LMC质量矮星的卫星：被Milky Way质量晕摧毁的近距离卫星
Satellites of LMC-Mass Dwarfs: Close Friendships Ruined by Milky Way Mass Halos
摘要：
受最近在大麦云（LMC）附近发现的几颗矮星的启发，我们利用ELVIS的N体模拟研究了大质量卫星在类银河系（MW）/M31晕上的吸积.我们确定了25个幸存的LMC质量的subhalos，并调查了与这些subhalos的低质量的卫星之前，他们落入MW/M31晕。通常，MW/M31晕的总z=0卫星群的7%在落入MW/M31晕之前在存活的LMC组中。该分数可以在1%和25%之间变化，对于具有较高质量和/或较近的坠落时间的组更高。卫星群在坠落后在相空间中迅速分散，在4-8 Gyr后，它们相对于群中心的距离和速度在统计上与整个卫星群相似。我们量化的可能性，卫星与LMC质量组作为相对于LMC在z=0的距离和速度的函数。9个暗能量巡天候选矮星系与大麦哲伦星系的距离非常接近，这表明~2-4可能与大麦哲伦星系有关。此外，如果这些矮星中有几个是真正的成员，那么LMC群可能是最近才落入MW的，<2 Gyr前。如果与大麦哲伦星系的联系是通过后续的速度测量建立起来的，那么这些“卫星的卫星”就代表了研究星系群预处理对低质量矮星影响的主要候选者。
英文摘要：
Motivated by the recent discovery of several dwarfs near the Large Magellanic Cloud (LMC), we study the accretion of massive satellites onto Milky Way (MW)/M31-like halos using the ELVIS suite of N-body simulations. We identify 25 surviving LMC-mass subhalos, and investigate the lower-mass satellites that were associated with these subhalos before they fell into the MW/M31 halos. Typically, 7% of the overall z=0 satellite population of MW/M31 halos were in a surviving LMC-group before falling into the MW/M31 halo. This fraction can vary between 1% and 25%, being higher for groups with higher mass and/or more recent infall times. Groups of satellites disperse rapidly in phase space after infall, and their distances and velocities relative to the group center become statistically similar to the overall satellite population after 4-8 Gyr. We quantify the likelihood that satellites were associated with an LMC-mass group as a function of both distance and velocity relative to the LMC at z=0. The close proximity in distance of the nine Dark Energy Survey candidate dwarf galaxies to the LMC suggest that ~2-4 are likely associated with the LMC. Furthermore, if several of these dwarfs are genuine members, then the LMC-group probably fell into the MW very recently, <2 Gyr ago. If the connection with the LMC is established with follow-up velocity measurements, these "satellites of satellites" represent prime candidates to study the affects of group pre-processing on lower mass dwarfs.
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