Disentangling luminosity, morphology, star formation, stellar mass, and environment in galaxy evolution Item Type text; Dissertation-Reproduction (electronic) Authors Christlein, Daniel 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 16:42:30 Link to Item http://hdl.handle.net/10150/280595 DISENTANGLING LUMINOSITY, MORPHOLOGY, STAR FORMATION, STELLAR MASS, AND ENVIRONMENT IN GALAXY EVOLUTION by Daniel Christlein 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 2004 UMI Number: 3145054 INFORMATION TO USERS The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleed-through, substandard margins, and improper alignment can adversely affect reproduction. In the unlikely event that the author did not send a complete manuscript and there are missing pages, these will be noted. Also, if unauthorized copyright material had to be removed, a note will indicate the deletion. UMI UMI Microform 3145054 Copyright 2004 by ProQuest Information and Learning Company. All rights reserved. This microform edition is protected against unauthorized copying under Title 17, United States Code. ProQuest Information and Learning Company 300 North Zeeb Road P.O. Box 1346 Ann Arbor, Ml 48106-1346 2 The University of Arizona ® Graduate College As members of the Final Examination Committee, we certify that we have read the dissertation prepared by Daniel Christlfiin entitled Disentangling Luminosity. Morphology. Star Formation. Stellar Mass. and Environment in Galaxy Eyolution and recommend that it be accepted as fulfilling the dissertation requirement for the Degree of Doctor of PInilosophy Z nson DanieL-Eisenstein date i I" i~ f/5 date William Tifft Final approval and acceptance of this dissertation is contingent upon the candidate's submission of the final copies of the dissertation to the Graduate College. I hereby certify that I have read this dissertation prepared under my direction and recommend that it be accepted as fulfilling the dissertation requirement. Dks^ktion Director ^ Sate 3 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 Univer­ sity Library to be made available to borrowers under rules of the Library. Brief quotations from this dissertation are allowable without special permis­ sion, provided that accurate acknowledgment of source is made. Requests for permission for extended quotation from or reproduction 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 or her judgment the proposed use of the material is in the interests of scholarship. In all other instances, however, permission must be obtained from the author. SIGNED: 4 ACKNOWLEDGMENTS I would like to thank, first and foremost, my advisor and collaborator in the work presented here, Ann Zabludoff, for her guidance, support, persistence over many a manuscript revision, and her excellent dataset. Ann's work was a ma­ jor motivation for me to come to Arizona, and I have never rued that decision. Further thanks go to Dennis Zaritsky, Dan Eisenstein, Jose Arenas, and Anthony Gonzalez for comments on, discussions about, and contributions to the work pre­ sented here, and especially Luc Simard for his GIM2D code and Dan Mcintosh for his [/-band photometry, both of which are important pillars upon which this work rests. I also gratefully acknowledge financial support from a Graduate Assistantship and a Graduate College Fellowship from the University of Arizona, and from Ann's grants (NSF grant # AST-0206084 and NASA LISA grant # NAG5-11108). Extra thanks to Michelle, Catalina, and Joy for fighting many bureaucratic battles and being persistently victorious. Furthermore, I am particularly grateful to Bill Tifft and Chip Arp for remind­ ing me that reality is not bound by theories and for providing a sense of balance and skepticism throughout my graduate school career. And special thanks are due to Kelly and Amy for their friendship and for helping me maintain vestiges of a life outside the office, Anna for teaching me more about life than I learned from five years of graduate school, and, above all, Wolfgang Amade Mozart for bringing joy and serenity into even the loneliest nightly hour spent before the monitor. DEDICATION This work is dedicated to the memory of Dr. Rainer Christleiri (1940-1983). 