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Rapid Environmental Quenching of Satellite Dwarf Galaxies in the Local Group | | Andrew R. Wetzel
; Erik J. Tollerud
; Daniel R. Weisz
; | | Date: |
23 Mar 2015 | | Abstract: | In the Local Group, nearly all of the dwarf galaxies (M_star < 10^9 M_sun)
that are satellites within 300 kpc (the virial radius) of the Milky Way (MW)
and Andromeda (M31) have quiescent star formation and little-to-no cold gas.
This contrasts strongly with comparatively isolated dwarf galaxies, which are
almost all actively star-forming and gas-rich. This near dichotomy implies a
rapid transformation after falling into the halos of the MW or M31. We combine
the observed quiescent fractions for satellites of the MW and M31 with the
infall times of satellites from the ELVIS suite of cosmological simulations to
determine the typical timescales over which environmental processes within the
MW/M31 halos remove gas and quench star formation in low-mass satellite
galaxies. The quenching timescales for satellites with M_star < 10^8 M_sun are
short, < 2 Gyr, and quenching is more rapid at lower M_star. These quenching
timescales can be 1 - 2 Gyr longer if environmental preprocessing in lower-mass
groups prior to MW/M31 infall is important. We compare with quenching
timescales for more massive satellites from previous works and synthesize the
nature of satellite quenching across the observable range of M_star = 10^{3-11}
M_sun. The environmental quenching timescale increases rapidly with satellite
M_star, peaking at ~9.5 Gyr for M_star ~ 10^9 M_sun, and rapidly decreases at
higher M_star to < 5 Gyr at M_star > 5x10^9 M_sun. Overall, galaxies with
M_star ~ 10^9 M_sun, similar to the Magellanic Clouds, exhibit the longest
quenching timescales, regardless of environmental or internal mechanisms. | | Source: | arXiv, 1503.6799 | | Services: | Forum | Review | PDF | Favorites | |
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