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We report LOFAR and VLA detections of extended radio emission in the spiralgalaxy HCG 97b, hosted by an X-ray bright galaxy group. The extended radioemission detected at 144 MHz, 1.4 GHz and 4.86 GHz is elongated along theoptical disk and has a tail that extends 27 kpc in projection towards thecentre of the group at GHz frequencies or 60 kpc at 144 MHz. Chandra X-ray datashow two off-nuclear ultra-luminous X-ray sources (ULXs), with the farther onebeing a plausible candidate for an accreting intermediate-mass black hole(IMBH). The asymmetry observed in both CO emission morphology and kinematicsindicates that HCG 97b is undergoing ram-pressure stripping, with the leadingside at the southeastern edge of the disk. Moreover, the VLA 4.86 GHz imagereveals two bright radio blobs near one ULX, aligning with the disk and tail,respectively. The spectral indices in the disk and tail are comparable and flat($\alpha > -1$), suggesting the presence of recent outflows potentially linkedto ULX feedback. This hypothesis gains support from estimates showing that thebulk velocity of the relativistic electrons needed for transport from the diskto the tail is approximately $\sim 1300$ $\rm km~s^{-1}$. This velocity is muchhigher than those observed in ram-pressure stripped galaxies ($100-600$ $\rmkm~s^{-1}$), implying an alternative mechanism aiding the stripping process.Therefore, we conclude that HCG 97b is subject to ram pressure, with theformation of its stripped radio tail likely influenced by the putative IMBHactivities.

Ram-pressure stripped radio tail and two ULXs in the spiral galaxy HCG 97b