论文标题
揭示黑洞生长与星形星系之间的宿主 - 半紧凑性之间的关系
Revealing the relation between black-hole growth and host-galaxy compactness among star-forming galaxies
论文作者
论文摘要
最近的研究表明，黑洞（BH）生长与恒星质量（$ M_ \ BIGSTAR $）或星形形成率（SFR）之间的普遍关系是对BH-Galaxy共同进化的过度简化，并且还必须考虑宿主星系的形态和结构特性。特别是，在恒星形成（SF）星系中确定了BH生长与宿主 - 半紧凑度之间的可能联系。利用$ \ 6300 $的大规模星系和$ i _ {\ rm 814W} 〜24 $在$ z $ $ $ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <$ <在控制形态和$ M_ \ BIGSTAR $（或SFR）时。在我们的研究中，使用预计的中央表面质量密度在1 kpc（$σ_{1} $）内代表宿主 - 果实紧凑性。我们发现，$ \ rm \ Overline {bhar} $ - $σ_{1} $关系比$ \ rm \ rm \ overline {bhar} $ - $ m_ \ bigstar $或$ \ bigStar $或$ \ rm \ rm \ rm \ rm \ rm \ overline {bhar} $ - sfreline and sf-sf-sf-sf-sf-sf Galaxies和sf Galaxies和sf Galaxies and \ \ \ \ \ \ \ c \ rm \ rm crm \ edline {bhar} $ - $σ_{1} $关系适用于不受凸起主导的凸起主导的星系和星系。这个$ \ rm \ Overline {Bhar} $ - $σ_{1} $之间的关系表明，KPC量表上BH增长与宿主星系的中央气体密度之间存在联系，这可能进一步暗示BH的气体在BH的VICINITY和中央$ sim $ sim $ KPC中的共同起源。这个$ \ rm \ edline {bhar} $ - $σ_{1} $关系也可以解释为BH增长与给定气体含量的主机星系的中央速度分散之间的关系，这表明主机 - 纳克斯电位在调节BH上的宿主 - 循环电位孔的作用。
Recent studies show that a universal relation between black-hole (BH) growth and stellar mass ($M_\bigstar$) or star formation rate (SFR) is an oversimplification of BH-galaxy co-evolution, and that morphological and structural properties of host galaxies must also be considered. Particularly, a possible connection between BH growth and host-galaxy compactness was identified among star-forming (SF) galaxies. Utilizing $\approx 6300$ massive galaxies with $I_{\rm 814W}~<~24$ at $z$ $<$ 1.2 in the COSMOS field, we perform systematic partial-correlation analyses to investigate how sample-averaged BH accretion rate ($\rm \overline{BHAR}$) depends on host-galaxy compactness among SF galaxies, when controlling for morphology and $M_\bigstar$ (or SFR). The projected central surface-mass density within 1 kpc, $Σ_{1}$, is utilized to represent host-galaxy compactness in our study. We find that the $\rm \overline{BHAR}$-$Σ_{1}$ relation is stronger than either the $\rm \overline{BHAR}$-$M_\bigstar$ or $\rm \overline{BHAR}$-SFR relation among SF galaxies, and this $\rm \overline{BHAR}$-$Σ_{1}$ relation applies to both bulge-dominated galaxies and galaxies that are not dominated by bulges. This $\rm \overline{BHAR}$-$Σ_{1}$ relation among SF galaxies suggests a link between BH growth and the central gas density of host galaxies on the kpc scale, which may further imply a common origin of the gas in the vicinity of the BH and in the central $\sim$ kpc of the galaxy. This $\rm \overline{BHAR}$-$Σ_{1}$ relation can also be interpreted as the relation between BH growth and the central velocity dispersion of host galaxies at a given gas content, indicating the role of the host-galaxy potential well in regulating accretion onto the BH.
