Group pre-processing versus cluster ram-pressure stripping: the case of ESO156-G029. (arXiv:1909.01509v1 [astro-ph.GA])

Group pre-processing versus cluster ram-pressure stripping: the case of ESO156-G029. (arXiv:1909.01509v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dzudzar_R/0/1/0/all/0/1">Robert Dzudzar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kilborn_V/0/1/0/all/0/1">Virginia Kilborn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murugeshan_C/0/1/0/all/0/1">Chandrashekar Murugeshan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meurer_G/0/1/0/all/0/1">Gerhardt Meurer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sweet_S/0/1/0/all/0/1">Sarah M. Sweet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Putman_M/0/1/0/all/0/1">Mary Putman</a>

We report on observations of ESO156-G029, member of a galaxy group which is
positioned at the virial radius of cluster Abell 3193. ESO156-G029 is located ~
1.4 Mpc in projected distance from the brightest cluster galaxy NGC1500. We
show that ESO156-G029 has disturbed gas kinematics and a highly asymmetric
neutral hydrogen (HI) distribution, which are consequences of group
pre-processing, and possibly of ram-pressure. Based on the current data we
propose a scenario in which ESO156-G029 had a minor gas-rich merger in the past
and now starts to experience ram-pressure. We infer that the galaxy will
undergo rapid evolution once it gets closer to the cluster centre (less than
0.5 Mpc) where ram-pressure is strong enough to begin stripping the HI from the
galaxy.

http://arxiv.org/icons/sfx.gif