Speaker: Samantha Penny

Despite being the dominant galaxy population by number in groups and clusters, the formation timescale and mechanism of quenched dwarf galaxies remains unknown. Are quenched dwarfs the remnants of hierarchical galaxy assembly, or are they formed at later times via the morphological transformation of more massive galaxies? To address this question requires spatially-resolved spectroscopy to uncover their kinematics and formation timescales. Using data from the first year of the SDSS-IV MaNGA IFU survey, we identify a sample of 39 quenched, low mass (dwarf) galaxies with M* < 5×10^9 Msun, selected independently of morphology and environment. In this talk, I will show the majority of quenched dwarf galaxies exhibit coherent rotation in their stellar kinematics, and several host disc or spiral features, inconsistent with a primordial origin. Several exhibit kinematically distinct cores which must form via gas infall and accretion. I will discuss an origin for these dwarfs as quenched low-mass disc/spiral galaxies, supporting the hypothesis that galaxy-galaxy or galaxy-group interactions quench star formation in low mass galaxies. I will also show that despite being the "simplest" galaxies in our current models of galaxy formation, quenched dwarf galaxies are a diverse population, with detailed spectroscopy crucial to understand their origin.