论文标题
使用祖细胞质量在不同的红移时匹配的subhalo丰度：两种恒星质量生长印在Subaru HSC Galaxy群集中
Subhalo abundance matching using progenitor mass at varying redshift: Two modes of stellar mass growth imprinted into the Subaru HSC galaxy clustering
论文作者
论文摘要
我们提出了一种新型的subhalo丰度匹配（假）模型，该模型使用每个（子）光环$ m _ {\ rm prog} $的主祖细胞的病毒质量作为观察时的星系恒星质量$ m _*$的代理。此$ m _ {\ rm prog} $模型模型可预测两点相关功能，具体取决于$ m_ \ mathrm {prog} $的时代$ z _ {\ rm prog} $的选择。以$ z {\ rm prog} $作为拟合参数，我们将$ m _ {\ rm prog} $模型应用于用$ m _ { $ 10^{8.6} $使用Subaru Hyper Soprime-Cam调查中的$ z \ simeq0.4 $的星系样本。 $ m _ {\ rm prog} $模型可以重现观测值，超过$ 10〜H^{ - 1} {\ rm kpc} \ textrm { - } 10〜h^{ - 1} { - 1} {\ rm mpc} $。我们发现，对于$ 10^{9.2} \ leq m _ {*，〜{\ rm lim}}}/（h^{ - 2} m_ \ odot）\ leq10^{10.2 {10.2} $，相关性功能由大量使用的$ v _ empl ampl ampl ampl and ampl andud andud， $ \ Lessim1〜H^{ - 1} {\ rm mpc} $，这表明$ M _ {\ rm prog} $比传统$ v _ {\ rm peacs} $更好地代表星系恒星质量。 The $z_{\rm prog}$ parameter is highest ($z_{\rm prog}\simeq3$) for intermediate mass galaxies at $M_*\simeq10^{9.9}~h^{-2}M_\odot$, and becomes smaller down to $z_\mathrm{prog}\simeq1$ for both lower- and高质量星系。我们将这些趋势解释为反映了低质量星系中原位恒星形成的缩小尺寸，以及在高质量星系中前势恒星质量增长的较大贡献。
We propose a novel subhalo abundance matching (SHAM) model that uses the virial mass of the main progenitor of each (sub)halo $M_{\rm prog}$ as a proxy of the galaxy stellar mass $M_*$ at the time of observation. This $M_{\rm prog}$ model predicts the two-point correlation functions depending on the choice of the epoch $z_{\rm prog}$ at which $M_\mathrm{prog}$ is quoted. With $z_{\rm prog}$ as a fitting parameter, we apply the $M_{\rm prog}$ model to the angular correlation functions measured with varying stellar mass thresholds from $M_{*,~{\rm lim}}/(h^{-2}M_\odot)=10^{11}$ to $10^{8.6}$ using a sample of galaxies at $z\simeq0.4$ from the Subaru Hyper Suprime-Cam survey. The $M_{\rm prog}$ model can reproduce the observations very well over $10~h^{-1}{\rm kpc}\textrm{--}10~h^{-1}{\rm Mpc}$. We find that, for the samples of $10^{9.2}\leq M_{*,~{\rm lim}}/(h^{-2}M_\odot)\leq10^{10.2}$, the correlation functions predicted by the widely-used $V_{\rm peak}$ model lack amplitudes at $\lesssim1~h^{-1}{\rm Mpc}$, suggesting that $M_{\rm prog}$ is a better proxy of the galaxy stellar mass than conventional $V_{\rm peak}$. The $z_{\rm prog}$ parameter is highest ($z_{\rm prog}\simeq3$) for intermediate mass galaxies at $M_*\simeq10^{9.9}~h^{-2}M_\odot$, and becomes smaller down to $z_\mathrm{prog}\simeq1$ for both lower- and higher-mass galaxies. We interpret these trends as reflecting the downsizing in the in-situ star formation in lower-mass galaxies and the larger contribution of the ex-situ stellar mass growth in higher-mass galaxies.
