Authors: Joachim Janz, Samantha J. Penny, Alister W. Graham, Duncan A. Forbes, Roger L. Davies
We present the discovery of rotation in quenched, low-mass early-type galaxies that are isolated. This finding challenges the claim that (all) rotating dwarf early-type galaxies in clusters were once spiral galaxies that have since been harassed and transformed into early-type galaxies. Our search of the Sloan Digital Sky Survey data within the Local volume (z < 0.02) has yielded a sample of 46 galaxies with a stellar mass M* < 5×109 MSun (median M* ≈ 9.29×108 MSun), a low Hα equivalent width EWHα < 2 Angstrom, and no massive neighbour (M* > 3×1010 MSun) within a velocity interval of ΔV = 500 km/s and a projected distance of 1 Mpc. The median distance in projection to the closest bright neighbour is 1.85 Mpc, and the median ΔV = 222 km/s relating to that neighbour. Nine of these galaxies were subsequently observed with Keck ESI and their radial kinematics are presented here. These extend out to the half-light radius Re in the best cases, and beyond Re/2 for all. They reveal a variety of behaviours similar to those of a comparison sample of early-type dwarf galaxies in the Virgo cluster observed by Toloba et al. Both samples have similar frequencies of slow and fast rotators, as well as kinematically decoupled cores. This, and especially the finding of rotating quenched low-mass galaxies in isolation, reveals that contrary to popular belief, the early-type dwarfs in galaxy clusters need not be harassed or tidally stirred spiral galaxies.