useful approach. The Gore population may be able to be used to evaluate a reliable estimate of richness provided the cluster in question is centrally condensed and symmetric. In this case we would be sampling a known fraction of the population (~ 40%) as shown in F igure 6.2.1.

A method that appears to be more in keeping with the variations of cluster luminosity functions is an estimate of the total or core luminosity. This could be converted to mass by virtue of M/L ratios, but due to the many uncertainties in this type of analysis, in particular because of recent observations in the X-ray Conclusion 515 §6.2

Figure 6.2.1 Core Population from Dispersion Ellipse Calculations. regions of the spectrum which yield masses of clusters in excess of that determined by estimates using luminous matter because of intracluster gas, no attempt has been made to do so.

Equipartition: Due to the lack of sufficient time, it is generally believed that the process of equipartition is incomplete in clusters of galaxies. As the process continues, one would expect that the most massive galaxies in a cluster lose energy to the less massive ones, and consequently fall towards the center of the cluster. It would be reasonable to expect, therefore, that the effects of equipartition would be observed by a segregation of mass, or more directly, by luminosity. Oemler (1974) suggested that equipartition has proceeded to the point where it was evidenced by the brightest cluster members. He found that for the average of his data, the brightest two magnitudes of the cluster population were systematically closer to the cluster center than the fainter members.

In order to estimate the degree of equipartition in our sample we applied a zeroth-order approximation by considering the position of the three brightest cluster members from the center of the cluster as determined by the dispersion analysis. We simply determine the mean distance from center of these bright galaxies and for the Conclusion 516 §6.2

55 clusters of our sample their positions are generally less than 5.25 arcminutes from the cluster with

Core Radii: From Table 6.0.1 we find the collected results of our Isothermal Analysis. These results ought to be viewed with caution due to the illness of fit for most of the cluster core radii and their large dispersion. The effects of subclustering and large dips and peaks in the surface density distributions virtually forefit our attempts to model the observed surface densities with a smooth Isothermal model. The core radii so determined are small and are reasonable only inasmuch as we are able to model the very cores of clusters and not their extremities. There are, of course, portions of our surface density distributions that do agree, but since none of the cases fit the Isothermal model within statistical uncertainties, any conclusions drawn must be viewed with suspicion.

We do point out, however, the importance of such an analysis. The structural length, which is one of the parameters determined in the isothermal fitting, has Conclusion 5 1 7 § 6 . 2 been invoked as a standard candle. Bahcall (1975) measured a sample of 15 rich clusters with z < 0.14 and concluded that the core radii determined by isothermal fitting have similar linear values. The mean for the sample was 0.25 Mpc with a dispersion of 0.04 Mpc. This very small dispersion was very encouraging from the cosmological point of view and was the stimulus for determining the core radii for other clusters of galaxies. However, investigations of other authors have brought distrust in the applicability of the core radius as a standard measure. The core radii obtained by Austin and Peach (1974) and Dressier (1973) for some of the clusters in Bahcall’s sample were generally greater than those of Bahcall. The results of Chincarini and Materne (1980) are also at variance with Bahcall’s measures; they find that although the core radius seems to be fairly constant from cluster to cluster, it is doubtful when using the data presently available that we can determine it to an accuracy higher than 0.15 Mpc. Nevertheless, the core radius is a fair standard size for clusters of galaxies. Whether, however, the core radius as determined for a single cluster is an accurate parameter to be used with X-ray observations is uncertain, since the X-ray studies appear to give a more accurate determination of cluster masses. Combined with galaxy counts in a cluster they may allow a better modelling of the cluster potential. We may have to take into account asymmetries as are seen in the surface density distributions in our sample and perhaps find parameters that are less sensitive to the observational uncertainties or better at reflecting the true nature of a cluster of galaxies.

Luminosity Function: The concept of a Universal Luminosity Function is sum­ marized by Schechter (1975) and has found its way into many extragalactic prob­ lems. Abell (1963) proposed that luminosity functions of clusters of galaxies fol­ lowed a universal form and postulated that all clusters show the same characteristic Af* where the luminosity function changes slope. He later suggested (Bautz and Abell, 1973)that this absolute magnitude can be used as a standard candle for cosmological investigations. Conclusion 5 1 8 § 6 . 2

As we have found with the distribution of magnitudes in our survey, other investigators have attempted to derive means to describe the distribution of cluster members as a function of their brightness along the lines of Gaussian or similarly peaked functions (Hubble, 1936). In later studies, though, it became obvious that the luminosity function was more probably a monitonically increasing sequence down to as faint a limiting magnitude that could be observed (Zwicky, 1957).

It was then that Abell introduced the idea of an integrated luminosity func­ tion, that is, an analytic expression for the number of galaxies found with absolute magnitudes between M and M -f 6 M. He proposed the form

n(< M) = Adex{aM); a = 0.75 M < M*

n{< M) = Bdez(^M); ^ = 0.25 M > M* where n(< M) is the number of galaxies per unit volume which are brighter than the absolute magnitude M and the constants A and B must satisfy the continuity condition Adex{aM f) = Bdex{^M ^).

This expression maps as a pair of straight lines on the logN vs. AbsoluteMagnitude diagram. The “break,” or A/*, is defined as the the point where the function sufiTers a change in slope.

The accumulated luminosity function for our sample is given in Figure 6.2.2. and includes all clusters where the hmiting absolute magnitude corresponding to M = 17.5 is fainter or equal to M = —19.0. In this case, we find M , = —21.3.

From this sample it is reasonable to conclude that the luminosity function can serve as a standard candle if it relies on the magnitudes of many galaxies. Conclusion 5 1 9 §&2

LUMINOSITY FUNCTION 4.0

log$ = log$* 4- K1(M—M*) = log$+ + K2(M-M*) MkM*

3.0

sO M* = -2 1 .3

K1 = 1.591 K2 = 0.372

0.0 -2 3 .0 - 22.0 - 21.0 - 20.0 -19.0 - 18.0 ABSOLUTE MAGNITUDE

Figure 6.2.2. Luminosity Function for 55 Bright Southern Clusters of Galaxies. CoDclusion 520 §6.2

In conclusion we are reminded of a sobering fact to be kept in mind. After more than three hundred years of spectacular advances, the evaluation of the scientific cosmology formulated by Salviati, Galileo’s spokesman in the Dialogue, is still valid. Astronomy, Salviati admitted, has not yet arrived “ at such a state that there are not many things still remaining undecided, and perhaps still more which remain unknown.” BIBLIOGRAPHY

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