Abstract:
The spectral region between 1250–3000 A 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, H2 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.
