Planetary Nebulae with UVIT II: Revelations from FUV vision of Butterfly
  Nebula NGC 6302
  The high excitation planetary nebula, NGC 6302, has been imaged in two
far-ultraviolet (FUV) filters, F169M (Sapphire; {\lambda}$_{\rm eff}$: 1608
{\AA}) and F172M (Silica; {\lambda}$_{\rm eff}$: 1717 {\AA}) and two NUV
filters, N219M (B15; {\lambda}$_{\rm eff}$: 2196 {\AA}) and N279N (N2;
{\lambda}$_{\rm eff}$: 2792 {\AA}) with the Ultra Violet Imaging Telescope
(UVIT). The FUV F169M image shows faint emission lobes that extend to about 5
arcmin on either side of the central source. Faint orthogonal collimated
jet-like structures are present on either side of the FUV lobes through the
central source. These structures are not present in the two NUV filters nor in
the FUV F172M filter. Optical and IR images of NGC 6302 show bright emission
bipolar lobes in the east-west direction with a massive torus of molecular gas
and dust seen as a dark lane in the north-south direction. The FUV lobes are
much more extended and oriented at a position angle of 113{\deg}. They and the
jet-like structures might be remnants of an earlier evolutionary phase, prior
to the dramatic explosive event that triggered the Hubble type bipolar flows
approximately 2200 years ago. The source of the FUV lobe and jet emission is
not known, but is likely due to fluorescent emission from H$_2$ molecules. The
cause of the difference in orientation of optical and FUV lobes is not clear
and, we speculate, could be related to two binary interactions.
