椭圆星系中心黑洞的反馈。II：纯机械能反馈模型能工作吗？
Feedback from central black holes in elliptical galaxies. II: Can purely mechanical energy feedback models work?
摘要：
通过使用高分辨率的一维流体动力学模拟，我们调查的影响，从超大质量黑洞（SMBHs）在椭圆星系的演化过程中的纯机械反馈的反馈效率范围广泛，并比较结果的四个主要的观测约束。特别是，我们专注于1）中央黑洞恒星质量比的宿主星系，2）的发光类星体阶段的寿命，3）的质量的恒星形成的宿主星系内的最后Gyr，和4）X射线光度的热弥漫气体。因此，我们试图确定最成功的机械反馈效率范围。我们发现，虽然低反馈效率导致太多的增长的SMBH，高效率完全吹出热星际气体，和模型的特点是非常低的热X射线光度远低于观察范围。类星体相位的净寿命与SMBH和其宿主星系之间的质量比密切相关，而X射线光度通常与最后一个Gyr内最近的恒星形成有关。当考虑普遍采用的恒定反馈效率模型时，沉积到环境介质中的反馈能量应大于SMBH吸积能量的0.01%，以符合本地宇宙中SMBH质量与恒星质量的比例。然而，热气体的X射线光度有利于约0.005%的吸积能量作为AGN的机械反馈能量。我们的结论是，纯粹的机械反馈模式是不可能同时兼容的所有四个可观察到的测试，甚至允许广泛的反馈效率，包括辐射和机械反馈一起可能是一个解决方案，以遵守观测约束。[删节]
英文摘要：
By using high-resolution 1D hydrodynamical simulations, we investigate the effects of purely mechanical feedback from super massive black holes (SMBHs) in the evolution of elliptical galaxies for a broad range of feedback efficiencies and compare the results to four major observational constraints. In particular, we focus on 1) the central black hole to stellar mass ratio of the host galaxy, 2) the lifetime of the luminous quasar phase, 3) the mass of stars formed in the host galaxy within the last Gyr, and 4) the X-ray luminosity of the hot diffuse gas. As a result, we try to pin down the most successful range of mechanical feedback efficiencies. We find that while low feedback efficiencies result in too much growth of the SMBH, high efficiencies totally blow out the hot interstellar gas, and the models are characterized by very low thermal X-ray luminosity well below the observed range. The net lifetime of the quasar phase is strongly coupled to the mass ratio between SMBH and its host galaxy, while the X-ray luminosity is generally correlated to the recent star formation within the last Gyr. When considering the popularly adopted model of the constant feedback efficiency, the feedback energy deposited into the ambient medium should be more than 0.01% of the SMBH accretion energy to be consistent with the SMBH mass to stellar mass ratio in the local universe. Yet, the X-ray luminosity of the hot gas favors about 0.005% of the accretion energy as the mechanical AGN feedback energy. We conclude that the purely mechanical feedback mode is unlikely to be simultaneously compatible with all four observable tests, even allowing a broad range of feedback efficiencies, and that including both radiative and mechanical feedback together may be a solution to comply the observational constraints. [abridged]
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