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UNIVERSITY of CALIFORNIA RIVERSIDE Faint Star UNIVERSITY OF CALIFORNIA RIVERSIDE Faint Star-Forming Galaxies at the Peak Epoch of Star Formation: An Application of Strong Gravitational Lensing A Dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in Physics by Anahita Alavi December 2016 Dissertation Committee: Dr. Brian Siana, Chairperson Dr. Bahram Mobasher Dr. Naveen Reddy Copyright by Anahita Alavi 2016 The Dissertation of Anahita Alavi is approved: Committee Chairperson University of California, Riverside Acknowledgements This thesis became a reality with the kind support and help of many individuals. I wish to acknowledge all of them. I would like to express my sincere gratitude to my advisor, Professor Brian Siana, for his patience, motivation and his continuous support throughout my graduate study. He has always supported me not only by providing a research assistantship but also academically and emotionally through the rough road to finish this thesis. He genuinely cares about his students and believes that they can succeed. I was very lucky to work with him and I could not imagine having a better advisor and mentor for my Ph.D. study. Besides, I would like to thank my thesis committee: Prof. Naveen Reddy and Prof. Bahram Mobasher for their insightful comments and questions. In particular, I thank Prof. Reddy for all the discussions that I had with him and his valuable comments about dif- ferent parts of my Ph.D. projects. In addition, I am very grateful to Prof. Mobasher for encouraging me to come to UCR and all his help when I had just started as an international student. I also thank Prof. Gabriela Canalizo for being in my qualifying exam committee and for her constant encouragement throughout my research period. I am grateful to have worked with intellectual and awesome collaborators Johan Richard, Marc Rafelski, Al- berto Dominguez, Brant Robertson, Daniel Stark, Claudia Scarlata, Harry Teplitz, Mathilda Jauzac, and Marceau Limousin. In particular, I praise the enormous amount of help and explaining by Johan throughout these years of collaboration. I am so grateful of my fellow colleagues William Freeman, Najmeh Emami, Kaveh Vasei, Louise Daniels and our new teammate Tim Gburek for their friendship and all the fun that we had during our group meetings. I also thank Ali Ahmad Khostovan and Amanda Pagul for many interesting discussions that we had. I want to thank Dr. Mario De Leo Winkler for all his endeavors for promoting outreach activities in our astronomy group and providing a joyful opportunity for graduate students including me to jointly work with him. A special iv thanks to the Physics department student affairs officer Dr. Derek Beving who was always very helpful whenever I had any question or I needed any paperwork. And to wrap this up, my biggest thanks to Nader, my beloved husband whose love and support has been always with me. Without you, I would not have been able to accomplish my dreams. You are the best and thanks for coming into my life. Last but not the least, my beautiful parents receive my deepest gratitude and love for their dedications and many years of supporting and believing in me. And thank to my brother for all the sweet memories that he has made for me during all past years. This work is partly based on research that has been either published in the Astrophysical Journal (2014ApJ...780...143A) or submitted to (manuscript number: AAS01234). v To Nader for his endless love And to my parents and my grandma for their unconditional supports vi ABSTRACT OF THE DISSERTATION Faint Star-Forming Galaxies at the Peak Epoch of Star Formation: An Application of Strong Gravitational Lensing by Anahita Alavi Doctor of Philosophy, Graduate Program Physics University of California, Riverside, December 2016 Dr. Brian Siana, Chairperson Obtaining a complete census of cosmic star formation requires an understanding of the faint star-forming galaxies that are beyond the detection limits of our current surveys. To find these faint galaxies, we use the power of gravitational lensing from foreground massive galaxy clusters to push the detection limits of the Hubble Space Telescope (HST) to much fainter luminosities. Combining very deep ultraviolet, optical and near-IR imaging from HST, with magnification of strong gravitational lensing from three foreground galaxy clusters, we discover a sample of 780 ultra-faint star-forming galaxies at 1 < z < 3. The UV absolute magnitude of these galaxies are extended down to very faint magnitudes of MUV < 12:5 − AB mag. Using this