Planetary Nebulae with UVIT: A Progress Report
  The spectral region between 1250 Angstroms - 3000 Angstroms contains
important spectral lines to understand the morphological structures and
evolution of planetary
  nebulae. This is the region sampled by UVIT through various filter bands both
in the continuum and in emission lines (e.g. C IV, He I, Mg II etc.). We have
mapped several planetary nebulae with different characteristics, ranging in
morphology from bipolar to wide and diffuse, and in various states of
ionization, comparing the UV with the x-ray morphologies wherever the x-ray
images were also available. The major unanticipated discovery with UVIT has
been the detection of previously undetected, cold, fluorescent, molecular
hydrogen gas surrounding some planetary nebulae. This may be a possible
solution to the missing mass problem. Here we present a review of our studies
so far done (both published and on going) with UVIT.
