Rapid Environmental Quenching of Satellite Dwarf Galaxies in the Local Group

TL;DR

This study investigates how quickly dwarf satellite galaxies in the Local Group stop forming stars after falling into the Milky Way or Andromeda, revealing that low-mass satellites quench rapidly within 2 Gyr, with quenching timescales varying with galaxy mass.

Contribution

It combines observational data with cosmological simulations to quantify the environmental quenching timescales of satellite dwarf galaxies across a wide mass range, highlighting the rapid quenching in low-mass satellites.

Findings

Quenching timescales are less than 2 Gyr for satellites with M_star < 10^8 M_sun.

Quenching timescales increase with galaxy mass, peaking at ~9.5 Gyr around 10^9 M_sun.

Quenching is faster at lower galaxy masses and can be extended by pre-processing in groups.

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 of satellite dwarf galaxies 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 Exploring the Local Volume in Simulations (ELVIS) suite of cosmological zoom-in 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 satellite quenching timescales can be 1 - 2 Gyr longer if one includes the time that satellites were environmentally preprocessed by low-mass groups prior to MW/M31 infall. We compare with quenching timescales for more massive satellites from previous works to synthesize the nature of satellite galaxy quenching across the observable range of M_star = 10^{3-11} M_sun. The satellite quenching timescale increases rapidly with satellite M_star, peaking at ~9.5 Gyr for M_star ~ 10^9 M_sun, and the timescale rapidly decreases at higher M_star to < 5 Gyr at M_star > 5 x 10^9 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.