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The Discovery of a Hidden Broad-line AGN in a Bulgeless Galaxy: Keck NIR Spectroscopic Observations of SDSS J085153.64+392611.76
The Astrophysical Journal ( IF 4.8 ) Pub Date : 2020-08-14 , DOI: 10.3847/1538-4357/aba52c
Thomas Bohn 1 , Gabriela Canalizo 1 , Shobita Satyapal 2 , Ryan W. Pfeifle 2
Affiliation  

We report the discovery of a buried, active supermassive black hole in SDSS J085153.64+392611.76, a bulgeless Seyfert 2 (Sy2) galaxy. Keck near-infrared observations reveal a hidden broad line region, allowing for the rare case where strong constraints can be placed on both the black hole mass and bulge component. Using virial mass estimators, we obtain a black hole mass of log($M_{\rm{BH}}/M_{\odot}$) = $6.78 \pm 0.50$. This is one of the only Sy2 AGN hosted in a bulgeless galaxy with a virial black hole mass estimate and could provide important constraints on the formation scenarios of the black hole seed population. The lack of a bulge component suggests that the SMBH has grown quiescently, likely caused by secular processes independent of major mergers. In the absence of a detectable bulge component, we find the $M_{\rm{BH}}$ - $M_{\rm{stellar}}$ relation to be more reliable than the $M_{\rm{BH}}$ - $M_{\rm{bulge}}$ relation. In addition, we detect extended narrow Pa$\alpha$ emission that allows us to create a rotation curve where we see counter-rotating gas within the central kiloparsec (kpc). Possible causes of this counter-rotation include a galactic bar or disruption of the inner gas by a recent fly-by of a companion galaxy. This in turn could have triggered accretion onto the central SMBH in the current AGN phase.

中文翻译:

在无膨胀星系中发现隐藏的宽线 AGN:SDSS J085153.64+392611.76 的凯克近红外光谱观测

我们报告在 SDSS J085153.64+392611.76 中发现了一个埋藏的、活跃的超大质量黑洞,这是一个无膨胀的赛弗特 2 (Sy2) 星系。凯克近红外观测揭示了一个隐藏的宽线区域,允许对黑洞质量和凸起部分都施加强约束的罕见情况。使用维里质量估计器,我们获得了 log($M_{\rm{BH}}/M_{\odot}$) = $6.78 \pm 0.50$ 的黑洞质量。这是在无球星系中仅有的一个 Sy2 AGN,其具有虚拟黑洞质量估计,并且可以为黑洞种子种群的形成场景提供重要的限制。缺乏凸出部分表明 SMBH 一直在悄悄增长,这可能是由独立于重大合并的长期过程引起的。在没有可检测的凸起成分的情况下,我们发现 $M_{\rm{BH}}$ - $M_{\rm{stellar}}$ 的关系比 $M_{\rm{BH}}$ - $M_{\rm{bulge} 更可靠}$ 关系。此外,我们检测到扩展的窄 Pa$\alpha$ 发射,这使我们能够创建旋转曲线,在那里我们可以看到中央千秒差距 (kpc) 内的反向旋转气体。这种反向旋转的可能原因包括星系棒或最近的伴星系飞越对内部气体的破坏。这反过来可能在当前 AGN 阶段触发了中央 SMBH 的吸积。这种反向旋转的可能原因包括星系棒或最近的伴星系飞越对内部气体的破坏。这反过来可能在当前 AGN 阶段触发了中央 SMBH 的吸积。这种反向旋转的可能原因包括星系棒或最近的伴星系飞越对内部气体的破坏。这反过来可能在当前 AGN 阶段触发了中央 SMBH 的吸积。
更新日期:2020-08-14
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