论文标题
黑洞积聚和星系中的恒星形成的共同进化至z = 3.5
Co-evolution of black hole accretion and star formation in galaxies up to z=3.5
论文作者
论文摘要
我们研究了不同星系生命阶段的黑洞积聚速率（BHAR）与恒星形成率（SFR）之间的共同进化：在不同宇宙时期，主要序列星形星系，静态和星爆骨星系。 我们利用了Chandra Cosmos-Legacy调查的X射线数据以及在COSMOS2015目录中呈现的COSMOS场中广泛的多波长辅助观测值。我们执行X射线堆叠分析，并以广泛的红移间隔（0.1 <z <3.5 $）将其与检测到的来源相结合。 X射线光度用于预测BHAR，而对远红外赫歇尔图的类似堆叠分析用于测量相应的SFR。 我们专注于平均SFR-Stellar质量（M*）关系的演变，并将其与BHAR-M*关系进行比较。我们发现，尽管它取决于恒星质量，但BHAR和SFR之间的比率并没有随红移而发展。对于形成明星的人群，对M*的依赖性具有$ \ sim0.6 $的对数斜率，对于$ \ sim0.4 $的Starburst样本，两者都与保持恒定的quiescent来源相矛盾（$ \ log log log（\ rm {bhar}/{bhar}/{\ rm sfr} \ rm sfr}）\ sim -3.4 $）通过研究特定的BHAR和特定的SFR，我们发现M*和Black Hole质量的缩减迹象（M $ _ {\ rm BH} $）：Quiescents在很早的时候就会增长其超级质量的黑洞，而Star-Forming和Starburst Galaxies的增值却持续了直到最近的时代。 我们的结果支持这样的想法，即相同的物理过程会进食并维持恒星形成和黑洞积聚。我们对M*-M $ _ {\ rm BH} $的关系的集成估计，在所有红移中都与对本地M*-M $ $ _ {\ rm BH} $的关系独立确定，因此将关键证据添加到BHAR/SFR的弱进化中，与BHAR/SFR的弱进化相比，与局部动态M $ $ _ $ _-M*-M*-M*-M*-M*-M*-M*-M*-M*-M*-M*-M*-M*-M*{
We study the co-evolution between the black hole accretion rate (BHAR) and the star formation rate (SFR) in different galaxy life phases: main sequence star-forming galaxies, quiescent and starburst galaxies at different cosmic epochs. We take advantage of the X-ray data from the Chandra COSMOS-Legacy survey and of the extensive multiwavelength ancillary observations in the COSMOS field presented in the COSMOS2015 catalog. We perform an X-ray stacking analysis and combine it with detected sources, in a broad redshift interval ($0.1<z<3.5$). The X-ray luminosity is used to predict the BHAR, while a similar stacking analysis on far-infrared Herschel maps is used to measure the corresponding SFR. We focus on the evolution of the average SFR-stellar mass (M*) relation and compare it with the BHAR-M* relation. We find that the ratio between BHAR and SFR does not evolve with redshift, although it depends on stellar mass. For the star-forming populations, this dependence on M* has a logarithmic slope of $\sim0.6$, for the starburst sample of $\sim0.4$, both at odds with quiescent sources where it remains constant ($\log(\rm {BHAR}/{\rm SFR})\sim -3.4$). By studying the specific BHAR and specific SFR we find signs of downsizing for both M* and black hole mass (M$_{\rm BH}$): quiescents grew their super-massive black hole at very early times, while star-forming and starburst galaxies had an accretion that endured until more recent times. Our results support the idea that the same physical processes feed and sustain both star formation and black hole accretion. Our integrated estimates of the M*-M$_{\rm BH}$ relation at all redshifts are consistent with independent determinations of the local M*-M$_{\rm BH}$ relation, thus adding key evidence to a weak evolution in the BHAR/SFR, and its low normalization compared to local dynamical M*-M$_{\rm BH}$ relations.
