The Many lives of AGN: Cooling flows, black holes and the luminosities and colours of galaxies
The Many lives of AGN: Cooling flows, black holes and the luminosities and colours of galaxies
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DOI：
10.1111/j.1365-2966.2006.09994.x
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发表时间：
2006-02
影响因子：
4.8
通讯作者：
D. Croton;G. Kauffmann;V. Springel;S. White;G. Lucia;A. Jenkins;J. Navarro;C. Frenk;Liang Gao-Lian
中科院分区：
文献类型：
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作者：
D. Croton;G. Kauffmann;V. Springel;S. White;G. Lucia;A. Jenkins;J. Navarro;C. Frenk;Liang Gao-Lian
我们通过在千年运行的输出上实现一套半解析模型来模拟星系及其中心超大质量黑洞的增长，千年运行是一个非常大的concordance ecdm宇宙学模拟。我们的程序跟踪每个物体的详细组装历史，并且能够跟踪所有比小麦哲伦星云更大的星系的演化，整个体积可与大型现代红移调查相媲美。在这第一篇论文中，我们用一种新的“射电”反馈模型补充了先前对中心黑洞生长和活动的处理方法，该模型来自位于星系群或星系团中准静态x射线发射大气中心的AGN。我们表明，对于能量上和观测上合理的参数，这样的模型可以同时解释：(i)在冷却流中观测到的低质量脱落率；（ii）星系亮度函数亮端的指数截止值；（iii）事实上，质量最大的星系往往是星团中以膨胀为主的系统，并且比质量较小的星系包含系统年龄更大的恒星。这一成功的发生是因为静态的热大气球只在最巨大的结构中形成，而无线电反馈（与超新星或星暴反馈相反）可以抑制进一步的冷却和恒星形成，而不需要恒星形成。我们讨论了可能的物理模型，这些模型可能解释了我们的现象学“射电模式”模型成功所需的吸积率缩放。
We simulate the growth of galaxies and their central supermassive black holes by implementing a suite of semi-analytic models on the output of the Millennium Run, a very large simulation of the concordanceCDM cosmogony. Our procedures fol- low the detailed assembly history of each object and are able to track the evolution of all galaxies more massive than the Small Magellanic Cloud throughout a volume comparable to that of large modern redshift surveys. In this first paper we supple- ment previous treatments of the growth and activity of central black holes with a new model for 'radio' feedback from those AGN that lie at the centre of a quasistatic X-ray emitting atmosphere in a galaxy group or cluster. We show that for energetically and observationally plausible parameters such a model can simultaneously explain: (i) the low observed mass drop-out rate in cooling flows; (ii) the exponential cut-off at the bright end of the galaxy luminosity function; and (iii) the fact that the most massive galaxies tend to be bulge-dominated systems in clusters and to contain systematically older stars than lower mass galaxies. This success occurs because static hot atmo- spheres form only in the most massive structures, and radio feedback (in contrast, for example, to supernova or starburst feedback) can suppress further cooling and star formation without itself requiring star formation. We discuss possible physical mod- els which might explain the accretion rate scalings required for our phenomenological 'radio mode' model to be successful.