论文标题
星系猝灭中的特征质量：环境与内部效果
Characteristic mass in galaxy quenching: environmental versus internal effects
论文作者
论文摘要
在恒星质量的多参数空间（$ m _*$），凸起的总质量比（$ b/t _ {\ rm m} $），halo mass（$ m _ {\ m _ {\ rm h} $）和卤代居中（$ r _ r/r r _ r _ r _ r _ 180}）。对于给定的光环质量，对于过渡的特征性恒星质量（$ m _ {*，\ rm ch} $）约为相应的中央星系的五分之一，几乎独立于$ b/t _ {\ rm m m} $。一旦修复了$ b/t _ {\ rm m} $，就会用$ m _ {*} <m _ {*，\ rm ch} $增加星系的淬火部分，随着$ m _ {\ rm h} $的增加而增加，但用$ m _*$减少了$ m _*$ in Balos of Halos（$ r/r/r/r/r/r/r/r/r/r/r r _的内部）。在外部部分（$ r/r_ {180}> 0.5 $）中，$ m _ {\ rm h} $的趋势仍然存在，但与$ m _*$的相关性是不存在的，或者是正面的。对于$ m _ {\ rm *，ch} $的星系，并且固定$ b/t _ {\ rm m} $固定的$ m _ {\ rm *} $增加，但仅依赖于$ m _ {\ rm *} $，但仅依赖于$ m _ {\ m _ {\ rm h} $。在固定的$ b/t _ {\ rm m} $和$ m _*$的情况下，淬火分数增加，随着$ r/r_ {180} $的减少，带有$ m _ {*} <m _ {*} <m _ {*，\ rm ch} $的星系$，仅对$ r/r/r/r/r _} $ {180} $ {180} m _ {*，\ rm ch} $。我们的发现提供了一种物理动机的方法，将Halos中的星系分类为两个类别的淬火属性：带有$ M _ { *}> M _ { *}> m _ {\ rm *，ch} $的“上层类”和$ m _ { *} <m _ {环境淬火对于“下层”星系很重要，而内部淬火对“上层阶级”起了主导作用。
A clear transition feature of galaxy quenching is identified in the multi-parameter space of stellar mass ($M_*$), bulge to total mass ratio ($B/T_{\rm m}$), halo mass ($M_{\rm h}$) and halo-centric distance ($r/r_{180}$). For given halo mass, the characteristic stellar mass ($M_{*, \rm ch}$) for the transition is about one-fifth of that of the corresponding central galaxy, and almost independent of $B/T_{\rm m}$. Once $B/T_{\rm m}$ is fixed, the quenched fraction of galaxies with $M_{*} < M_{*, \rm ch}$ increases with $M_{\rm h}$, but decreases with $M_*$ in the inner part of halos ($r/r_{180} < 0.5$). In the outer part ($r/r_{180} > 0.5$), the trend with $M_{\rm h}$ remains but the correlation with $M_*$ is absent or becomes positive. For galaxies above $M_{\rm *, ch}$ and with $B/T_{\rm m}$ fixed, the quenched fraction increases with $M_{\rm *}$, but depends only weakly on $M_{\rm h}$ in both the inner and outer regions. At fixed $B/T_{\rm m}$ and $M_*$, the quenched fraction increases with decreasing $r/r_{180}$ for galaxies with $M_{*} < M_{*, \rm ch}$, and depends only weakly on $r/r_{180}$ for galaxies with $M_{*} > M_{*, \rm ch}$. Our finding provides a physically-motivated way to classify galaxies in halos into two classes based on their quenching properties: an `upper class' with $M_{*} > M_{\rm *,ch}$ and a `lower class' with $M_{*} < M_{\rm *,ch}$. Environmental quenching is important for `lower class' galaxies, while internal quenching plays the dominating role for the `upper class'.
