  Several recent studies find that 10 - 50% of morphologically selected field
early-type galaxies at redshifts z <= 1 have blue colors indicative of recent
star formation. Such ``blue spheroids''might be massive early-type galaxies
with active star formation, perhaps induced by recent merger events.
  Alternatively, they could be starbursting, low-mass spheroids. To distinguish
between these two choices, we have selected 10 ``Blue Spheroid Candidates''
  (hereafter, BSCs) from a quantitatively selected E/S0 sample and studied
their properties, including kinematics from Keck spectra obtained as part of
the DEEP Groth Strip Survey (GSS). Most BSCs (70%) turn out to belong to two
broad categories, while the remaining objects are likely to be misclassified
objects. Type-1 BSCs have underlying red stellar components with bluer inner
components. Type-2 BSCs do not show an obvious sign of the underlying red
stellar component, and their overall colors are quite blue ((U-B)_rest < 0).
  Both Type-1 and Type-2 BSCs have internal velocity dispersions measured from
emission lines sigma < 80$ km/sec and estimated dynamical masses of only a few
times 10^10 M_sun or less. For Type-1 BSCs, we estimate sigma of the red
component using the fundamental plane relation of distant field absorption-line
galaxies and find that these sigma estimates are similar to the sigma measured
from emission lines. Overall, we conclude that our Type-1 and Type-2 BSCs are
more likely to be star-forming low mass spheroids than star-forming, massive,
early-type galaxies.
