Luminosity Functions and Host-to-host Scatter of Dwarf Satellite Systems in the Local Volume
Luminosity Functions and Host-to-host Scatter of Dwarf Satellite Systems in the Local Volume
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DOI：
10.3847/1538-4357/abd039
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发表时间：
2020-06
期刊：
影响因子：
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通讯作者：
S. Carlsten;J. Greene;A. Peter;R. Beaton;J. Greco
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文献类型：
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作者：
S. Carlsten;J. Greene;A. Peter;R. Beaton;J. Greco
类银河系低质量卫星是研究小尺度结构和星系形成的重要探针。然而，通过距离测量确认候选卫星仍然是当地卷（LV）快速进展的关键障碍。我们测量了最近编目的候选矮卫星周围的10个大质量主机在D < 12 Mpc的表面亮度波动距离，以确认关联。这些主机的卫星系统是完整的，并且在搜索足迹范围内，大部分污染物都被清除到M g-9到-10。加入这个样本与主机调查，以比较或更好的完整性在文献中，我们探讨如何以及宇宙学模拟结合常见的恒星晕质量关系（SHMR）匹配观测到的卫星光度函数在经典的卫星光度制度。采用与水动力学模拟相匹配的SHMR，我们发现预测的总体卫星丰度与观测结果吻合得很好。MW的光度函数在LV宿主中是非常典型的。我们发现，主机到主机的散射模型预测的是在密切的协议与所观察到的系统之间的散射，一旦观察到的系统的不同质量被考虑在内。然而，我们发现显着的证据表明，所观察到的系统有更多的明亮和更少的微弱的卫星比SHMR模型预测，可能需要更高的标准化的SHMR周围的晕质量1011兆或显着更大的散射比目前在常见的SHMR。这些结果表明附近的卫星系统在推断低质量制度的星系-晕下连接的效用。
Low-mass satellites around Milky Way (MW)-like galaxies are important probes of small-scale structure and galaxy formation. However, confirmation of satellite candidates with distance measurements remains a key barrier to fast progress in the Local Volume (LV). We measure the surface brightness fluctuation distances to recently cataloged candidate dwarf satellites around 10 massive hosts within D < 12 Mpc to confirm association. The satellite systems of these hosts are complete and mostly cleaned of contaminants down to M g ∼ −9 to −10, within the area of the search footprints. Joining this sample with hosts surveyed to comparable or better completeness in the literature, we explore how well cosmological simulations combined with common stellar to halo mass relations (SHMR) match observed satellite luminosity functions in the classical satellite luminosity regime. Adopting an SHMR that matches hydrodynamic simulations, we find that the predicted overall satellite abundance agrees well with the observations. The MW is remarkably typical in its luminosity function among LV hosts. We find that the host-to-host scatter predicted by the model is in close agreement with the scatter between the observed systems, once the different masses of the observed systems are taken into account. However, we find significant evidence that the observed systems have more bright and fewer faint satellites than the SHMR model predicts, possibly necessitating a higher normalization of the SHMR around halo masses of 1011 M ⊙ or significantly greater scatter than present in common SHMRs. These results demonstrate the utility of nearby satellite systems in inferring the galaxy–subhalo connection in the low-mass regime.