arXiv 0910.22322009-10astro-ph.CO

星系合并中黑洞标度关系的演化

The evolution of Black Hole scaling relations in galaxy mergers

Peter H. Johansson, Andreas Burkert, Thorsten Naab

备注：: 6 pages, 4 figures, accepted to ApJL (minor revisions to match accepted version)
发表信息：: Astrophys.J.707:L184-L189,2009
DOI：: 10.1088/0004-637X/707/2/L184

摘要：

研究了处于合并过程中的盘星系中M_BH-sigma和M_BH-M_bulge平面上的黑洞（BH）随时间的演化。我们开始模拟的祖先黑洞质量最初低于（Δ log M_BH=-2），（Δ log M_BH=0）和以上（Δ log M_BH=0.5）所观察到的本地关系。最终的关系是在星系和它们的黑洞最终合并之后迅速建立起来的。具有低初始气体分数（f_gas=0.2）的祖先从低于关系式开始演变到关系式上（Δ log M_BH=-0.18），关系式上的祖先停留在那里（Δ log M_BH=0），最后关系式上方的祖先朝向关系式演变，但仍保持在它们上方（Δ log M_BH=0.35）。在所有情况下（Δ log M_BH=0.5），其中祖先具有高初始气体分数（f_gas=0.8）的合并都在关系式之上发展。我们发现，初始气体馏分是分散在所观察到的关系的主要来源，占主导地位的合并残余物的演化阶段所产生的散射。事实上，BH开始以上的关系不演变的关系，表明我们的模拟排除了超大质量BH演变的关系，通过丰富的气体合并的情况。由此暗示，我们的模拟不赞成超大质量黑洞在其母核膨胀之前显著发展的情况。

英文摘要：

We study the evolution of black holes (BHs) on the M_BH-sigma and M_BH-M_bulge planes as a function of time in disk galaxies undergoing mergers. We begin the simulations with the progenitor black hole masses being initially below (Delta log M_BH=-2), on (Delta log M_BH=0) and above (Delta log M_BH=0.5) the observed local relations. The final relations are rapidly established after the final coalescense of the galaxies and their BHs. Progenitors with low initial gas fractions (f_gas=0.2) starting below the relations evolve onto the relations (Delta log M_BH=-0.18), progenitors on the relations stay there (Delta log M_BH=0) and finally progenitors above the relations evolve towards the relations, but still remaining above them (Delta log M_BH=0.35). Mergers in which the progenitors have high initial gas fractions (f_gas=0.8) evolve above the relations in all cases (Delta log M_BH=0.5). We find that the initial gas fraction is the prime source of scatter in the observed relations, dominating over the scatter arising from the evolutionary stage of the merger remnants. The fact that BHs starting above the relations do not evolve onto the relations, indicates that our simulations rule out the scenario in which overmassive BHs evolve onto the relations through gas-rich mergers. By implication our simulations thus disfavor the picture in which supermassive BHs develop significantly before their parent bulges.

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