Star-Forming, Rotating Spheroidal Galaxies in the GAMA and SAMI Surveys
  The Galaxy And Mass Assembly (GAMA) survey has morphologically identified a
class of "Little Blue Spheroid" (LBS) galaxies whose relationship to other
classes of galaxies we now examine in detail. Considering a sample of 868 LBSs,
we find that such galaxies display similar but not identical colours, specific
star formation rates, stellar population ages, mass-to-light ratios, and
metallicities to Sd-Irr galaxies. We also find that LBSs typically occupy
environments of even lower density than those of Sd-Irr galaxies, where ~65% of
LBS galaxies live in isolation. Using deep, high-resolution imaging from VST
KiDS and the new Bayesian, two-dimensional galaxy profile modeling code PROFIT,
we further examine the detailed structure of LBSs and find that their S\'ersic
indices, sizes, and axial ratios are compatible with those of low-mass
elliptical galaxies. We then examine SAMI Galaxy survey integral field emission
line kinematics for a subset of 62 LBSs and find that the majority (42) of
these galaxies display ordered rotation with the remainder displaying
disturbed/non-ordered dynamics. Finally, we consider potential evolutionary
scenarios for a population with this unusual combination of properties,
concluding that LBSs are likely formed by a mixture of merger and accretion
processes still recently active in low-redshift dwarf populations. We also
infer that if LBS-like galaxies were subjected to quenching in a rich
environment, they would plausibly resemble cluster dwarf ellipticals.
