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首页> 外文期刊>The Astrophysical journal >Hα TAIL, INTRACLUSTER H Ⅱ REGIONS, AND STAR FORMATION: ESO 137-001 IN ABELL 3627
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Hα TAIL, INTRACLUSTER H Ⅱ REGIONS, AND STAR FORMATION: ESO 137-001 IN ABELL 3627

机译：Hα尾巴，Intraluster HⅡ区域和恒星形成：ABELL 3627中的ESO 137-001

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摘要

We present the discovery of a 40 kpc Hα tail and at least 29 emission-line objects downstream of a star-forming galaxy, ESO 137-001, in the rich, nearby cluster A3627. The galaxy is known to possess a dramatic 70 kpc X-ray tail. The detected Hα tail coincides positionally with the X-ray tail. The Ha emission in the galaxy is sharply truncated on the front and the sides near the nucleus, indicating significant ram pressure stripping. ESO 137-001 is thus the first cluster late-type galaxy known unambiguously to have both an X-ray tail and an Hα tail. The emission-line objects are all distributed downstream of the galaxy, with projected distances of up to 39 kpc from the galaxy. From the analysis on the Hα_(off) frame and the estimate of the background emission-line objects, we conclude that it is very likely that all 29 emission-line objects are H Ⅱ regions in A3627. The high surface number density and luminosities of these H Ⅱ regions (up to 10~(40) ergs s~(-1)) dwarf the previously known examples of isolated H Ⅱ regions in clusters. We suggest that star formation may proceed in the stripped ISM in both the galactic halo and intracluster space. The total mass of formed stars in the stripped ISM of ESO 137-001 may approach several times 10~7 M_☉. Therefore, stripping of the ISM not only contributes to the ICM, but also adds to the intracluster stellar light through subsequent star formation. The data also imply that ESO 137-001 is in an active stage of transformation accompanied by the buildup of a central bulge and depletion of the ISM.
机译：我们介绍了一个40 kpcHα尾巴和至少29个发射线物体的发现，该物体位于一个富裕的附近星团A3627中，由一个恒星形成星系ESO 137-001组成。已知该银河系拥有引人注目的70 kpc X射线尾巴。检测到的Hα尾巴在位置上与X射线尾巴重合。银河系中的Ha发射在靠近原子核的正面和侧面均被截断，表明显着的冲压压力剥离。因此，ESO 137-001是第一个星团晚期类型星系，明确知道它同时具有X射线尾巴和Hα尾巴。发射线物体全部分布在银河的下游，与银河的投影距离最大为39 kpc。通过对Hα_（off）框架的分析和背景发射线目标的估计，我们得出结论，很可能所有29个发射线目标都是A3627中的HⅡ区。这些HⅡ区的高表面数密度和发光度（高达10〜（40）ergs s〜（-1））使簇中孤立的HⅡ区的先前已知例子相形见.。我们建议恒星形成可能会在银河晕和星团内部空间的剥离ISM中进行。 ESO 137-001剥离的ISM中形成的恒星总质量可能接近10〜7M_☉的数倍。因此，ISM的剥离不仅有助于ICM，而且还通过随后的恒星形成而增加了星团内部的恒星光。数据还暗示，ESO 137-001处于转型的活跃阶段，伴随着中央凸起的形成和ISM的枯竭。

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