  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 $M_\star \lesssim
5\times10^9$ M$_\odot$ (median $M_\star \sim 9.29 \times 10^8$ M$_\odot$), a
low H$\alpha$ equivalent width EW$_{{\rm H}\alpha}< 2$ \AA, and no massive
neighbour ($M_{\star}\gtrsim3 \times 10^{10}$ M$_{\odot}$) within a velocity
interval of $\Delta V = 500$ km s$^{-1}$ and a projected distance of $\sim$1
Mpc. 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
$R_e$ in the best cases, and beyond $R_e/2$ 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 the early-type dwarfs in galaxy clusters need not be
harassed or tidally stirred spiral galaxies.
