  We describe results of a multi-spectral study of a blue compact dwarf galaxy
in Virgo. The object was observed with broad-band and H$\alpha$ imaging, UV
observations, and radio synthesis. Our data were combined with published
optical observations, with HI single-beam observation and with FIR data, and
were compared to results of evolutionary synthesis programs. The radio
observations revealed a compact source of HI coincident with the optical
galaxy, embedded in a diffuse, HI cloud which has no trace in the optical.
While the overall velocity dispersion and size of the HI structure suggests
that the total mass in stars and gas is not sufficient to gravitationally bind
the system, the HI clump coincident with the optical galaxy requires little or
no dark matter to be self-gravitating. The optical-UV data can be explained by
a single population of stars formed in a recent burst, indicating that this is
a genuine young galaxy. The efficiency of star formation is similar to that in
large disk galaxies. The IR emission indicates the presence of dust; this must
have been formed very recently, or was already present within the original HI
cloud from which the galaxy was formed. The round and smooth isophotes and HI
redshifts, and the lack of any suitable nearby galaxy, indicate that the
starburst was probably not triggered by an external interaction with a visible
galaxy. The distribution of HI fits better a blow-out scenario than an
accretion or collision with a companion. We point out features in common with
other actively star-forming dwarf galaxies and conclude that, at least in the
southern outskirts of the Virgo cluster, intensive star formation, perhaps for
the first time in some objects, takes place at present.
