The resolve survey atomic gas census and environmental influences on galaxy gas reservoirs
- Physics and Astronomy Department, University of North Carolina, Chapel Hill, NC 27516 (United States)
- Department of Physics and Astronomy, Vanderbilt University, Nashville, TN 37240 (United States)
- European Southern Observatory, Santiago (Chile)
- Jeremiah Horrocks Institute, University of Central Lancashire, Preston, Lancashire, PR1 2HE (United Kingdom)
- Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853 (United States)
- Department of Astronomy, the Ohio State University, Columbus, OH 43210 (United States)
- Department of Physics and Astronomy, West Virginia University, Morgantown, WV 26506 (United States)
- Atmospheric and Environmental Research, Lexington, MA 02421 (United States)
- Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Santiago (Chile)
We present the H i mass inventory for the REsolved Spectroscopy Of a Local VolumE (RESOLVE) survey, a volume-limited, multi-wavelength census of >1500 z = 0 galaxies spanning diverse environments and complete in baryonic mass down to dwarfs of ∼10{sup 9} M{sub ⊙}. This first 21 cm data release provides robust detections or strong upper limits (1.4M {sub H i} < 5%–10% of stellar mass M {sub *}) for ∼94% of RESOLVE. We examine global atomic gas-to-stellar mass ratios (G/S) in relation to galaxy environment using several metrics: group dark matter halo mass M {sub h}, central/satellite designation, relative mass density of the cosmic web, and distance to the nearest massive group. We find that at fixed M {sub *}, satellites have decreasing G/S with increasing M {sub h} starting clearly at M {sub h} ∼ 10{sup 12} M{sub ⊙}, suggesting the presence of starvation and/or stripping mechanisms associated with halo gas heating in intermediate-mass groups. The analogous relationship for centrals is uncertain because halo abundance matching builds in relationships between central G/S, stellar mass, and halo mass, which depend on the integrated group property used as a proxy for halo mass (stellar or baryonic mass). On larger scales G/S trends are less sensitive to the abundance matching method. At fixed M {sub h} ≤ 10{sup 12} M{sub ⊙}, the fraction of gas-poor centrals increases with large-scale structure density. In overdense regions, we identify a rare population of gas-poor centrals in low-mass (M {sub h} < 10{sup 11.4} M{sub ⊙}) halos primarily located within ∼1.5× the virial radius of more massive (M {sub h} > 10{sup 12} M{sub ⊙}) halos, suggesting that gas stripping and/or starvation may be induced by interactions with larger halos or the surrounding cosmic web. We find that the detailed relationship between G/S and environment varies when we examine different subvolumes of RESOLVE independently, which we suggest may be a signature of assembly bias.
- OSTI ID:
- 22868431
- Journal Information:
- Astrophysical Journal, Vol. 832, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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