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UNIVERSITY of CALIFORNIA SAN DIEGO Properties and Impact Of UNIVERSITY OF CALIFORNIA SAN DIEGO Properties and Impact of Active Galactic Nuclei-driven Outflows through Cosmic Time A dissertation submitted in partial satisfaction of the requirements for the degree Doctor of Philosophy in Physics by Gene Chun Kwan Leung Committee in charge: Professor Alison L. Coil, Chair Professor Farhat N. Beg Professor Patrick H. Diamond Professor Karin M. Sandstrom Professor Shelley A. Wright 2020 Copyright Gene Chun Kwan Leung, 2020 All rights reserved. The dissertation of Gene Chun Kwan Leung is approved, and it is acceptable in quality and form for publication on microfilm and electronically: Chair University of California San Diego 2020 iii DEDICATION To my parents iv EPIGRAPH Once we overcome our fear of being tiny, we find ourselves on the threshold of a vast and awesome Universe that utterly dwarfs – in time, in space, and in potential – the tidy anthropocentric proscenium of our ancestors. —Carl Edward Sagan v TABLE OF CONTENTS Signature Page . iii Dedication . iv Epigraph . v Table of Contents . vi List of Figures . ix List of Tables . xii Acknowledgements . xiii Vita ............................................. xv Abstract of the Dissertation . xviii Chapter 1 Introduction . 1 1.1 Galaxies . 2 1.2 Active Galactic Nuclei . 3 1.3 Co-evolution of Galaxies and SMBHs . 6 1.4 AGN Feedback . 9 1.5 Overview . 12 Chapter 2 The MOSDEF survey: the prevalence and properties of galaxy-wide AGN- driven outflows at z ∼ 2........................... 13 2.1 Abstract . 13 2.2 Introduction . 14 2.3 Observations and AGN Sample . 18 2.3.1 The MOSDEF Survey . 18 2.3.2 X-ray AGN Sample . 19 2.3.3 IR AGN Sample . 20 2.3.4 Optical AGN Sample . 21 2.3.5 Stellar Masses and Star Formation Rates . 24 2.4 Outflow Detection and Analysis . 25 2.4.1 Detection of Outflows in AGN . 25 2.4.2 Detection of Outflows in Galaxies . 28 2.4.3 Kinematics . 30 2.4.4 Line Ratios . 31 2.4.5 Physical Extent . 33 2.4.6 COSMOS 11223 . 36 vi 2.5 Discussion . 39 2.5.1 Outflow Incidence . 39 2.5.2 Correlation with Host Galaxy Properties . 40 2.5.3 Correlation with [OIII] Luminosity and S/N . 42 2.5.4 Correlation with X-ray, IR and Optical AGN Identification . 44 2.5.5 Mass and Energy Outflow Rates . 45 2.5.6 Physical Driver of Outflows and Impact on Host Galaxies . 50 2.5.7 Positive AGN Feedback in MOSDEF and SDSS . 53 2.6 Conclusions . 56 2.7 Acknowledgements . 58 Chapter 3 The MOSDEF survey: a census of AGN-driven ionized outflows at z = 1:4 − 3:8................................... 60 3.1 Abstract . 60 3.2 Introduction . 61 3.3 Observations and AGN Sample . 65 3.3.1 The MOSDEF Survey . 65 3.3.2 Emission Line Measurements . 66 3.3.3 AGN Sample . 67 3.3.4 Stellar Masses and Star Formation Rates . 69 3.4 Outflow Detection and Characterization . 69 3.4.1 Detection of Outflows in AGNs . 70 3.4.2 Detection of Outflows in Inactive Galaxies . 71 3.4.3 Outflow Kinematics . 74 3.4.4 Emission Line Ratios . 75 3.4.5 Physical Extent . 77 3.4.6 Mass and Energy Outflow Rates . 79 3.4.7 Stacked Spectrum Analysis . 84 3.5 Outflow Incidence and Host Properties . 85 3.5.1 Host Galaxy Properties . 85 3.5.2 [OIII] Luminosity . 88 3.6 Outflow Parameters and Host Galaxy Properties . 91 3.6.1 Outflow Velocity and Radius . 92 3.6.2 Mass and Energy Outflow Rates . 96 3.6.3 Physical Driver of the Outflows . 100 3.6.4 Mass Loading Factor . 101 3.6.5 Momentum Flux . 105 3.7 Conclusions . 107 3.8 Acknowledgements . 111 3.9 Appendix . 111 3.9.1 Emission Line Spectra and Tabulated Data . 111 vii Chapter 4 KCWI observations of the extended nebulae in Mrk 273 . 115 4.1 Abstract . 115 4.2 Introduction . 116 4.3 Observations and Data . 119 4.3.1 KCWI Observations . 119 4.3.2 Data Reduction . 120 4.3.3 Data Analysis . 121 4.4 Results . 123 4.4.1 Morphology . 123 4.4.2 Emission Lines . 125 4.4.3 Kinematics . 129 4.4.4 Emission Line Ratio Maps . 