unprecedented sample, we study the evolution of the UV luminosity function (LF) between 1 < z < 3. We find that the UV LFs are steep with an estimate of faint-end slopes of α = 1:56 0:04, α = 1:72 0:04 and α = 1:94 0:06 at 1:0 < z < 1:6, − ± − ± − ± 1:6 < z < 2:2 and 2:2 < z < 3:0, respectively. We demonstrate that there is no sign of turnover in these UV LFs at least down to MUV = 14. As an important consequence of − steep LFs, we show that the faint star-forming galaxies covered in this study with 18 < − MUV < 12:5, produce a majority (55% 60%) of the unobscured UV luminosity density − − vii at 1 < z < 3. Furthermore, we examine two techniques, fitting a power law to broad-band photometry as well as best-fit SED for each object, to study the evolution of rest-frame UV spectral slopes β for these ultra-faint galaxies. We demonstrate that our UV spectral slopes β change with UV luminosity, such that galaxies become bluer at fainter luminosities. However, we show that the UV spectral slope β MUV correlation is not tight and there is a − large intrinsic scatter in the UV slope distribution at a given MUV . Using hydro-dynamical simulations of dwarf galaxies, we demonstrate that the bursty star formation histories alone can explain the intrinsic scatter in β. viii Contents 1 Introduction 1 1.1 Cosmic Star Formation History . 2 1.2 Why Faint Galaxies Are Important? . 4 1.3 Strong Gravitation Lensing . 6 1.4 Summary of Thesis . 9 2 Ultra-faint Ultraviolet Galaxies at z 2 Behind the Lensing Cluster Abell ∼ 1689 11 2.1 Introduction . 13 2.2 Observations . 16 2.2.1 Data Reduction . 17 2.3 Color Selection and Sample . 19 2.4 Completeness . 23 2.4.1 Simulating the Faint Galaxies . 23 2.4.2 Monte Carlo Simulation : IGM Opacity . 24 2.4.3 Simulation: Incompleteness Correction . 27 2.4.4 F275W Non-detections and CTI . 32 2.5 Luminosity Function . 34 2.5.1 Cosmic Variance . 39 2.6 UV Spectral Slope . 40 2.7 Discussion . 42 ix 2.7.1 Comparison with Other Space Density Measurements at z 2 . 43 ∼ 2.7.2 Evolution of the Faint-End Slope . 44 2.7.3 Evolution of Dust in Faint Star-Forming Galaxies . 44 2.7.4 The Effect of Intracluster Dust . 47 2.7.5 UV Luminosity Density . 48 2.7.6 Star Formation Rate Density . 49 2.8 Summary . 51 3 The Evolution of the Faint End of The UV Luminosity Function at 1 < z < 3 54 3.1 Introduction . 56 3.2 Data . 60 3.2.1 Hubble Frontier Field Observations and Data Reduction . 60 3.2.2 A1689 Observations and Data Reduction . 62 3.3 Object Photometry . 62 3.4 Photometric Redshifts . 64 3.5 Lens Models . 68 3.5.1 HFF Lensing Models . 68 3.5.2 A1689 Lensing Model . 69 3.5.3 Multiply Imaged Systems . 69 3.6 Sample Selection . 70 3.7 Completeness Simulations . 74 3.7.1 The Effective Survey Volume . 79 3.8 Luminosity Function of Photometric Redshift Samples . 81 3.8.1 The Binned UV LFs . 81 3.8.2 The Unbinned Maximum Likelihood Estimator . 84 3.9 Luminosity Function of LBG Samples . 91 3.10 Discussion . 94 x 3.10.1 Comparing the UV LFs of Photometric redshift and LBG Samples . 94 3.10.2 Evolution of the LF Schechter parameters . 94 3.10.3 UV Luminosity Density . 97 3.10.4 No Turnover in the UV LF . 102 3.11 Summary . 102 Appendix . 105 A1 Lyman break Selection . 105 A2 Completeness Simulation for LBG LF . 109 A3 New Multiply Imaged Systems . 111 4 The UV Continuum Slopes of Faint Lensed Star-forming Galaxies 115 4.1 Introduction . 117 4.2 Data and Sample Selection . 119 4.3 UV Spectral Slope . 120 4.3.1 Power Law Fitting . 121 4.3.2 SED Fitting . 121 4.3.3 Comparing the Methods . 122 4.4 Dependence of β on UV Magnitude . 124 4.4.1 Methodology . 125 4.4.2 Compare a Constant and Changing Intrinsic Scatter . 128 4.5 Comparison to the Other Studies . 128 4.6 Dependence of β on Redshift . 131 4.7 Discussion . 135 4.7.1 Bursty Star Formation History in Faint Galaxies . 135 4.7.2 Dust reddening, Metallicity and Future Work . 141 4.8 Summary . 143 References 146 xi List of Figures 1.1 Cosmic star formation history . 2 1.2 UV luminosity function . 4 1.3 Strong gravitational lensing in clusters . 7 1.4 Color image of three lensing clusters . 8 2.1 Color selection of z 2 Lyman-break galaxies (F275W-dropouts) . 20 ∼ 2.2 The magnification distribution of Lyman-break galaxies. 22 2.3 The intrinsic absolute magnitude vs. observed B-band magnitude . 25 2.4 Completeness contours . 28 2.5 The spectroscopic redshift distribution . 32 2.6 The photometric redshift distribution . 33 2.7 The UV luminosity function at z 2........................ 35 ∼ 2.8 UV spectral slope and E(B-V) as a function of absolute UV magnitude .
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