论文标题
凸起与触发性重质质量比与传奇星系的卫星数量之间的相关性的含义
Implications of the correlation between bulge-to-total baryonic mass ratio and the number of satellites for SAGA galaxies
论文作者
论文摘要
我们在类似银河系的宿主星系中搜索了卫星数量与基本银河系特性之间的相关性，以便更好地了解其不同的卫星种群。我们特别旨在了解为什么在恒星质量含量，星形形成率和当地环境中非常相似的星系具有非常不同的卫星。银河类似物（SAGA）光谱调查的卫星已经完成了其病毒半径中36个银河系样星系的光谱观测，直到Leo I Dwarf Galaxy的亮度。来自文献中的传奇星系的所有可用银河系特性以及测得的恒星质量与卫星数量相关，却没有发现显着相关性。但是，当我们考虑基于重型凸起与统计比率之间的相关性和卫星数量的“预期”数量时，确认了几个附近星系的卫星数量，那么该数量和（1）凸起的质量之间就出现了强相关性，（1）（1）（1）总特定角度动量。正如已经确认的那样，第一个相关性是积极的，这表明具有更大凸起的星系具有更多的卫星。与角动量的第二个相关性为负，这意味着，角动量越小，预期卫星的数量越大。这意味着，如果星系角动量太高，则不能形成卫星，或者该卫星内外形成，因此角动量被转移到星系的外部。但是，需要更深的光谱观测来确认这些发现，因为它们依赖于预期的而不是检测到的卫星数量。传奇调查等同于狮子银河系中的leo卫星的光度限制。
We searched for correlations between the number of satellites and fundamental galactic properties for the Milky Way-like host galaxies in order to better understand their diverse satellite populations. We specifically aim to understand why galaxies that are very similar in stellar mass content, star formation rate, and local environment have very different numbers of satellites. Satellites of Galactic Analogs (SAGA) spectroscopic survey has completed spectroscopic observations of 36 Milky Way-like galaxies within their virial radii down to the luminosity of Leo I dwarf galaxy. All the available galactic properties of SAGA galaxies from the literature along with measured stellar masses were correlated with the number of satellites and no significant correlation was found. However, when we considered the "expected" number of satellites based on the correlation between the baryonic bulge-to-total ratio and the number of satellites confirmed for several nearby galaxies then strong correlations emerge between this number and (1) the mass of the bulge, and (2) the total specific angular momentum. The first correlation is positive, implying that galaxies with more massive bulges have more satellites, as already confirmed. The second correlation with the angular momentum is negative, meaning that, the smaller the angular momentum, the greater the number of expected satellites. This would imply that either satellites cannot form if galaxy angular momentum is too high, or that satellites form inside-out, so that angular momentum is being transferred to the outer parts of the galaxies. However, deeper spectroscopic observations are needed to confirm these findings, because they rely on the expected rather than detected number of satellites. There was a luminosity limit to the SAGA survey equivalent to the luminosity of Leo I dwarf satellite of the Milky Way galaxy.
