论文标题
探测淬火与形态演化之间的联系
Probing the link between quenching and morphological evolution
论文作者
论文摘要
我们使用星系形成的半分析模型比较了两个淬火方案的预测：光晕淬灭和黑洞（BH）淬火。校准了这两种模型以使它们符合星系的质量功能后，BH淬火与被动星系的比例更好地一致，这是恒星质量$ M _*$的函数，以及星系形态分布在星形形态比率上与$ M _*$ _*$图。除了这一主要发现外，这项研究还有另外两个结果。首先，成功的BH猝灭模型要求较小的合并有助于超级BHS的增长。如果通过重复的未成熟合并达到高$ m _*$的星系没有被淬灭，那么高质量的蓝色星系太多了。其次，合并中BHS的增长必须在低质量下的效率降低，以便重现$ m _ {\ rm bh} $ - $ m _*$关系和被动分数，而被动分数则是$ m _*$的函数，与超级NOVAE的想法相吻合，即超级NOVAE可预防较低升级速度的SyperNovae BH增长。我们的发现与类星体反馈的情况一致，在这种情况下，BHS生长直到它们足够巨大以使其宿主星系中的冷气吹走，并将热的环境培养基加热到如此高的熵，以至于其冷却时间很长。他们还支持这样的观念，即淬火和维护对应于不同的反馈制度。
We use a semianalytic model of galaxy formation to compare the predictions of two quenching scenarios: halo quenching and black-hole (BH) quenching. After calibrating both models so that they fit the mass function of galaxies, BH quenching is in better agreement with the fraction of passive galaxies as a function of stellar mass $M_*$ and with the galaxy morphological distribution on a star-formation-rate vs. $M_*$ diagram. Besides this main finding, there are two other results from this research. First, a successful BH-quenching model requires that minor mergers contribute to the growth of supermassive BHs. If galaxies that reach high $M_*$ through repeated minor mergers are not quenched, there are too many blue galaxies at high masses. Second, the growth of BHs in mergers must become less efficient at low masses in order to reproduce the $M_{\rm BH}$--$M_*$ relation and the passive fraction as a function of $M_*$, in agreement with the idea that supernovae prevent efficient BH growth in systems with low escape speeds. Our findings are consistent with a quasar-feedback scenario in which BHs grow until they are massive enough to blow away the cold gas in their host galaxies and to heat the hot circumgalactic medium to such high entropy that its cooling time becomes long. They also support the notion that quenching and maintenance correspond to different feedback regimes.
