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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >OISTER optical and near-infrared monitoring observations of peculiar radio-loud active galactic nucleus SDSS?J110006.07+442144.3
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OISTER optical and near-infrared monitoring observations of peculiar radio-loud active galactic nucleus SDSS?J110006.07+442144.3

机译：特殊的放射性大声活跃银河核SDSS的OISTER光学和近红外监测观察？J110006.07 + 442144.3

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摘要

We present monitoring campaign observations at optical and near-infrared (NIR) wavelengths for a radio-loud active galactic nucleus (AGN) at z = 0.840, SDSS?J110006.07+442144.3 (hereafter, J1100+4421), which was identified during a flare phase in late 2014 February. The campaigns consist of three intensive observing runs from the discovery to 2015 March, mostly within the scheme of the OISTER collaboration. Optical–NIR light curves and simultaneous spectral energy distributions (SEDs) are obtained. Our measurements show the strongest brightening in 2015 March. We found that the optical–NIR SEDs of J1100+4421 show an almost steady shape despite the large and rapid intranight variability. This constant SED shape is confirmed to extend to ～5?μm in the observed frame using the archival WISE data. Given the lack of absorption lines and the steep power-law spectrum of αν ～ ?1.4, where $$f_{u }propto u ^{lpha _{u }}$$, synchrotron radiation by a relativistic jet with no or small contributions from the host galaxy and the accretion disk seems most plausible as an optical–NIR emission mechanism. The steep optical–NIR spectral shape and the large amplitude of variability are consistent with this object being a low νpeak jet-dominated AGN. In addition, sub-arcsecond resolution optical imaging data taken with Subaru Hyper Suprime-Cam does not show a clear extended component and the spatial scales are significantly smaller than the large extensions detected at radio wavelengths. The optical spectrum of a possible faint companion galaxy does not show any emission lines at the same redshift, and hence a merging hypothesis for this AGN-related activity is not supported by our observations.
机译：我们提出了在z = 0.840，SDSS？J110006.07 + 442144.3（以下称为J1100 + 4421）处发现的放射性大声活跃银河核（AGN）在光学和近红外（NIR）波长下的监视活动观测结果。在2014年2月下旬爆发。这些运动包括从发现到2015年3月的三个密集观测运行，主要是在OISTER合作计划范围内。获得光学–NIR光曲线和同时的光谱能量分布（SED）。我们的测量结果显示，2015年3月最亮。我们发现J1100 + 4421的光学–近红外SED表现出几乎稳定的形状，尽管夜间波动很大且变化很快。使用档案WISE数据，可以在观察到的帧中确认这种恒定的SED形状扩展到〜5？μm。考虑到缺乏吸收线和αν〜？1.4的陡幂律谱，其中$$ f _ { nu} propto nu ^ { alpha {{nu}} $$几乎没有来自主星系和吸积盘的贡献，这似乎是一种光学的近红外发射机制。陡峭的光学-NIR光谱形状和较大的变化幅度与该物体为低νpeak射流为主的AGN一致。此外，用Subaru Hyper Suprime-Cam拍摄的亚秒级分辨率光学成像数据未显示清晰的扩展分量，并且空间尺度明显小于在无线电波长下检测到的大扩展。可能的暗淡伴星系的光谱在相同的红移下没有显示任何发射线，因此我们的观测结果不支持这种与AGN相关的活动的合并假设。

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