纤维光谱的混乱性质：伪装成双重1型活动星系核的星-类星体对
The Messy Nature of Fiber Spectra: Star-Quasar Pairs Masquerading as Dual Type 1 AGNs
摘要：
理论研究预测，超大质量黑洞最显著的增长发生在合并的后期，与双活动星系核（AGN）的出现相吻合，并且主合并和次合并都对双活动星系核的增长具有重要意义。事实上，双活动星系核在较小的合并应该是路标有效的较小的合并诱导SMBH增长的更多和更少的大规模的祖。我们确定了两个候选的双重活动星系核，它们存在于明显的次要合并中，质量比分别为$\sim$ 1：7和$\sim$ 1：30。SDSS光纤光谱显示，宽和窄的发射线在每个合并的初级核，而只有一个狭窄的[O III]发射线和广泛和突出的H $α$ /[N II]复合物中观察到的次级核。在每次合并中，初级核和次级核中的宽H $α$线的FWHM是不一致的，这表明每次合并中的每个核都有一个1型活动星系核。然而，空间分辨LBT光谱揭示了静止帧恒星吸收特征，表明次级源是前景恒星，并且先前检测到的宽线可能是SDSS观测时大气视宁度引起的光纤溢出效应的结果。这项研究表明，第一次，光学光谱搜索1型/1型对同样遭受光纤溢出效应已观察到以前的赛弗特2双活动星系核候选人。如果使用波长范围或灵敏度更有限的仪器，前景恒星的存在可能并不清楚。
英文摘要：
Theoretical studies predict that the most significant growth of supermassive black holes occurs in late-stage mergers, coinciding with the manifestation of dual active galactic nuclei (AGNs), and both major and minor mergers are expected to be important for dual AGN growth. In fact, dual AGNs in minor mergers should be signposts for efficient minor merger-induced SMBH growth for both the more and less massive progenitor. We identified two candidate dual AGNs residing in apparent minor mergers with mass ratios of $\sim$1:7 and $\sim$1:30. SDSS fiber spectra show broad and narrow emission lines in the primary nuclei of each merger while only a narrow [O III] emission line and a broad and prominent H$α$/[N II] complex is observed in the secondary nuclei. The FWHMs of the broad H$α$ lines in the primary and secondary nuclei are inconsistent in each merger, suggesting that each nucleus in each merger hosts a Type 1 AGN. However, spatially-resolved LBT optical spectroscopy reveal rest-frame stellar absorption features, indicating the secondary sources are foreground stars and that the previously detected broad lines are likely the result of fiber spillover effects induced by the atmospheric seeing at the time of the SDSS observations. This study demonstrates for the first time that optical spectroscopic searches for Type 1/Type 1 pairs similarly suffer from fiber spillover effects as has been observed previously for Seyfert 2 dual AGN candidates. The presence of foreground stars may not have been clear if an instrument with more limited wavelength range or limited sensitivity had been used.
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