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Supermassive Black Holes in Bulgeless and Dwarf Galaxies: A Multi-Wavelength Investigation

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dc.contributor.advisor Satyapal, Shobita
dc.contributor.author Secrest, Nathan en_US
dc.creator Secrest, Nathan en_US
dc.date.accessioned 2015-02-12T02:59:15Z
dc.date.available 2015-02-12T02:59:15Z
dc.date.issued 2014 en_US
dc.identifier.uri http://hdl.handle.net/1920/9180
dc.description.abstract Supermassive black holes (SMBHs) are now understood to reside at the centers of nearly all major galaxies in the Universe. From studies of high-redshift quasars, we understand that SMBHs formed very early in the Universe's history, and well-studied correlations between other properties of galaxies, such as their morphologies, star formation rate, and merger history, with their central SMBH shows that SMBHs played a key role in the evolution of galaxies. The fact that the post-Big Bang Universe was extremely uniform and homogeneous presents a major mystery: How did SMBHs millions to billions of times as massive as the Sun form in such a short time? Given the theoretical limit at which a black hole can accrete material, it is not plausible that SMBHs could have formed through the conventional route: the end stage of the lifecycle of a massive star. Rather, there are two major theories for the formation of SMBHs, each with its own prediction for the black hole mass distribution and occupation fraction in the local Universe. Understanding this mass distribution and occupation fraction is therefore imperative to understanding the formation of SMBHs, the quasars that reveal their presence in the early Universe, and ultimately the evolution of galaxies to the present day. While large SMBHs in major, bulge-dominated galaxies are relatively easy to detect and characterize, this population of SMBHs is understood to have been built up largely through black hole merger events that erase any information about the progenitor black holes' masses. We must therefore search for SMBHs in late-type, bulgeless, and dwarf galaxies, which are much more likely to have had a relatively quiet, merger-free history, in order to glimpse the properties of the `seed' black holes that led to the buildup of SMBHs during the earliest epoch of the Universe. In this thesis, I will discuss my contributions to the understanding of this question, as well as what questions remain to be answered and the future of research in this field. en_US
dc.format.extent 109 pages en_US
dc.language.iso en en_US
dc.rights Copyright 2014 Nathan Secrest en_US
dc.subject Astrophysics en_US
dc.subject Astronomy en_US
dc.subject Physics en_US
dc.subject active galactic nuclei en_US
dc.subject black holes en_US
dc.subject extragalactic en_US
dc.subject galaxies en_US
dc.subject infrared astronomy en_US
dc.subject X-ray astronomy en_US
dc.title Supermassive Black Holes in Bulgeless and Dwarf Galaxies: A Multi-Wavelength Investigation en_US
dc.type Dissertation en
thesis.degree.level Doctoral en
thesis.degree.discipline Physics en
thesis.degree.grantor George Mason University en


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