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Download Date 30/09/2021 18:12:24 GALAXY ANGULAR MOMENTUM Item Type text; Dissertation-Reproduction (electronic) Authors Thompson, Laird Alan, 1947- Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 30/09/2021 18:12:24 Link to Item http://hdl.handle.net/10150/288356 INFORMATION TO USERS This material was produced from a microfilm copy of the original document. While ihs most advanced technological means to photograph and reproduce this document have been used, the quality is heavily dependent upon the quality of the original submitted. The following explanation of techniques is provided to help you understand markings or patterns which may appear on this reproduction. t 1.The sign or "target" for pages apparently lacking from the document photographed is "Missing Page(s)". If it was possible to obtain the missing page(s) or section, they are spliced into the film along with adjacent pages. This may have necessitated cutting thru an image and duplicating adjacent pages to insure you complete continuity. 2. When an image on the film is obliterated with a large round black mark, it is an indication that the photographer suspected that the copy may have moved during exposure and thus cause a blurred image. You will find a good image of the page in the adjacent frame. 3. When a map, drawing or chart, etc., was part of the material being photographed the photographer followed a definite method in "sectioning" the material. It is customary to begin photoing at the upper left hand corner of a large sheet and to continue photoing from left to right in equal*'sections with a small overlap. If necessary, sectioning is continued again — beginning below the first row and continuing on until complete. 4. The majority of users indicate that the textual content is of greatest value, however, a somewhat higher quality reproduction could be made from "photographs" if essential to the understanding of the dissertation. Silver prints of "photographs" may be ordered at additional charge by writing the Order Department, giving the catalog number, title, author and specific pages you wish reproduced. 5. PLEASE NOTE: Some pages may have indistinct print. Filmed as received. Xerox University Microfilms 300 North Ze«b Road Ann Arbor, Michigan 43100 75-14,212 THOMPSON, Laird Alan, 1947- GALAXY ANGULAR MOMENTUM. The University of Arizona, Ph.D., 1974 Astronomy J I Xerox University Microfilms, Ann Arbor, Michigan 4biob THIS DISSERTATION HAS BEEN MICROFILMED EXACTLY AS RECEIVED. GALAXY ANGULAR MOMENTUM by Laird Alan Thompson A Dissertation Submitted to the Faculty of the DEPARTMENT OF ASTRONOMY In Partial Fulfillment of the Requirements For the Degree of DOCTOR OF PHILOSOPHY In the Graduate College THE UNIVERSITY OF ARIZONA 1 9 7 ^ THE UNIVERSITY OF ARIZONA GRADUATE COLLEGE I hereby recommend that this dissertation prepared under my direction by Laird Alan Thompson entitled Galaxy Angular Momentum be accepted as fulfilling the dissertation requirement of the degree of Doctor of Philosophy A/pis </ 79- Dissertation D Date After inspection of the final copy of the dissertation, the follov/ing members of the Final Examination Committee concur in its approval and recommend its acceptance*." d/w ¥- /*-/} -ifI'/4b- Qrl^hWrd /l/ov, S-, Ak./, x-7 , '^V This approval and acceptance is contingent on the candidate's adequate performance and defense of this dissertation at the final oral examination. The inclusion of this sheet bound into the library copy of the dissertation is evidence of satisfactory performance at the final examination. STATEMENT BY AUTHOR This dissertation has been submitted in partial fulfillment of requirements for an advanced degree at The University of Arizona and is deposited in the University Library to be made available to borrowers under the rules of the Library. Brief quotations from this dissertation are allowable without special permission, provided that accurate acknowledgment of source is made. Requests for permission for extended quotation from or reproduc­ tion of this manuscript in whole or in part may be granted by the head of the major department or the Dean of the Graduate College when in his judgment the proposed use of the material is in the interests of scholarship. In all other instances, however, permission must be ob­ tained from the author. SIGNED WJumyMn . ACKNOWLEDGMENTS I am grateful to the following individuals for providing me with some measure of assistance during the course of this dissertation analysis: Dr. H. Arp, Dr. J. Harvey, C. Jewsbury, Dr. P.J.E. Peebles, R. Schiff, and S.P. Worden. I would like to thank the members of my dissertation committee for carefully and critically reading the original version of this work. And I would like to acknowledge Dr. G.O. Abell for originally stimulating my interest in extragalactic astronomy while I was a student at U.C.L.A. and my graduate advisor Dr. W.G. Tifft for his helpful assistance during the course of this dissertation work. iii