Active Galactic Nuclei and Galaxy Interactions
Active Galactic Nuclei and Galaxy Interactions
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DOI：
10.1111/j.1365-2966.2007.11367.x
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发表时间：
2007-03
影响因子：
4.8
通讯作者：
M. S. Alonso;D. Lambas;P. Tissera;G. Coldwell
中科院分区：
文献类型：
--
作者：
M. S. Alonso;D. Lambas;P. Tissera;G. Coldwell
我们进行了活动星系核（AGN）的主机特性和核活动的活动星系核对和没有同伴的统计分析。我们的研究涉及一个由Kauffmann等人的Sloan Digital Sky Survey Data Release 4数据导出的活动星系核样本，以及由Alonso等人的同一数据集导出的成对星系。（rp <25kpc h-1，ΔV < 350 km s-1），根据通过扭曲形态和潮汐特征相互作用的证据，为我们提供了更有信心的从这个样本中评估星系间的相互作用。我们注意到，在一个给定的光度或恒星质量含量，AGN的分数是较大的对星系表现出强相互作用和潮汐功能，也表现出强烈的星星形成活动的迹象的证据。尽管如此，这一过程只占活动星系核比例增加的2.10%。在以前的工作中，我们发现活动星系核主机是红色的，具有较大的浓度形态指数比非活动星系核星系。这种效应不依赖于活动星系核主机是成对的还是孤立的。具有强相互作用特征的活动星系核的O III光度明显大于其他活动星系核，无论是成对的还是孤立的。对吸积率L[O III]/M BH的估计表明，合并对中的活动星系核正在积极地喂养它们的黑洞，而不管它们的恒星质量如何。我们还发现伴星系的光度似乎是决定黑洞活动的一个关键参数。在给定的宿主光度下，有明亮伴星（Mr < -20）的活动星系核的O III光度和L[O III]/MBH都明显大于无伴星的活动星系核。
We perform a statistical analysis of active galactic nucleus (AGN) host characteristics and nuclear activity for AGNs in pairs and without companions. Our study concerns a sample of AGNs derived from the Sloan Digital Sky Survey Data Release 4 data by Kauffmann et al. and pair galaxies obtained from the same data set by Alonso et al. An eye-ball classification of images of 1607 close pairs (r p < 25 kpc h -1 ,ΔV < 350 km s -1 ) according to the evidence of interaction through distorted morphologies and tidal features provides us with a more confident · assessment of galaxy interactions from this sample. We notice that, at a given luminosity or stellar mass content, the fraction of AGNs is larger for pair galaxies exhibiting evidence for strong interaction and tidal features which also show signs of strong star formation activity. Nevertheless, this process accounts only for a ∼10 per cent increase of the fraction of AGNs. As in previous works, we find AGN hosts to be redder and with a larger concentration morphological index than non-AGN galaxies. This effect does not depend on whether AGN hosts are in pairs or in isolation. The O III luminosity of AGNs with strong interaction features is found to be significantly larger than that of other AGNs, either in pairs or in isolation. Estimations of the accretion rate, L[O III]/M BH , show that AGNs in merging pairs are actively feeding their black holes, regardless of their stellar masses. We also find that the luminosity of the companion galaxy seems to be a key parameter in the determination of the black hole activity. At a given host luminosity, both the O III luminosity and the L[O III]/M BH are significantly larger in AGNs with a bright companion (M r < -20) than otherwise.