We describe results of a multi-spectral study of a blue compact dwarf
galaxy in the Virgo Cluster. The object was observed with broad-band a
nd Her imaging, ultraviolet observations, and radio synthesis. Our dat
a were combined with previously published optical observations, with H
I single-beam observation and with far-infrared data, and were compare
d to results of evolutionary synthesis programs. The radio synthesis o
bservations revealed a compact concentration of HI coincident with the
optical galaxy, embedded in a diffuse, asymmetric HI cloud which has
no trace of optical emission. While the overall velocity dispersion an
d size of the KI structure suggests that the total mass in stars and g
as is not sufficient to gravitationally bind the system as a whole, th
e HI clump coincident with the optical galaxy requires little or no da
rk matter to be self-gravitating. The diffuse cloud has more complex v
elocity structure and is extended in a direction approximately perpend
icular to the optical major axis. 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 t
he 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, the correspondence of the opt
ical and HI redshifts, and the lack of any suitable nearby galaxy, ind
icate that the starburst was probably not triggered by an external int
eraction with a visible galaxy. The distribution of HI fits better a b
low-out scenario than an accretion or collision with a companion. We p
oint out features in common with other actively star-forming dwarf gal
axies and conclude that, at least in the southern outskirts of the Vir
go cluster, intensive star formation, perhaps for the first time in so
me objects, takes place at present.