  We report LOFAR and VLA detections of extended radio emission in the spiral
galaxy HCG 97b, hosted by an X-ray bright galaxy group. The extended radio
emission detected at 144 MHz, 1.4 GHz and 4.86 GHz is elongated along the
optical disk and has a tail that extends 27 kpc in projection towards the
centre of the group at GHz frequencies or 60 kpc at 144 MHz. Chandra X-ray data
show two off-nuclear ultra-luminous X-ray sources (ULXs), with the farther one
being a plausible candidate for an accreting intermediate-mass black hole
(IMBH). The asymmetry observed in both CO emission morphology and kinematics
indicates that HCG 97b is undergoing ram-pressure stripping, with the leading
side at the southeastern edge of the disk. Moreover, the VLA 4.86 GHz image
reveals 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 linked
to ULX feedback. This hypothesis gains support from estimates showing that the
bulk velocity of the relativistic electrons needed for transport from the disk
to the tail is approximately $\sim 1300$ $\rm km~s^{-1}$. This velocity is much
higher than those observed in ram-pressure stripped galaxies ($100-600$ $\rm
km~s^{-1}$), implying an alternative mechanism aiding the stripping process.
Therefore, we conclude that HCG 97b is subject to ram pressure, with the
formation of its stripped radio tail likely influenced by the putative IMBH
activities.
