FGC 1287 and its enigmatic 250 kpc long HI tail in the outskirts of Abell 1367

We present HI and radio continuum, narrow-band H$\alpha$ imaging, IFU spectroscopy, X-ray observations of the FGC 1287 triplet projected $\sim$ 1.8 Mpc west galaxy cluster Abell 1367. One member, 1287, displays an exceptionally long, 250 kpc tail unperturbed stellar disk which are typical signatures ram pressure stripping (RPS). To generate detectable RPS presence Intra-cluster medium (ICM)/intra-group (IGM) with sufficient density to produce at a realistic velocity relative ICM/IGM is prerequisite. However, XMM-Newton were not able detect emission from triplet, implying that if hot present, its density, n${_e}$, less than 2.6 $\times$ 10$^{-5}$ cm$^{-3}$. Higher-resolution VLA data presented here show 1287's truncated significantly warped whereas clumpy. TNG imaging identified three star forming clumps within 20 disk, VIMOS-IFU confirming two these counterparts in tail. The triplet's kinematics, together continuum suggests interaction may have enhanced formation but cannot readily account for origin long consider several scenarios might reconcile non-detection none unambiguously explains