6 TABLE OF CONTENTS LIST OF FIGURES 10 LIST OF TABLES 12 ABSTRACT 13 CHAPTER 1 INTRODUCTION 15 CHAPTER 2 GALAXY LUMINOSITY FUNCTIONS FROM DEEP SPECTROSCOPIC SAMPLES OF RICH CLUSTERS 21 2.1 Chapter Summary 21 2.2 Introduction 22 2.3 The Data 25 2.3.1 The Sample 25 2.3.2 Spectroscopy 26 2.3.3 Imaging 29 2.3.4 Image processing 29 2.3.5 Photometry 31 2.3.6 The Galaxy Catalog 34 2.4 Calculating the Luminosity Function 36 2.4.1 The Sampling Fraction 36 2.4.2 The Individual Cluster GLFs 43 2.4.3 The Field and Composite Cluster GLFs 44 2.5 Results and Discussion 47 2.5.1 Individual Cluster GLFs 47 2.5.1.1 Comparisons among Cluster GLFs 48 2.5.1.2 Radial Sampling Bias 53 2.5.1.3 Aperture Bias 54 2.5.1.4 The Uniformity of Cluster GLFs 56 2.5.2 Cluster Composite GLF 57 2.5.3 Field GLFs 60 2.5.4 Comparisons between Field and Clusters 63 2.5.5 The Bright End 71 2.6 Conclusions 73 CHAPTER 3 THE U-BAND GALAXY LUMINOSITY FUNCTION OF NEARBY CLUSTERS 75 3.1 Chapter Summary 75 3.2 Introduction 76 7 TABLE OF CONTENTS — CONTINUED 3.3 The Data 81 3.3.1 The Cluster Sample 81 3.3.2 i?-band Survey 81 3.3.3 f/-band survey 82 3.4 Calculatmg the Luminosity Function 84 3.4.1 A New Method 84 3.4.2 The Sampling Fraction 85 3.4.3 Consistency checks 85 3.4.4 Coverage of {MR, MU, IJLR) Parameter Space 87 3.5 Results and Discussion 89 3.5.1 [/-band GLFs for Individual Clusters 89 3.5.2 Composite [/-band GLFs 92 3.5.3 Comparison to i?-band GLFs 95 3.5.4 Contribution from Clusters and Groups to Near-UV Back­ ground 100 3.6 Conclusions 105 CHAPTER 4 CAN EARLY TYPE GALAXIES EVOLVE FROM FADING THE DISKS OF LATE TYPES? 109 4.1 Chapter Summary 109 4.2 Introduction 109 4.3 The Data 112 4.4 Bulge-Disk Decomposition 113 4.5 Calculating the Bulge and Disk Luminosity Functions 116 4.6 Results and Discussion 117 4.6.1 Bulge-and Disk Luminosity as a Function of Morphology . 117 4.6.2 Bulge- and Disk Luminosity as a Function of Environment . 128 4.7 Conclusions 130 CHAPTER 5 DISENTANGLING MORPHOLOGY, STAR FORMATION, STELLAR MASS, AND ENVIRONMENT 132 5.1 Chapter Summary 132 5.2 Introduction 132 5.3 The Cluster Survey 137 5.4 Galaxy Properties 138 5.4.1 Star Formation Indices 138 5.4.2 Morphologies 139 5.4.3 Luminosities and Stellar Masses 141 5.4.4 Mean Stellar Age 144 8 TABLE OF CONTENTS — CONTINUED 5.5 The Analysis 145 5.5.1 Partial Correlation Coefficients 145 5.5.2 Completeness-Corrected Correlation Coefficients 148 5.5.3 The Discrete Maximum Likelihood Method 150 5.5.4 The Completeness Function 152 5.5.4.1 Spectroscopic Incompleteness 152 5.5.4.2 Morphological Completeness 154 5.5.4.3 Radial Incompleteness 155 5.5.4.4 Summarial Completeness Function 155 5.6 Results 157 5.6.1 Morphology-Environment and Star Formation-Environment Relations 157 5.6.2 Residual Star Formation Versus Environment 159 5.6.2.1 Residual Correlation of Current Star Formation with Environment 161 5.6.2.2 Residual Correlation of Recent Star Formation with Environment 163 5.6.2.3 What is the effect of controlling individual vari­ ables on the star formation gradient? 165 5.6.2.4 Is the residual star formation gradient a major com­ ponent of the total star formation gradient? .... 168 5.6.3 Effect of Errors and Uncertainties on the Residual Correla­ tions 169 5.7 Conclusions 174 CHAPTER 6 CONCLUSIONS 177 APPENDIX A THE I?-BAND PHOTOMETRIC DETECTION CATALOG 183 APPENDIX B CORRECTION OF FOR SELECTION IN A DIFFERENT FILTER BAND 189 APPENDIX C HIGHER-ORDER CORRECTIONS IN CALCULATING THE SAM­ PLING FRACTION 192 APPENDIX D THE DISCRETE MAXIMUM LIKELIHOOD METHOD 194 APPENDIX E DETERMINATION OF THE SAMPLING FRACTION 204 APPENDIX F HOW MUCH LIGHT FROM FAINTER GALAXIES? 209 9 TABLE OF CONTENTS — CONTINUED APPENDIX G HOW MUCH LIGHT FROM LARGER RADII? 215 REFERENCES 217 10 LIST OF FIGURES 2.1 Optical versus HI radial velocities 28 2.2 Averaged Galaxy Sampling Fraction as a function of {rriR-, HR) ... 39 2.3 Cluster GLFs for All Spectral Types 49 2.4 Cluster GLFs for Emission-Line Galaxies 50 2.5 Cluster GLFs for Non-Emission-Line Galaxies 51 2.6 Composite GLFs for Field and Clusters 58 2.7 Error Contours for Schechter Fits 61 2.8 Fraction of Emission-Line Galaxies as a Function of MR 69 3.1 Comparison Between Rest-Frame and Observed Filter Bands .... 78 3.2 Comparison of i?-band GLFs Recovered with Different Methods .