论文标题
低质量星系的光度质量估计和恒星质量质量关系
Photometric Mass Estimation and the Stellar Mass-Halo Mass Relation for Low Mass Galaxies
论文作者
论文摘要
我们为局部星系提供了一项光度光量质量估计技术，使我们能够建立出色的质量质量质量质量（SMHM）关系，至10 $^5 $ m $ _ \ odot $的恒星质量。我们发现四个局部星系群的SMHM关系之间或群集和现场关系之间没有可检测的差异，我们发现使用丰度匹配方法得出的先前SMHM关系的推断一致。我们适合我们的经验SMHM关系，发现对于采用NFW暗物质配置文件，对于M $ _* <10^9 $ m $ _ \ odot $，Halo Mass为m $ _H = 10^{10.35 \ pm0.02} m} _ \ odot）^{0.63 \ pm0.02} $。这种关系的归一化易受取决于所采用的暗物质潜力的系统建模错误，引用的不确定性是指中位数关系中的不确定性。对于满足我们的选择标准的M $ _* <10^{9} $ m $ _ \ odot $的星系，大约在$ m_h $中的散布，包括我们方法论引起的不确定性，为0.3 dex。最后，我们使用相同的技术将较低的亮度本地组的星系放在SMHM关系上，将其扩展到m $ _* \ sim 10^3 $ m $ _ \ odot $，并建议其中一些星系显示出证据表明有效的半径是额外的质量内部，超出了标准暗物质配置。如果该质量是中央黑洞的形式，则黑洞质量在中间质量的黑洞范围内，$ 10^{（5.7 \ pm0.6）} $ M $ _ \ odot $，对应于几个M $ _H $的群众，远远超过了描述更多大型星系的人际关系中的价值观。
We present a photometric halo mass estimation technique for local galaxies that enables us to establish the stellar mass-halo mass (SMHM) relation down to stellar masses of 10$^5$ M$_\odot$. 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 for M$_* < 10^9$ M$_\odot$, the halo mass is M$_h = 10^{10.35\pm0.02}({\rm M}_*/10^8 {\rm M}_\odot)^{0.63\pm0.02}$. The normalisation 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 with M$_* < 10^{9}$ M$_\odot$ that satisfy our selection criteria, the scatter about the fit in $M_h$, 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 to M$_* \sim 10^3$ M$_\odot$ 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, $10^{(5.7\pm0.6)}$ M$_\odot$, which corresponds to masses of a few percent of M$_h$, well above values extrapolated from the relationships describing more massive galaxies.