TABLE OF CONTENTS Page LIST OF ILLUSTRATIONS vi LIST OF TABLES viii ABSTRACT ix CHAPTER I. INTRODUCTION 1 The Nature of Galaxy Angular Momentum 2 Theoretical Investigations into the Origin of Galaxy Angular Momentum 8 Previous Observational Investigations 11 Cluster Approach 1^ Scope of this Project 16 II. OBSERVATIONAL DATA 17 Cluster Sample and Galaxy Sample 17 Measuring Procedures and Accuracy of the Data 20 Data Correction Procedures 2k III. GALAXY ORIENTATION 29 Major Axis Position Angle Data 30 Spiral Winding Data UO IV. GALAXY ELLIPTICITY Uk Morphological Type - Ellipticity Analysis individual Cluster Ellipticity Distributions 52 Ellipticity Distributions for Large and Small Galaxies 55 Morphological Type Separation 58 V. ORIGIN AND EVOLUTION OF GALAXY ANGULAR MOMENTIM 65 Evolution of Galaxy Angular Momentum 65 Galaxy Collapse Process 65 Tidal Interactions 67 Radio Source Ejection 69 iv v TABLE OF CONTENTS—Continued Galaxy Precession 71 Disruptive Collisions 75 General Summary 78 Origin of Galaxy Angular Momentum 79 Tidal Acceleration of Spherical Protogalaxies 80 Formation of Galaxies "by Gravitational Accretion 86 Gravitational Instability of a Protocluster Disk 90 Turbulence Models of Galaxy Formation 93 Turbulence Model of Ozernoi 9^ Turbulence Model of Jones 97 Collapse of Massive Prolate Spheroidal Protoclusters 99 VI. INTERPRETATION AND CONCLUSIONS . 103 Comparison of Observational and Theoretical Results 103 Concluding Remarks Relating Each Theoretical Model to the Observational Results 106 Tidal Acceleration Model . 106 Gravitational Accretion Model 107 Turbulence Models of Ozernoi and Jones 107 Protocluster Disk and Prolate Spheroid Models . 107 Special Properties of A 2197 108 APPENDIX I. OBSERVATIONAL DATA Ill APPENDIX II. DATA CORRECTION PROCEDURES 173 Virgo Cluster Diameter Transfer Relation 173 Holmberg Corrections 175 Apparent to Intrinsic Ellipticity Conversion ...... 179 REFERENCES 182 LIST OF ILLUSTRATIONS Figure Page 1. Position Angle Distributions for Each Cluster 32 2. Position Angle Distribution for Total Sample without A 2197 * * 35 3. Position Angle Distributions for A 2199 37 1*. Position Angle Distributions for Core and Halo Samples of A 2197 39 5. Radial Position Angle Distribution for Cluster A 1656 ... ^1 6. Apparent Ellipticity Distributions for Various Morphological Types ^7 7. Intrinsic Ellipticity Distributions for E, SO, S and Total Sample 50 8. Apparent Ellipticity Distributions for - the Eight Clusters .......... 5^ 9. Apparent Ellipticity Distributions for Large and Small E, SO and S Galaxies 57 10. Line of Sight-Optical Depth Effect 59 11. Intrinsic Ellipticity Distributions for Large and Small SO Galaxies . 60 12. Radial Distribution of Morphological Types 6k 13. Luminosity Map of A -2197 and A 2199 Cluster Area 110 lk. Cluster A 119 • 166 15. Cluster A U00 167 16. Cluster A 1656 (Coma) .......... 168 17. Cluster A 21^7 169 18. Cluster A 2151 (Hercules) 170 vi vil LIST OF ILLUSTRATIONS— Continued Figure Page 19. Cluster A 2197 171 20. Cluster A 2199 172 21. Holmberg ELlipticity Correction 180 LIST OF TABLES Table Page 1. Position Angle Distributions 31 2. Spiral Winding Analysis if3 3. Ellipticity Distribution for Each Morphological Type .... *f5 k. Ellipticity Distributions for Each Cluster Sample 53 5. Diameter Separation of Galaxy Ellipticity 56 6. Radial Distribution of Morphological Types within Clusters ........ 62 7. Summary of Theoretical Models 102 8. Description of the Following Computer Listed Galaxy Data .. 112 9. Basic Cluster Parameters ..... l6l 10. Cluster Centers 162 11. S.A.O. Standard Position Stars 163 12. Galaxy Identification for Virgo Cluster l6k 13. Galaxy Identification for Finder Charts 165 1^. Holmberg Correction Data 176 15. Ellipticity Corrections 178 16. Frequency Distributions for Apparent to Intrinsic Ellipticity Transformation 181 viii ABSTRACT In order to test the theories which purport to explain the origin of galaxy angular momentum, this study presents new data for about 1000 individual galaxies in eight rich clusters. The clusters which are studied include Virgo, A 119, A ^00, A 1656 (Coma), A 2lkff A 2151 (Hercules), A 2197» and A 2199. Selected samples of these data are used to investigate systematic alignment effects in clusters of galaxies and to investigate the intrinsic ellipticities of E, SO, and spiral galaxies. The following new results are reported: 1. Galaxies in the cluster A 2197 show a significant alignment effect probability< 0.0002), and the preferential direction of alignment corresponds approximately to the major axis of the overall cluster elongation. The galaxies in the core of the cluster are less significantly aligned, consistent with a model of slow dynamic reorientation in the dense cluster core. 2. None of the other seven clusters show any significant alignment trends; this includes A 2199, "the cluster for which Rood and Sastry reported a marginal alignment effect (X2 probability » 0.02).
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