Active Galactic Nucleus Black Hole Masses and Bolometric Luminosities
Active Galactic Nucleus Black Hole Masses and Bolometric Luminosities
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DOI：
10.1086/342878
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发表时间：
2002-07
期刊：
影响因子：
--
通讯作者：
J. Woo;C. Urry
中科院分区：
文献类型：
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作者：
J. Woo;C. Urry
黑洞质量和质量吸积率是活动星系核(AGN)的基本性质。黑洞质量通过爱丁顿极限为活动星系核的能量学设定了近似的上限。我们收集并比较了所有来自文献的活动星系核黑洞质量估计值；这177个质量大多基于宽发射线的维里假设，宽线区域的大小由混响映射或光学光度确定。我们引入了200个额外的黑洞质量估计，基于宿主星系膨胀的性质，使用观测到的恒星速度色散或基本平面关系来推断σ；这些方法假设AGN宿主是正常星系。我们比较了36个用不同方法产生黑洞质量的例子，发现单个物体的散布高达几个数量级。方法越不直接，与其他估计的差异就越大，这可能是因为假设的潜在相关性存在很大的散布。利用已公布的通量，我们计算了234个活动星系核的辐射光度，并研究了黑洞质量与光度的关系。与其他研究相比，我们没有发现黑洞质量与光度的显著相关性，除了在估计黑洞质量时由循环推理引起的相关性。爱丁顿极限定义了亮度分布的近似上包络，但下包络完全取决于所包括的活动星系核的样本。对于任何给定的黑洞质量，爱丁顿比的范围最高可达3个数量级。
Black hole mass, along with mass accretion rate, is a fundamental property of active galactic nuclei (AGNs). Black hole mass sets an approximate upper limit to AGN energetics via the Eddington limit. We collect and compare all AGN black hole mass estimates from the literature; these 177 masses are mostly based on the virial assumption for the broad emission lines, with the broad-line region size determined from either reverberation mapping or optical luminosity. We introduce 200 additional black hole mass estimates based on properties of the host galaxy bulges, using either the observed stellar velocity dispersion or the fundamental plane relation to infer σ; these methods assume that AGN hosts are normal galaxies. We compare 36 cases for which black hole mass has been generated by different methods and find, for individual objects, a scatter as high as a couple of orders of magnitude. The less direct the method, the larger the discrepancy with other estimates, probably due to the large scatter in the underlying correlations assumed. Using published fluxes, we calculate bolometric luminosities for 234 AGNs and investigate the relation between black hole mass and luminosity. In contrast to other studies, we find no significant correlation of black hole mass with luminosity, other than those induced by circular reasoning in the estimation of black hole mass. The Eddington limit defines an approximate upper envelope to the distribution of luminosities, but the lower envelope depends entirely on the sample of AGNs included. For any given black hole mass, there is a range in Eddington ratio of up to 3 orders of magnitude.