Abstract
ABSTRACT 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 H i 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 µJy per 4 arcsec 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 α emission by a factor of ∼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 infrared emission by a factor of ∼2 compared to star-forming galaxies. The enhancement is likely related to ram pressure and turbulence in the tail. We furthermore present H i 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.
Highlights
Ram pressure stripped (RPS) galaxies are characterized by gas being stripped from the affected galaxy by the intracluster medium (ICM; e.g. Gunn & Gott 1972; Nulsen 1982)
We investigate if the observed radio continuum emission is mainly related to Star formation (SF) in the tail or due to relativistic electrons that were stripped from the galaxy by ram pressure
H α surface brightness (SB) values for the same tail/galaxy regions are estimated from the Subaru data as in Yagi et al (2017), except that of KUG 1258+279A which is from GOLDMine
Summary
Ram pressure stripped (RPS) galaxies are characterized by gas being stripped from the affected galaxy by the intracluster medium (ICM; e.g. Gunn & Gott 1972; Nulsen 1982). Ram pressure stripped (RPS) galaxies are characterized by gas being stripped from the affected galaxy by the intracluster medium Star formation (SF) can be triggered by ram pressure at the early interaction stage by compression of interstellar medium (ISM), as shown in observations and simulations Ram pressure stripping is an important process affecting galaxy evolution in rich environments like galaxy groups and clusters. The mixing of the stripped cold ISM with the hot ICM will produce a multiphase gas Some of the stripped ISM can turn into stars in the galactic halo and the intracluster space (e.g. Cortese et al 2007; Sun et al 2007; Owers et al 2012; Ebeling, Stephenson & Edge 2014; Cramer et al 2019), especially in the high ICM pressure environment Stripped tails emerge as ideal targets to study this multiphase medium and SF conditions in an extreme environment
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