Abstract:
Spiral galaxies undergo strong ram-pressure effects when they fall into the galaxy cluster potential. As a consequence, their
gas is stripped to form extended tails within which star formation can happen, giving them the typical jellyfish appearance.
The ultraviolet imaging observations of jellyfish galaxies provide an opportunity to understand ongoing star formation in the
stripped tails. We report the ultraviolet observations of the jellyfish galaxies JW39, JO60, JO194 and compare with observations
in optical continuum and Hα. We detect knots of star formation in the disc and tails of the galaxies and find that their UV and Hα
flux are well correlated. The optical emission line ratio maps of these galaxies are used to identify for every region the emission
mechanism, due to either star formation, LINER or a mix of the two phenomena. The star-forming regions in the emission line
maps match very well with the regions having significant UV flux. The central regions of two galaxies (JW39, JO194) show a
reduction in UV flux which coincides with composite or LINER regions in the emission line maps. The galaxies studied here
demonstrate significant star formation in the stripped tails, suppressed star formation in the central regions and present a possible
case of accelerated quenching happening in jellyfish galaxies.
