0 Assigned ID: 4219 ----- Attempting Submission 1 (Wed May 24 01:00:30 GMT 2023) ----- We propose to run a new suite of high-resolution cosmological simulations optimized to study dwarf satellite galaxies as they interact with their hosts. Hubble has played a pivotal role in revealing the rich diversity of dwarf galaxies in the Local Group, with the key finding that the fraction of satellite galaxies that are quenched approaches 100% at low mass, a phenomenon rarely if ever seen in the field. This is known as 'environmental quenching'; the gas contents of satellite galaxies are modulated by their interactions with the larger host and its gas halo. However, evidence is mounting that Local Group dwarf galaxies are more commonly quenched relative to satellites of other nearby L* hosts. While cosmological zooms have addressed these issues, no simulation has yet achieved the fine mass and time resolution on which gas stripping occurs when it is seen directly in observations. We will implement novel techniques to focus computational resources on the dwarfs and the host halo through which they travel, rather than on the host's disk, allowing us to reach 10-100x gains in mass and time resolution for a large sample of simulated satellites. These simulations will allow us to track the main physical mechanisms - ram-pressure stripping/compression, heating from shocks, turbulence, and tidal forces - in sufficient detail to quantify their relative influence on the gas content and star formation of an accreting dwarf throughout its lifetime. We will release derived catalogs from these dwarf simulations so that other groups can test them against the observed star formation histories and quenched fractions of satellite populations in the Milky Way and nearby galaxies. Dr. Anna Wright (PI, JHU) is an observationally oriented computational astrophysicist who specializes in the formation and evolution of dwarf and low surface brightness galaxies, with a particular focus on how these galaxies are influenced by their environments. She has experience running and analyzing simulations run with Gasoline, ChaNGa, and Enzo. She will be selecting the targets, running the simulations, and performing the bulk of the analysis. Dr. Jason Tumlinson (Co-I, STScI/JHU) is an observational and theoretical astrophysicist with a strong focus on the role of gas processes in driving galaxy evolution. He was PI of the COS-Halos team, which used 263 orbits of COS time to explore the diffuse CGM of 80 low redshift galaxies in the most comprehensive survey of gas up to that time. Dr. Tumlinson is currently a Co-PI of the FOGGIE (Figuring Out Gas and Galaxies In Enzo) collaboration and serves as the Head of Community Missions at STScI. He will provide scientific advice and administrative oversight to the program and co-author the key publications. Dr. Molly Peeples (Co-I, STScI/JHU) is the PI of the FOGGIE collaboration. She will provide overall scientific oversight and co-author publications. Prof. Brian O'Shea (Co-I, MSU) is a computational astrophysicist and one of the primary developers of the Enzo code. Dr. Erik Tollerud (Co-I, STScI) is an expert on dwarf galaxy evolution and a CoI on the SAGA project. He also has experience bridging observations and simulations of dwarf galaxies. Dr. Cassandra Lochhaas (Co-I, STScI) is a postdoc in the STScI FOGGIE collaboration with expertise in using AMR-based hydro simulations to explore the gas flows that drive galaxy evolution. For this project, Dr. Lochhaas will consult on the analysis as an expert on AMR simulations of the CGM and co-author publications. Dr. Raymond Simons (Co-I, UConn) is a collaborator with the FOGGIE group. His detailed study of gas stripping in FOGGIE halos partially motivated this proposal. Dr. Greg Snyder (Co-I, STScI) is a staff scientist and an expert on galaxy formation, simulations, and connecting theory to observations. Galaxies 0 Regular false false false true false false SUPPORTED