http://www.loc.gov/mods/v3 http://www.loc.gov/standards/mods/v3/mods-3-2.xsd
Exploring the Extremes of Galaxy Evolution: Progenitors of Star-Forming Galaxies and Relics of Quiescent Galaxies
In this dissertation, I investigate the formation and evolution of galaxies by studying two extreme populations ⁰́₄ young, highly star forming galaxies (SFGs) at z > 2, and old, quiescent galaxies in the local Universe that are likely unchanged since z ⁹́⁸ 2. In the first project, I use spectral energy distribution (SED)-fitting to analyze the star formation histories (SFHs) of a population of extreme emission line galaxies (EELGs) identified in the ZFOURGE Survey at 2.5 ⁹́Þ z ⁹́Þ 4, comparing them to more typical SFGs at the same redshift range. This is the first z > 2 study to use the PROSPECTOR SED-fitting code. The EELGs display rising SFHs in the most recent 50 Myr, while more typical SFGs do not. I estimate that many, if not most, SFGs at z ⁹́Æ 2.5 undergo an extreme HÎø+[OIII] emission line phase early in their lifetimes. In the second project, I present 0Êð.14-resolution Atacama Large Millimeter/submillimeter Array (ALMA) CO(2⁸́₂1) observations of the circumnuclear gas disk in the local compact galaxy UGC 2698, a member of a sample of nearby early-type galaxies that are plausible z ⁹́⁸ 2 red nugget relics. I fit molecular gas-dynamical models to the ALMA data cube, assuming the CO emission originates from a dynamically cold, thin disk, and measure the mass of the supermassive black hole (BH) in UGC 2698. I explore systematics in the model and their effects on the measured BH mass. The BH in UGC 2698 is found to be consistent with the BH scaling relations, which I contrast with previous stellar-dynamical measurements for three other objects in the local compact galaxy sample. In the third project, I present ALMA CO(2⁸́₂1) observations at a resolution of 0Êð.22 in the local compact galaxies NGC 384 and PGC 11179. I make preliminary molecular gas-dynamical BH mass measurements in these galaxies and explore their systematic uncertainties. Finally, I discuss the next steps required to finalize these measurements and the implications of these results for our understanding of BH⁸́₂host galaxy co-evolution and the scatter of the BH scaling relations. The electronic version of this dissertation is accessible from https://hdl.handle.net/1969.1/197785
Doctor of Philosophy Texas A&M University 2022 https://hdl.handle.net/1969.1/197785