  We present the first HI spectral line images of the nearby, star-forming
dwarf galaxies UGC11411 and UGC 8245, acquired as part of the "Observing for
University Classes" program with the Karl G. Jansky Very Large Array (VLA).
These low-resolution images localize the HI gas and reveal the bulk kinematics
of each system. Comparing with HST broadband and ground-based H{\alpha}
imaging, we find that the ongoing star formation in each galaxy is associated
with the highest HI mass surface density regions. UGC 8245 has a much lower
current star formation rate than UGC 11411, which harbors very high surface
brightness H{\alpha} emission in the inner disk and diffuse, lower surface
brightness nebular gas that extends well beyond the stellar disk as traced by
HST. We measure the dynamical masses of each galaxy and find that the halo of
UGC 11411 is more than an order of magnitude more massive than the halo of UGC
8245, even though the HI and stellar masses of the sources are similar. We show
that UGC8245 shares similar physical properties with other well-studied
low-mass galaxies, while UGC11411 is more highly dark matter dominated. Both
systems have negative peculiar velocities that are associated with a coherent
flow of nearby galaxies at high supergalactic latitude.
