Photometric mass estimation and the stellar mass–halo mass relation for low mass galaxies
Photometric mass estimation and the stellar mass–halo mass relation for low mass galaxies
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低质量星系的光度质量估计和恒星质量-晕质量关系
DOI：
10.1093/mnras/stac3610
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发表时间：
2022
影响因子：
4.8
通讯作者：
Behroozi, Peter
中科院分区：
文献类型：
--
作者：
Zaritsky, Dennis;Behroozi, Peter
我们提出了一个光度晕质量估计技术的本地星系，使我们能够建立恒星质量晕质量（SMHM）的关系下降到恒星质量的105 M。我们发现没有检测到的差异SMHM关系的四个本地星系团或集群和场之间的关系，我们发现与以前的SMHM关系使用丰度匹配的方法得出的外推协议。我们将幂律拟合到经验SMHM关系式中，发现对于采用的NFW暗物质剖面，当M *<109 M时，晕质量为Mh = 1010.35 ± 0.02（M*/108 M）0.63 ± 0.02。这种关系的归一化容易受到系统建模误差的影响，这些误差取决于所采用的暗物质势，所引用的不确定性指的是中值关系中的不确定性。对于满足我们选择标准的M *<109 M的星系，Mh拟合的离散度，包括我们方法产生的不确定性，为0.3 dex。最后，我们把较低的光度本星系群的SMHM关系使用相同的技术，扩展到M *<$103 M <$，并建议，这些星系中的一些显示出额外的质量内部的有效半径超出了标准的暗物质配置文件提供的证据。如果这个质量是以中心黑洞的形式存在，那么黑洞的质量就在中等质量黑洞的范围内，10（5.7 ± 0.6）M，相当于Mh的百分之几，远高于从描述更大质量星系的关系式中推断出来的值。
We present a photometric halo mass estimation technique for local galaxies that enables us to establish the stellar mass–halo mass (SMHM) relation down to stellar masses of 105M⊙. We find no detectable differences among the SMHM relations of four local galaxy clusters or between the cluster and field relations and we find agreement with extrapolations of previous SMHM relations derived using abundance matching approaches. We fit a power law to our empirical SMHM relation and find that for adopted NFW dark matter profiles and forM*< 109M⊙, the halo mass isMh= 1010.35 ± 0.02(M*/108M⊙)0.63 ± 0.02. The normalization of this relation is susceptible to systematic modelling errors that depend on the adopted dark matter potential and the quoted uncertainties refer to the uncertainties in the median relation. For galaxies withM*< 109M⊙that satisfy our selection criteria, the scatter about the fit inMh, including uncertainties arising from our methodology, is 0.3 dex. Finally, we place lower luminosity Local Group galaxies on the SMHM relationship using the same technique, extending it toM*∼ 103M⊙and suggest that some of these galaxies show evidence for additional mass interior to the effective radius beyond that provided by the standard dark matter profile. If this mass is in the form of a central black hole, the black hole masses are in the range of intermediate mass black holes, 10(5.7 ± 0.6)M⊙, which corresponds to masses of a few percent ofMh, well above values extrapolated from the relationships describing more massive galaxies.