FGC 1287和它神秘的250 kpc长的HI尾巴在阿贝尔1367的外围
FGC 1287 and its enigmatic 250 kpc long HI tail in the outskirts of Abell 1367
摘要：
我们提出了HI和无线电连续谱，窄带H $α$成像，IFU光谱，和X射线观测的FGC 1287三重投影$\sim$ 1.8 Mpc的星系团阿贝尔1367。一个三重态成员，FGC 1287，显示了一个非常长的，250 kpc的HI尾巴和一个未扰动的恒星盘，这是典型的冲压压力剥离（RPS）的标志。为了生成可检测的RPS特征，存在具有足够密度的簇内介质（ICM）/组内介质（IGM）以相对于ICM/IGM的实际速度产生RPS是先决条件。然而，XMM-牛顿观测无法探测到来自三重态的X射线发射，这意味着如果存在热ICM/IGM，其密度n ${_e}$小于2.6 $\times$ 10 $^{-5}$ cm $^{-3}$。这里提供的高分辨率VLA HI数据显示FGC 1287的HI盘被截断并显著弯曲，而HI尾部是cluperous。TNG H $α$成像确定了三个恒星形成的团块，投射在FGC 1287盘的20 kpc范围内，VIMOS-IFU数据证实其中两个是尾部HI团块的对应物。三重态的HI运动学，以及H $α$和无线电连续成像表明，相互作用可能增强了FGC 1287盘中的恒星形成，但不能轻易解释长HI尾的起源。我们考虑了几种可能使RPS与未检测到ICM/IGM X射线发射相一致的情况，但这些情况都不能明确解释长HI尾的起源。
英文摘要：
We present HI and radio continuum, narrow-band H$α$ imaging, IFU spectroscopy, and X-ray observations of the FGC 1287 triplet projected $\sim$ 1.8 Mpc west of the galaxy cluster Abell 1367. One triplet member, FGC 1287, displays an exceptionally long, 250 kpc HI tail and an unperturbed stellar disk which are the typical signatures of ram pressure stripping (RPS). To generate detectable RPS signatures the presence of an Intra-cluster medium (ICM)/intra-group medium (IGM) with sufficient density to produce RPS at a realistic velocity relative to the ICM/IGM is a prerequisite. However, XMM-Newton observations were not able to detect X-ray emission from the triplet, implying that if a hot ICM/IGM is present, its density, n${_e}$, is less than 2.6 $\times$ 10$^{-5}$ cm$^{-3}$. Higher-resolution VLA HI data presented here show FGC 1287's HI disk is truncated and significantly warped whereas the HI tail is clumpy. TNG H$α$ imaging identified three star forming clumps projected within 20 kpc of FGC 1287's disk, with VIMOS-IFU data confirming two of these are counterparts to HI clumps in the tail. The triplet's HI kinematics, together with H$α$ and radio continuum imaging suggests an interaction may have enhanced star formation in FGC 1287's disk, but cannot readily account for the origin of the long HI tail. We consider several scenarios which might reconcile RPS with the non-detection of ICM/IGM X-ray emission but none of these unambiguously explains the origin of the long HI tail.
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