Young, blue, and isolated stellar systems in the Virgo Cluster. II. A
  new class of stellar system
  We discuss five blue stellar systems in the direction of the Virgo cluster,
analogous to the enigmatic object SECCO 1 (AGC 226067). These objects were
identified based on their optical and UV morphology and followed up with HI
observations with the VLA (and GBT), MUSE/VLT optical spectroscopy, and HST
imaging. These new data indicate that one system is a distant group of
galaxies. The remaining four are extremely low mass ($M_\ast \sim 10^5 \;
\mathrm{M_\odot}$), are dominated by young, blue stars, have highly irregular
and clumpy morphologies, are only a few kpc across, yet host an abundance of
metal-rich, $12 + \log (\mathrm{O/H}) > 8.2$, HII regions. These high
metallicities indicate that these stellar systems formed from gas stripped from
much more massive galaxies. Despite the young age of their stellar populations,
only one system is detected in HI, while the remaining three have minimal (if
any) gas reservoirs. Furthermore, two systems are surprisingly isolated and
have no plausible parent galaxy within $\sim$30' ($\sim$140 kpc). Although
tidal stripping cannot be conclusively excluded as the formation mechanism of
these objects, ram pressure stripping more naturally explains their properties,
in particular their isolation, owing to the higher velocities, relative to the
parent system, that can be achieved. Therefore, we posit that most of these
systems formed from ram pressure stripped gas removed from new infalling
cluster members, and survived in the intracluster medium long enough to become
separated from their parent galaxies by hundreds of kiloparsecs, and that they
thus represent a new type of stellar system.
