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arXiv 0705.1165astro-ph
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超大质量黑洞质量的宿主星系膨胀预测

Host Galaxy Bulge Predictors of Supermassive Black Hole Mass

M. C. Aller, D. O. Richstone

备注：
accepted for publication in ApJ
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摘要：

各种宿主星系（隆起）的参数进行检查，以确定其预测能力，在确定质量的超大质量黑洞（SMBH）在星系中心。基于一个23个邻近星系的样本，包括椭圆星系和螺旋/透镜状凸起，我们确定了一个强烈的相关性之间的凸起引力结合能（$E_g$），跟踪的恒星光剖面，和SMBH质量（$M_{\bullet}$），这样$M_{\bullet} \propto E_g^{0.6}$。这种关系的离散性表明，对于椭圆星系子样本，这与速度色散（$σ$）一样是$M_{\bullet}$的强预测因子。改进的质光比，获得与IFU光谱学和I波段测光的SAURON集团，被用于这些样本星系在可用的地方，导致在能量预测具有相同的斜率，但减少了散射。替代$M_{\bullet}$预测，如引力势和隆起的质量也进行了探讨，但这些被发现是劣质的隆起的引力结合能和隆起的速度色散预测相比，为整个星系的样本。

英文摘要：

A variety of host galaxy (bulge) parameters are examined in order to determine their predictive power in ascertaining the masses of the supermassive black holes (SMBH) at the centers of the galaxies. Based on a sample of 23 nearby galaxies, comprised of both elliptical galaxies and spiral/lenticular bulges, we identify a strong correlation between the bulge gravitational binding energy ($E_g$), as traced by the stellar light profile, and the SMBH mass ($M_{\bullet}$), such that $M_{\bullet} \propto E_g^{0.6}$. The scatter about the relationship indicates that this is as strong a predictor of $M_{\bullet}$ as the velocity dispersion ($σ$), for the elliptical galaxy subsample. Improved mass-to-light ratios, obtained with IFU spectroscopy and I-band photometry by the SAURON group, were used for those sample galaxies where available, resulting in an energy predictor with the same slope, but with reduced scatter. Alternative $M_{\bullet}$ predictors such as the gravitational potential and the bulge mass are also explored, but these are found to be inferior when compared with both the bulge gravitational binding energy and bulge velocity dispersion predictors, for the full galaxy sample.

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