黑洞是否大到足以使星系团冷核的冷却淬灭？
Are black holes big enough to quench cooling in cluster cool cores?
摘要：
总能量参数（例如，Fabian等人（2002年）提出，黑洞的质量需要大大超过经典黑洞质量-速度弥散关系（M-sigma）的预测，以便抵消巨大冷核心星系团中的冷却损失。这表明黑洞可能太小，无法为这样的星系团提供能量。然而，Lauer等人（2007）认为，黑洞质量-膨胀光度关系是高光度星系中黑洞质量的更好预测，并且这种关系预测了BCGs中更高的质量。他们发现，与亮度较低的星系相比，BCGs中的速度色散随着亮度的增加而缓慢增加，有效半径随着亮度的增加而迅速增加。受这些结果和Boylan-Kolchin等人（2006）关于孤立合并的理论工作的启发，我们对千禧年运行中确定的大质量星系团中的干合并进行了高分辨率的宇宙学模拟，包括合并星系的暗物质晕和恒星隆起。我们证明了BCG明显地偏离了由较小星系定义的大小-光度关系（即，关系弯曲），并且我们还看到亮度-σ关系中的弯曲。由于黑洞质量与BCGs（如果它们主要是在无耗散合并中形成的）的恒星隆起的质量和光度成正比，我们的发现与Lauer等人（2007）在定性水平上的结果一致，并表明BCGs中的黑洞可能确实比标准M-sigma关系预测的质量更大。
英文摘要：
Total energy arguments (e.g., Fabian et al. 2002) suggest that black holes need to have masses significantly in excess of the prediction from the classic black hole mass - velocity dispersion relation (M-sigma) in order to offset the cooling losses in massive cool core clusters. This suggests that the black holes may be too small to power such clusters. However, Lauer et al. (2007) argue that the black hole mass - bulge luminosity relationship is a better predictor of black hole masses in high luminosity galaxies and that this relationship predicts significantly higher masses in BCGs. They find slow increase in the velocity dispersion with luminosity and a more rapid increase in effective radii with luminosity seen in BCGs as opposed to less luminous galaxies. Motivated by these results and the theoretical work of Boylan-Kolchin et al. (2006) on isolated mergers, we perform high-resolution cosmological simulations of dry mergers in a massive galaxy cluster identified in the Millennium Run including both the dark matter halos and stellar bulges of merging galaxies. We demonstrate that the BCG clearly evolves away from the size-luminosity relation as defined by the smaller galaxies (i.e., the relation bends) and we also see a bending in the luminosity-sigma relation. As black hole mass is expected to be proportional to the mass and luminosity of the stellar bulge of the BCGs (if they were formed in predominantly dissipationless mergers), our findings are consistent with those of Lauer et al. (2007) on a qualitative level and suggest that the black holes in BCGs may indeed be more massive than predicted from the standard M-sigma relation.
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