Home
Resource
Using cosmological hydrodynamic simulations to understand faint dwarf galaxies
PDF
PDF format is widely accepted and good for printing.
Plug-in required
PDF-1(2.23 MB)
Citation & Export
View Usage Statistics
Staff View

Citation & Export
Hide

Simple citation

Applebaum, Elaad. Using cosmological hydrodynamic simulations to understand faint dwarf galaxies. Retrieved from https://doi.org/doi:10.7282/t3-5m6q-kn08

Export

Click here for information about Citation Management Tools at Rutgers.

Statistics
Hide

Description

TitleUsing cosmological hydrodynamic simulations to understand faint dwarf galaxies
NameApplebaum, Elaad (author); Brooks, Alyson (chair); Christensen, Charlotte (member); Gawiser, Eric (member); Keeton, Charles (member); Somalwar, Sunil (member); Rutgers University; School of Graduate Studies
Date Created2021
Other Date2021-10 (degree)
SubjectAstrophysics, Dwarf galaxies
Extent1 online resource (x, 174 pages) : illustrations
DescriptionRecently, many new faint dwarf galaxies have been discovered around the Milky Way,including dozens of ultra-faint dwarf (UFD) galaxies—the smallest and most ancient galaxies known. We use cosmological hydrodynamic zoom-in simulations to study the formation and evolution of these galaxies. First, we introduce a new suite of high-resolution simulations of Milky Way-like hosts, enabling the study of UFDs in environments similar to those in which they have been discovered. We show that the simulated galaxies reproduce a variety of observed properties over orders of magnitude in luminosity. We further demonstrate that many of the properties of these simulated galaxies are influenced by interactions with their Milky Way-like hosts. Such interactions may contribute to the diversity seen in observed faint dwarfs.
Given the small potential wells of dwarf galaxies, they are very sensitive to the physicsof galaxy formation, much of which occurs on scales beneath our resolution. Therefore, we study how sub-grid models impact the properties of dwarf galaxies in the simulations. First, we update the treatment of the stellar initial mass function (IMF), which describes the distribution of stellar masses contained within each star particle. We implement a stochastically populated IMF, and show that it leads to burstier feedback, which suppresses star formation compared to a continuous treatment. Finally, we investigate how the underlying physics of star formation alters UFD properties by testing several different star formation models. We show that galaxy stellar metallicities are sensitive to changes between the runs, and can be paired with observations to constrain the models.
NotePh.D.
NoteIncludes bibliographical references
Genretheses
Persistent URLhttps://doi.org/doi:10.7282/t3-5m6q-kn08
LanguageEnglish
CollectionSchool of Graduate Studies Electronic Theses and Dissertations
Organization NameRutgers, The State University of New Jersey
RightsThe author owns the copyright to this work.
Version 8.5.5
Rutgers University Libraries - Copyright ©2024