The M-sigma and M-L Relations in Galactic Bulges and Determinations of their Intrinsic Scatter
Kayhan Gultekin, Douglas O. Richstone, Karl Gebhardt, Tod R. Lauer, Scott Tremaine, M. C. Aller, Ralf Bender, Alan Dressler, S. M. Faber, Alexei V. Filippenko, … 展开作者
Kayhan Gultekin, Douglas O. Richstone, Karl Gebhardt, Tod R. Lauer, Scott Tremaine, M. C. Aller, Ralf Bender, Alan Dressler, S. M. Faber, Alexei V. Filippenko, Richard Green, Luis C. Ho, John Kormendy, John Magorrian, Jason Pinkney, Christos Siopis
We derive improved versions of the relations between supermassive black hole mass (M_BH) and host-galaxy bulge velocity dispersion (sigma) and luminosity (L) (the M-sigma and M-L relations), based on 49 M_BH measurements and 19 upper limits. Particular attention is paid to recovery of the intrinsic scatter (epsilon_0) in both relations. We find log(M_BH / M_sun) = alpha + beta * log(sigma / 200 km/s) with (alpha, beta, epsilon_0) = (8.12 +/- 0.08, 4.24 +/- 0.41, 0.44 +/- 0.06) for all galaxies and (alpha, beta, epsilon_0) = (8.23 +/- 0.08, 3.96 +/- 0.42, 0.31 +/- 0.06) for ellipticals. The results for ellipticals are consistent with previous studies, but the intrinsic scatter recovered for spirals is significantly larger. The scatter inferred reinforces the need for its consideration when calculating local black hole mass function based on the M-sigma relation, and further implies that there may be substantial selection bias in studies of the evolution of the M-sigma relation. We estimate the M-L relationship as log(M_BH / M_sun) = alpha + beta * log(L_V / 10^11 L_sun,V) of (alpha, beta, epsilon_0) = (8.95 +/- 0.11, 1.11 +/- 0.18, 0.38 +/- 0.09); using only early-type galaxies. These results appear to be insensitive to a wide range of assumptions about the measurement errors and the distribution of intrinsic scatter. We show that culling the sample according to the resolution of the black hole's sphere of influence biases the relations to larger mean masses, larger slopes, and incorrect intrinsic residuals.
An Improved [O III] Line Width to Stellar Velocity Dispersion Calibration: Curvature, Scatter, and Lack of Evolution in the Black-Hole Mass Versus Stellar Velocity Dispersion Relationship
Resonant scattering effect on the soft X-ray line emission from the hot interstellar medium: I. galactic bulges
漫射软X射线线发射通常用于追踪附近星系中热星际介质的热和化学性质及其内容。虽然共振线散射使发射的解释复杂化，但它也提供了测量介质运动学的机会。我们已经实现了一个直接的蒙特卡罗模拟计划，使我们能够占介质中的共振散射效应，在原则上，与任意的空间，热，化学和运动学分布。在这里，我们应用此方案通过无量纲计算的等温，化学均匀，球对称介质的径向密度分布的特点是由$β$模型。该应用程序同时考虑到由于散射引起的共振线发射的光学深度相关的空间失真和强度变化，与先前的计算一致。我们进一步将建模方案应用于M31凸起的XMM-牛顿RGS光谱中观察到的OVII和OVIII发射线复合体。这个模型，虽然由于其简单性而具有各种限制，但表明共振散射确实可以解释发射的大部分空间失真，以及线的相对强度，特别是OVII He $α$三重态的大的禁戒与共振线之比。我们首次估计了M31中各向同性湍流马赫数为$\sim0.17$，线发射气体温度为$\sim2.3\times10^6$ K。我们的结论是，共振散射一般可以发挥重要作用，在塑造软X射线光谱的弥漫热气体在正常的星系。
