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One triplet member, FGC\u20091287, displays an exceptionally long, 250\u2009kpc H\u2009i tail and an unperturbed stellar disc which are the typical signatures of ram pressure stripping (RPS). To generate detectable RPS signatures the presence of an Intracluster medium ICM or intragroup medium IGM with sufficient density to produce RPS at a realistic velocity relative to the ICM or IGM is a prerequisite. However, XMM\u2013Newton observations were not able to detect X-ray emission from the triplet, implying that if a hot ICM\/IGM is present, its density, ne, is less than 2.6\u00a0\u00d7\u00a010\u22125\u2009cm\u22123. Higher resolution VLA H\u2009i data presented here show FGC\u20091287\u2019s H\u2009i disc is truncated and significantly warped, whereas the H\u2009i tail is clumpy. TNG H\u03b1 imaging identified three star-forming clumps projected within 20\u00a0kpc of FGC\u20091287\u2019s disc, with VIMOS\u2013IFU data confirming two of these are counterparts to H\u2009i clumps in the tail. The triplet\u2019s H\u2009i kinematics, together with H\u03b1 and radio continuum imaging suggests an interaction may have enhanced star formation in FGC\u20091287\u2019s disc, but cannot readily account for the origin of the long H\u2009i tail. 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