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arXiv 1303.5490astro-ph.CO
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超大质量黑洞质量-椭球恒星质量关系的Sérsic和Core-Sérsic星系

The Supermassive Black Hole Mass - Spheroid Stellar Mass Relation for Sérsic and Core-Sérsic Galaxies

Nicholas Scott, Alister W. Graham, James Schombert

备注：
10 pages, 5 figures, accepted for publication in ApJ
发表信息：
2013, ApJ, 768, 76
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摘要：

本文以75个邻近星系为样本，研究了超大质量黑洞质量（M $_{BH}$）与宿主椭球体恒星质量（M $_{sph,*}$）之间的关系。为了得到球状体恒星的质量，我们使用了改进的2 MASS K $_s$波段测光从ARCHANGEL测光管道。将我们的样本分为核心-Sérsic和Sérsic星系，我们发现它们由非常不同的M $_{BH}$ $_{sph,*}$关系描述。对于核心Sérsic星系-这是典型的质量和发光，M $_{BH} \gtrsim 2x10^8 M_\odot$ -我们发现M $_{BH} \propto M_{sph,*}^{(0.97 \pm 0.14)}$，与其他文献的关系。然而，对于Sérsic星系-具有典型的较低质量M $_{sph,*} \lesssim 3x10^10 M_\odot$ -我们发现M $_BH \propto M_{sph,*}^{(2.22 \pm 0.58)}$，一个非常陡峭的斜率，相差超过2个标准差。这个关系证实了，对于Sérsic星系，M $_{BH}$不是M $_{sph,*}$的常数。星系可以通过气体的吸积来增长，这些气体为恒星的形成和中心的黑洞提供了燃料，也可以通过合并来增长。它们的黑洞比它们的宿主球体增长得更快，在干合并事件产生核心-Sérsic星系之前，黑洞和球体同步增长。我们还将我们的Sérsic M $_{BH}$ -M $_{sph,*}$关系与核星团的相应关系进行了比较，证实了两类中心大质量天体遵循明显不同的标度关系。

英文摘要：

We have examined the relationship between supermassive black hole mass (M$_{BH}$) and the stellar mass of the host spheroid (M$_{sph,*}$) for a sample of 75 nearby galaxies. To derive the spheroid stellar masses we used improved 2MASS K$_s$-band photometry from the ARCHANGEL photometry pipeline. Dividing our sample into core-Sérsic and Sérsic galaxies, we find that they are described by very different M$_{BH}$-M$_{sph,*}$ relations. For core-Sérsic galaxies - which are typically massive and luminous, with M$_{BH} \gtrsim 2x10^8 M_\odot$ - we find M$_{BH} \propto M_{sph,*}^{(0.97 \pm 0.14)}$, consistent with other literature relations. However, for the Sérsic galaxies - with typically lower masses, M$_{sph,*} \lesssim 3x10^10 M_\odot$ - we find M$_BH \propto M_{sph,*}^{(2.22 \pm 0.58)}$, a dramatically steeper slope that differs by more than 2 standard deviations. This relation confirms that, for Sérsic galaxies, M$_{BH}$ is not a constant fraction of M$_{sph,*}$. Sérsic galaxies can grow via the accretion of gas which fuels both star formation and the central black hole, as well as through merging. Their black hole grows significantly more rapidly than their host spheroid, prior to growth by dry merging events that produce core-Sérsic galaxies, where the black hole and spheroid grow in lock step. We have additionally compared our Sérsic M$_{BH}$-M$_{sph,*}$ relation with the corresponding relation for nuclear star clusters, confirming that the two classes of central massive object follow significantly different scaling relations.

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