The ram pressure stripped radio tails of galaxies in the Coma cluster
  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 also enhanced relative to their IR emission by a factor of $\sim$2
compared to star-forming galaxies. The enhancement is likely related to ram
pressure and turbulence in the tail. 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.