131 4.4.5 Ionization Mechanism . 134 4.5 Discussion . 142 4.6 Conclusions . 143 4.7 Acknowledgements . 145 Chapter 5 Conclusions and Future Work . 146 5.1 Unveiling the Impact of Molecular AGN-Driven Outflows at z ∼ 2 . 148 5.2 Revealing the Full Physical Extent of AGN Outflows . 150 5.3 Quantifying AGN-driven Outflows with Very Large Samples . 151 viii LIST OF FIGURES Figure 1.1: Global star formation rate density and SMBH accretion rate density through cosmic time. 8 Figure 2.1: 1D spectra showing the Hb (left), [OIII], and Ha and [NII] emission lines of all 13 AGN outflows not identified as potential mergers. 26 Figure 2.2: Same as Figure 2.1 but for outflow candidates identified as potential mergers. 27 Figure 2.3: HST F160W band images of all 13 AGN outflows not identified as potential mergers. 29 Figure 2.4: Same as Figure 2.3 but for AGN outflow candidates identified as potential mergers. 29 Figure 2.5: Left: Distribution of the velocity widths (FWHMv) and velocity offsets (Dv) for the AGN outflows. Right: Distribution of the maximum velocity (vmax) of the AGN outflows. 30 Figure 2.6: [NII] BPT diagrams for gas in the narrow-line component (left) and outflow component (right) of the AGN with outflows in our sample. 32 Figure 2.7: Spatial profiles (upper) derived from 2D spectra (lower) of the [OIII]l5008 emission line for AGN outflows with significant spatial extent detected in this emission line. 34 Figure 2.8: Same as Figure 2.7 but for the Ha emission line. 34 Figure 2.9: (a) 1D (top) and 2D (bottom) spectra of COSMOS 11223. (b) HST F160W band images of COSMOS 11223. (c) Spatial profiles for the [OIII]l5008 (left) and Ha (right) emission lines. 37 Figure 2.10: Left: SFR versus stellar mass for all galaxies, AGN and AGN with outflows in the current sample. Upper right: Distribution of stellar mass for all AGN and AGN with outflows. Lower right: Distribution of SFR=SFRMS for all AGN and AGN with outflows. 42 Figure 2.11: Distribution of L[OIII] versus the signal-to-noise ratio in [OIII] for all AGN and AGN with outflows. 43 Figure 2.12: Left: Mass outflow rates estimated for the ionized gas versus the bolometric AGN luminosity. Right: Energy outflow rate of the ionized gas versus the bolometric AGN luminosity. 45 Figure 2.13: The ratio of the kinetic energy rates in the outflow to the AGN luminosity versus the ratio of the observed mass outflow rates to the maximum mass outflow rates that could be provided by stellar feedback. 51 Figure 2.14: The ratio of the momentum flux of the outflow to the radiation pressure of the AGN versus the luminosity of the AGN. 52 Figure 2.15: BPT diagrams for optically-selected AGN with outflows in SDSS using line ratios from Mullaney et al. (2013). 54 Figure 3.1: Velocity dispersion versus velocity shift for the detected AGN outflows in our sample. 73 ix Figure 3.2: Left: BPT diagram for the narrow-line component of each AGN with an outflow in our sample. Middle: Same as left panel, but for the outflow com- ponents in our sample. Right: Velocity dispersion of the outflow component versus the [NII] to Ha line ratio. 73 Figure 3.3: Stacked emission line spectrum of 23 AGNs with blueshifted outflows and no BLR emission, weighted by vmax...................... 78 Figure 3.4: Left: Distribution of SFR and M∗ for all AGNs in the MOSDEF survey and the AGNS with detected outflows in our sample. Middle: Histogram of M∗ for all AGNs and AGNs with outflows and the outflow fraction. Right: Same as the middle panel, but for SFR relative to the main sequence. 82 Figure 3.5: Left: M∗ histogram for all galaxies, all AGNs and AGNs with outflows in the MOSDEF survey. Middle: The fraction of galaxies that host an AGN and the fraction of galaxies that host an AGN and an outflow as a function of M∗. Right: The fraction of AGNs that host an outflow as a function of M∗. 85 Figure 3.6: Distribution of signal to noise (S/N) in.
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