Description
The scarcity of truly isolated quiescent dwarf galaxies (7 < (log$M_*/M_{\odot}$) < 9) is interpreted as evidence that becoming a satellite of a more massive halo is a necessary condition to quench star formation activity in these systems. In this study, we present a detailed analysis of environmental quenching using VLT-MUSE observations of a sample of 70+ dwarf galaxies from the MATLAS survey, which consists of groups at 15 < D < 35 Mpc. Integral field spectroscopy allows us to detect very faint Ha emission ( > $10^{-18}\ \mathrm{erg/s/cm^2/arcsec^2}$) and spatially resolve the star-forming gas. We find a quenched fraction of ~30% and star formation rates (SFR) in the range −3 < log SFR < −1. Notably, roughly half of the star-forming dwarfs exhibit off-centre star formation activity, which may be missed by traditional multi-object spectroscopic surveys. Finally, we will discuss the star-forming region properties of the satellites in the context of their orbital distribution using position-velocity phase-space diagrams. This sample of MATLAS dwarfs provides a local benchmark for studying star formation with unprecedented detail and sensitivity, offering new insights into the environmental quenching of low-mass satellites.
