arXiv 1810.048882018-10astro-ph.GA

螺旋星系的黑洞质量标度关系。II。$M_{\rm BH}$ - $M_{\rm ,tot}$和$M_{\rm BH}$ - $M_{\rm ,disk}$

Black Hole Mass Scaling Relations for Spiral Galaxies. II. $M_{\rm BH}$-$M_{\rm *,tot}$ and $M_{\rm BH}$-$M_{\rm *,disk}$

Benjamin L. Davis, Alister W. Graham, Ewan Cameron

备注：: 21 pages, 13 figures, and 4 tables
发表信息：: Davis, B. L., Graham, A. W., & Cameron, E. 2018, ApJ, 869, 113
DOI：: 10.3847/1538-4357/aae820

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摘要：

黑洞质量（$M_{BH}$）的标度关系通常是使用星系的膨胀和样本（高质量）的早期类型的星系为主的属性。研究晚型星系应该可以更深入地了解黑洞和星系在更富含气体的环境中的相互生长。我们已经用40个旋涡星系来确定$M_{BH}$如何与总恒星质量（$M_{*,tot}$）和盘的恒星质量成比例，测量了球状体（凸起）恒星质量（$M_{*,sph}$），并在论文I中提出了$M_{BH}$ - $M_{*,sph}$关系。涉及$M_{*,tot}$的关系对于从管线数据或在较高红移下估计$M_{BH}$可能是有益的，所述较高红移条件对于凸起的精确隔离不是理想的。对称贝叶斯分析找到$\log\left(M_{BH}/M_{\odot}\right)=\left(3.05_{-0.49}^{+0.57}\right)\log\left\{M_{*,tot}/[\upsilon(6.37\times10^{10}\,M_{\odot})]\right\}+(7.25_{-0.14}^{+0.13})$。$M_{BH}$对$M_{*,tot}$回归的散点为0.66 dex;比较$M_{BH}$对$M_{*,sph}$的0.56 dex和$0.57$对$M_{BH}$对$σ_*$的0.56 dex。该斜率是用核心-Sérsic早型星系得到的$>2$倍，与用$M_{*,sph}$得到的结果相似，支持不同形态类型星系的生长机制不同。这种陡峭的关系对星系/黑洞形成理论、模拟和预测黑洞质量都有影响。我们要注意的是：（i）由早型和晚型星系的混合物建立的$M_{BH}$ - $M_{*,tot}$关系会发现一个约为1-3的任意斜率，除了样本选择之外没有任何物理意义，（ii）$M_{BH}$ - $M_{*,tot}$关系的演化研究需要注意每个时期包括的星系类型。我们还更新了$M_{*,tot}$ -（$\textit{face-on}$螺旋臂节距角）关系。

英文摘要：

Black hole mass ($M_{BH}$) scaling relations are typically derived using the properties of a galaxy's bulge and samples dominated by (high-mass) early-type galaxies. Studying late-type galaxies should provide greater insight into the mutual growth of black holes and galaxies in more gas-rich environments. We have used 40 spiral galaxies to establish how $M_{BH}$ scales with both the total stellar mass ($M_{*,tot}$) and the disk's stellar mass, having measured the spheroid (bulge) stellar mass ($M_{*,sph}$) and presented the $M_{BH}$-$M_{*,sph}$ relation in Paper I. The relation involving $M_{*,tot}$ may be beneficial for estimating $M_{BH}$ either from pipeline data or at higher redshift, conditions that are not ideal for the accurate isolation of the bulge. A symmetric Bayesian analysis finds $\log\left(M_{BH}/M_{\odot}\right)=\left(3.05_{-0.49}^{+0.57}\right)\log\left\{M_{*,tot}/[\upsilon(6.37\times10^{10}\,M_{\odot})]\right\}+(7.25_{-0.14}^{+0.13})$. The scatter from the regression of $M_{BH}$ on $M_{*,tot}$ is 0.66 dex; compare 0.56 dex for $M_{BH}$ on $M_{*,sph}$ and $0.57$ dex for $M_{BH}$ on $σ_*$. The slope is $>2$ times that obtained using core-Sérsic early-type galaxies, echoing a similar result involving $M_{*,sph}$, and supporting a varied growth mechanism among different morphological types. This steeper relation has consequences for galaxy/black hole formation theories, simulations, and predicting black hole masses. We caution that (i) an $M_{BH}$-$M_{*,tot}$ relation built from a mixture of early- and late-type galaxies will find an arbitrary slope of approximately 1-3, with no physical meaning beyond one's sample selection, and (ii) evolutionary studies of the $M_{BH}$-$M_{*,tot}$ relation need to be mindful of the galaxy types included at each epoch. We additionally update the $M_{*,tot}$-($\textit{face-on}$ spiral arm pitch angle) relation.

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