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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Supermassive black holes with higher Eddington ratios preferentially form in gas-rich galaxies
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Supermassive black holes with higher Eddington ratios preferentially form in gas-rich galaxies

机译：埃丁顿比率更高的超大分子黑洞优先形成富含瓦斯的星系

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摘要

The Eddington ratio (lambda(Edd)) of supermassive black holes (SMBHs) is a fundamental parameter that governs their cosmic growth. Although gas mass accretion onto SMBHs is sustained when they are surrounded by large amounts of gas, little is known about the molecular content of galaxies, particularly those hosting super-Eddington SMBHs (lambda(Edd) 1: the key phase of SMBH growth). Here, we have compiled reported optical and (CO)-C-12(1-0) data of local quasars to characterize their hosts. We found that higher lambda(Edd) SMBHs tend to reside in gas-rich (i.e., high gas mass to stellar mass fraction = f(gas)) galaxies. We used two methods to make this conclusion: one uses black hole mass as a surrogate for stellar mass by assuming a local co-evolutionary relationship, and the other directly uses stellar masses estimated from near-infrared observations. The f(gas)-lambda(Edd) correlation we found concurs with the cosmic decreasing trend in lambda(Edd), as cold molecular gas is primarily consumed by star formation. This correlation qualitatively matches predictions of recent semi-analytic models of the cosmic downsizing of SMBHs as well. As the gas mass surface density would eventually be a key parameter controlling mass accretion, we need high-resolution observations to identify further differences in the molecular properties around super-Eddington and sub-Eddington SMBHs.
机译：超大分料黑洞（SMBHS）的Eddington比（Lambda（EDD））是一个基本参数，管辖他们的宇宙增长。尽管当它们被大量气体包围时，虽然气体质量增加在SMBH上，但对于大量气体的分子含量，特别是托管Super-Eddington SMBHS（Lambda（EDD）＆ 1：SMBH生长的关键阶段）。在这里，我们编译了报告的光学和（CO）-C-12（1-0）本地标准物数据以表征其主机。我们发现较高的Lambda（EDD）SMBHs倾向于居住在富含气体（即，高气体物质到恒星质量分数= F（气体））星系。我们使用了两种方法来制定了这一结论：通过假设局部共同关系关系，一种使用黑洞质量作为替代品的替代品，另一种直接使用近红外观察估计的恒星群体。 F（气体）-Lambda（EDD）相关性我们发现在λ（EDD）中的宇宙率下降趋势，因为冷分子气主要由星形成消耗。这种相关性与SMBHS的宇宙缩小尺寸最近半分析模型的预测相匹配。随着气体质量表面密度最终是控制质量增生的关键参数，我们需要高分辨率观察，以识别超级埃丁顿和亚埃丁顿SMBHS周围的分子特性的进一步差异。

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