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BH-宿主关联中的小离散&自调节BH增长的情形

The Small Scatter in BH-Host Correlations & The Case for Self-Regulated BH Growth

Philip F. Hopkins, Norman Murray, Todd Thompson

备注：
9 pages, 3 figures, accepted to MNRAS (revised to match published version)
发表信息：
Mon.Not.Roy.Astron.Soc. 398:303-311, 2009
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摘要：

超大质量黑洞（BH）的质量与其宿主星系的性质（如恒星总质量、速度色散和势阱深度）之间遵循严格的标度关系。这导致了BH生长的自我调节模型的发展，其中来自中央BH的反馈在达到临界阈值时停止其自身的生长。然而，也有人提出了反馈不起作用的模型：只要有固定比例的宿主气体供应被吸积，就可以重现所观察到的关系。在这里，我们认为，分散在所观察到的BH主机的相关性，其运行规模，提出了一个苛刻的约束这些相关性的任何模型，它有利于自我调节模型BH增长。我们发现，在观测到的椭圆和椭球体中，在半径R内的恒星质量分数的散射在小R处强烈增加。在固定的恒星总质量（或主机速度色散）下，在BH影响半径附近的非常小的尺度上，必须进入并形成恒星的气体量存在数量级的散射。简而言之，BH似乎比小尺度上的恒星和气体供应更了解大尺度上的全球宿主星系潜力。这是在自我调节模型中预测的;然而，没有反馈的模型通常会预测BH-宿主相关性的数量级分散。同样，模型中的BH反馈在“明亮”模式不调节BH本身的增长，但设置恒星质量的星系诱导恒星形成或吹出的气体质量远远大于星系恒星质量，是很难调和的散射在小尺度上。

英文摘要：

Supermassive black holes (BHs) obey tight scaling relations between their mass and their host galaxy properties such as total stellar mass, velocity dispersion, and potential well depth. This has led to the development of self-regulated models for BH growth, in which feedback from the central BH halts its own growth upon reaching a critical threshold. However, models have also been proposed in which feedback plays no role: so long as a fixed fraction of the host gas supply is accreted, relations like those observed can be reproduced. Here, we argue that the scatter in the observed BH-host correlations, and its run with scale, presents a demanding constraint on any model for these correlations, and that it favors self-regulated models of BH growth. We show that the scatter in the stellar mass fraction within a radius R in observed ellipticals and spheroids increases strongly at small R. At fixed total stellar mass (or host velocity dispersion), on very small scales near the BH radius of influence, there is an order-of-magnitude scatter in the amount of gas that must have entered and formed stars. In short, the BH appears to 'know more' about the global host galaxy potential on large scales than the stars and gas supply on small scales. This is predicted in self-regulated models; however, models where there is no feedback would generically predict order-of-magnitude scatter in the BH-host correlations. Likewise, models in which the BH feedback in the 'bright' mode does not regulate the growth of the BH itself, but sets the stellar mass of the galaxy by inducing star formation or blowing out a mass in gas much larger than the galaxy stellar mass, are difficult to reconcile with the scatter on small scales.

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