Investigating AGN black hole masses and the MBH–σe relation for low surface brightness galaxies
Investigating AGN black hole masses and the MBH–σe relation for low surface brightness galaxies
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DOI：
10.1093/mnras/stv2500
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发表时间：
2015-10
影响因子：
4.8
通讯作者：
S. Subramanian;Ramya.S;M. Das;K. George;Sivarani.T;T. Prabhu
中科院分区：
文献类型：
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作者：
S. Subramanian;Ramya.S;M. Das;K. George;Sivarani.T;T. Prabhu
本文分析了一个低表面亮度（LSB）星系的活动星系核（AGN）的光学核谱。利用斯隆数字巡天（SDSS）的数据，我们从它们的广义H α参数中推导出了24个星系的维里黑洞（BH）质量。我们发现我们对BH核质量的估计在10（5）-10（7）M圆点的范围内，中值质量为5.62 × 10（6）M圆点。球核恒星速度色散σ（e）是由恒星光谱确定的。我们将我们的结果与现有的BH质量-速度色散（M-BH-sigma（e））相关性进行了比较，发现我们的大多数样本位于低BH质量区域，低于M-BH-sigma（e）相关性。我们分析了M-BH估计中的任何系统偏差的影响，星系取向对sigma（e）测量的影响以及由于存在棒而导致的sigma（e）的增加，发现这些影响不足以解释M-BH-sigma（e）相关性中观察到的偏移。因此，LSB星系倾向于具有低质量的黑洞，这些黑洞可能不与宿主星系的凸起共同进化。需要详细研究凸起的性质和暗物质在BH生长中的作用，以进一步了解BH-凸起在这些演化不良和暗物质主导的系统中的共同演化。
We present an analysis of the optical nuclear spectra from the active galactic nuclei (AGN) in a sample of low surface brightness (LSB) galaxies. Using data from the Sloan Digital Sky Survey (SDSS), we derived the virial black hole (BH) masses of 24 galaxies from their broad H alpha parameters. We find that our estimates of nuclear BH masses lie in the range 10(5)-10(7) M-circle dot, with a median mass of 5.62 x 10(6) M-circle dot. The bulge stellar velocity dispersion sigma(e) was determined from the underlying stellar spectra. We compared our results with the existing BH mass-velocity dispersion (M-BH-sigma(e)) correlations and found that the majority of our sample lie in the low BH mass regime and below the M-BH-sigma(e) correlation. We analysed the effects of any systematic bias in the M-BH estimates, the effects of galaxy orientation in the measurement of sigma(e) and the increase of sigma(e) due to the presence of bars and found that these effects are insufficient to explain the observed offset in M-BH-sigma(e) correlation. Thus, the LSB galaxies tend to have low-mass BHs which probably are not in co-evolution with the host galaxy bulges. A detailed study of the nature of the bulges and the role of dark matter in the growth of the BHs is needed to further understand the BH-bulge co-evolution in these poorly evolved and dark matter dominated systems.