  NGC 2915 is a remarkable blue compact dwarf galaxy which contains an inner HI
bar and strong spiral structure in its HI disk extending well beyond its
optical disk. We propose here that NGC 2915 has a dark or faint (not yet
observed) massive disk component. By massive we mean of the same order as the
HI gas mass which ranges from 0.5 -- 10 Msol/pc^2. We present three different
dynamical arguments based on bar and spiral structure that an additional disk
mass component is required. The additional mass requirements from these three
dynamical arguments depend upon the distance of the galaxy in the same way. If
the galaxy were at a distance twice that estimated then the additional mass
required would be negligible. Virgocentric models show that then its radial
velocity would be 250-500 km/s below its local bulk flow value. Local flow
models suggest that this is unlikely, however they also do not exclude it at
high confidence levels. Detection of a quiescent or faint stellar disk
population would be an exciting prospect since it would be strong evidence for
a previous epoch of star formation in a previously low surface brightness
galaxy. Then NGC 2915 would be an example of a galaxy which has faded and so
could have been one of the faint blue galaxy population observed at moderate
redshift.
