标题： 正在合并星系中的中性氢分布：恒星与气体潮汐形态之间的差异 显示英文标题

标题： The Neutral Hydrogen Distribution in Merging Galaxies: Differences between Stellar and Gaseous Tidal Morphologies

摘要： 我们已经绘制了三个盘状星系合并系统（NGC 520、Arp 220 和 Arp 299）中的中性原子气体（HI）分布图。这些系统与大多数在HI中绘制的合并系统不同，因为它们的恒星和气体潮汐特征并不重合。特别是，它们表现出大的恒星潮汐特征，但几乎没有伴随的中性气体；同时也有大量富含气体的潮汐特征，但几乎没有伴随的星光。在较小尺度上，存在明显的反相关关系，其中气体和恒星潮汐特征似乎相互交叉。我们探讨了导致这些差异的几种可能原因，包括尘埃遮蔽、冲击压力剥离和电离效应。没有单一的解释可以涵盖所有观察到的差异。这些系统中每个都显示出超风驱动的星暴正在朝着最显著的反相关方向扩展的事实使我们建议，超风可能是导致这些差异的主要原因，无论是通过冲击压力清除气体特征，还是通过挖掘一条通往星暴区域的清晰视线，允许紫外线光子电离尾部区域。 显示英文摘要

摘要： We have mapped the neutral atomic gas (HI) in the three disk-disk merger systems NGC 520, Arp 220, and Arp 299. These systems differ from the majority of the mergers mapped in HI, in that their stellar and gaseous tidal features do not coincide. In particular, they exhibit large stellar tidal features with little if any accompanying neutral gas and large gas-rich tidal features with little if any accompanying starlight. On smaller scales, there are striking anti-correlations where the gaseous and stellar tidal features appear to cross. We explore several possible causes for these differences, including dust obscuration, ram pressure stripping, and ionization effects. No single explanation can account for all of the observed differences. The fact that each of these systems shows evidence for a starburst driven superwind expanding in the direction of the most striking anti-correlations leads us to suggest that the superwind is primarily responsible for the observed differences, either by sweeping the features clear of gas via ram pressure, or by excavating a clear sightline towards the starburst and allowing UV photons to ionize regions of the tails.