  In this paper we test if nearby blue spheroid (BSphs) galaxies may become the
progenitors of star-forming spiral galaxies or passively-evolving elliptical
galaxies. Our sample comprises 428 galaxies of various morphologies in the
redshift range 0.002<z<0.02 (8-87 Mpc) with panchromatic data from the Galaxy
and Mass Assembly survey. We find that BSph galaxies are structurally (mean
effective surface brightness, effective radius) very similar to their
passively-evolving red counterparts. However, their star-formation and other
properties such as colour, age and metallicity are more like star-forming
spirals than spheroids (ellipticals and lenticulars). We show that BSph
galaxies are statistically distinguishable from other spheroids as well as
spirals in the multi-dimensional space mapped by luminosity-weighted age,
metallicity, dust mass and specific star formation rate.
  We use HI data to reveal that some of the BSphs are (further) developing
their disks, hence their blue colours. They may eventually become spiral
galaxies --- if sufficient gas accretion occurs --- or more likely fade into
low-mass red galaxies.

Astrophysics of Galaxies