期刊
ASTROPHYSICAL JOURNAL
卷 759, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.1088/0004-637X/759/2/138
关键词
galaxies: dwarf; galaxies: evolution; galaxies: halos; galaxies: luminosity function, mass function; galaxies: statistics; radio lines: galaxies
资金
- NSF [AST-0607007, AST-1107390]
- Brinson Foundation
- Onassis Foundation
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy
- NASA
- Japanese Monbukagakusho
- Max Planck Society
- Higher Education Funding Council for England
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1107390] Funding Source: National Science Foundation
We use both an Hi-selected and an optically selected galaxy sample to directly measure the abundance of galaxies as a function of their baryonic mass (stars + atomic gas). Stellar masses are calculated based on optical data from the Sloan Digital Sky Survey and atomic gas masses are calculated using atomic hydrogen (H (I)) emission line data from the Arecibo Legacy Fast ALFA survey. By using the technique of abundance matching, we combine the measured baryonic function of galaxies with the dark matter halo mass function in a.CDM universe, in order to determine the galactic baryon fraction as a function of host halo mass. We find that the baryon fraction of low-mass halos is much smaller than the cosmic value, even when atomic gas is taken into account. We find that the galactic baryon deficit increases monotonically with decreasing halomass, in contrast with previous studies which suggested an approximately constant baryon fraction at the low-mass end. We argue that the observed baryon fractions of low-mass halos cannot be explained by reionization heating alone, and that additional feedback mechanisms (e.g., supernova blowout) must be invoked. However, the outflow rates needed to reproduce our result are not easily accommodated in the standard picture of galaxy formation in a Lambda CDM universe.
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