动态测量的超大质量黑洞样本中的选择偏差：它的结果和对最基本关系的探索
Selection bias in dynamically-measured super-massive black hole samples: its consequences and the quest for the most fundamental relation
摘要：
我们比较了一组本地星系动态测量黑洞与一个大的，公正的样本从斯隆数字巡天星系。我们证实了早期的工作表明，大多数的黑洞主机有显着较高的速度色散σ比本地星系类似的恒星质量。我们使用蒙特卡罗模拟来说明黑洞标度关系的影响，如果这种偏见所产生的要求，黑洞的影响范围必须解决测量黑洞质量与空间分辨运动学。我们发现，这种选择效应人为地增加了至少~3倍的标准化的Mbh-Sigma关系的Mbh-Mstar关系的偏差甚至更大。我们的蒙特卡罗模拟和分析的残差标度关系都表明，西格玛是更根本的比Mstar或有效半径。特别地，Mbh-Mstar关系主要是Mbh-sigma和sigma-Mstar关系的结果，并且在小质量时严重偏置高达50倍。这有助于解决基于动力学的黑洞-星系比例关系与活动星系比例关系之间的差异。我们的模拟也不赞成广泛分布的黑洞质量在固定的西格玛。校正这种偏差表明，用于估计活动星系中黑洞质量的校准因子应减少到fvir~1的值。黑洞的质量密度也应该成比例地更小，这可能意味着辐射效率/黑洞自旋显着更高。减少黑洞质量也减少了预期从黑洞合并中得到的引力波信号。
英文摘要：
We compare the set of local galaxies having dynamically measured black holes with a large, unbiased sample of galaxies extracted from the Sloan Digital Sky Survey. We confirm earlier work showing that the majority of black hole hosts have significantly higher velocity dispersions sigma than local galaxies of similar stellar mass. We use Monte-Carlo simulations to illustrate the effect on black hole scaling relations if this bias arises from the requirement that the black hole sphere of influence must be resolved to measure black hole masses with spatially resolved kinematics. We find that this selection effect artificially increases the normalization of the Mbh-sigma relation by a factor of at least ~3; the bias for the Mbh-Mstar relation is even larger. Our Monte Carlo simulations and analysis of the residuals from scaling relations both indicate that sigma is more fundamental than Mstar or effective radius. In particular, the Mbh-Mstar relation is mostly a consequence of the Mbh-sigma and sigma-Mstar relations, and is heavily biased by up to a factor of 50 at small masses. This helps resolve the discrepancy between dynamically-based black hole-galaxy scaling relations versus those of active galaxies. Our simulations also disfavour broad distributions of black hole masses at fixed sigma. Correcting for this bias suggests that the calibration factor used to estimate black hole masses in active galaxies should be reduced to values of fvir~1. Black hole mass densities should also be proportionally smaller, perhaps implying significantly higher radiative efficiencies/black hole spins. Reducing black hole masses also reduces the gravitational wave signal expected from black hole mergers.
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