The ram pressure stripped radio tails of galaxies in the Coma cluster. (arXiv:2004.06743v1 [astro-ph.GA])

The ram pressure stripped radio tails of galaxies in the Coma cluster. (arXiv:2004.06743v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Chen_H/0/1/0/all/0/1">Hao Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sun_M/0/1/0/all/0/1">Ming Sun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yagi_M/0/1/0/all/0/1">Masafumi Yagi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bravo_Alfaro_H/0/1/0/all/0/1">Hector Bravo-Alfaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brinks_E/0/1/0/all/0/1">Elias Brinks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kenney_J/0/1/0/all/0/1">Jeffrey Kenney</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Combes_F/0/1/0/all/0/1">Francoise Combes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sivanandam_S/0/1/0/all/0/1">Suresh Sivanandam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jachym_P/0/1/0/all/0/1">Pavel Jachym</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fossati_M/0/1/0/all/0/1">Matteo Fossati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gavazzi_G/0/1/0/all/0/1">Giuseppe Gavazzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boselli_A/0/1/0/all/0/1">Alessandro Boselli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nulsen_P/0/1/0/all/0/1">Paul Nulsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarazin_C/0/1/0/all/0/1">Craig Sarazin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ge_C/0/1/0/all/0/1">Chong Ge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yoshida_M/0/1/0/all/0/1">Michitoshi Yoshida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roediger_E/0/1/0/all/0/1">Elke Roediger</a>

Previous studies have revealed a population of galaxies in galaxy clusters
with ram pressure stripped (RPS) tails of gas and embedded young stars. We
observed 1.4 GHz continuum and HI emission with the Very Large Array in its
B-configuration in two fields of the Coma cluster to study the radio properties
of RPS galaxies. The best continuum sensitivities in the two fields are 6 and 8
$mu$Jy per 4” beam respectively, which are 4 and 3 times deeper than those
previously published. Radio continuum tails are found in 10 (8 are new) out of
20 RPS galaxies, unambiguously revealing the presence of relativistic electrons
and magnetic fields in the stripped tails. Our results also hint that the tail
has a steeper spectrum than the galaxy. The 1.4 GHz continuum in the tails is
enhanced relative to their H$alpha$ emission by a factor of $sim$7 compared
to the main bodies of the RPS galaxies. The 1.4 GHz continuum of the RPS
galaxies is enhanced relative to their IR emission by a factor of $sim$2
compared to star-forming galaxies. The ram pressure interaction may enhanced
the radio emission of the RPS galaxies, the tails were further enhanced for the
stripping. We furthermore present HI detections in three RPS galaxies and upper
limits for the other RPS galaxies. The cold gas in D100’s stripped tail is
dominated by molecular gas, which is likely a consequence of the high ambient
pressure. No evidence of radio emission associated with ultra-diffuse galaxies
is found in our data.

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