Investigating the multiwavelength behaviour of the flat spectrum radio quasar CTA 102 during 2013-2017
Investigating the multiwavelength behaviour of the flat spectrum radio quasar CTA 102 during 2013-2017
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研究 2013-2017 年期间平坦频谱射电类星体 CTA 102 的多波长行为
DOI：
10.1093/mnras/stz2792
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发表时间：
2019
影响因子：
4.8
通讯作者：
D'Ammando F
中科院分区：
文献类型：
--
作者：
D'Ammando F
我们在2013-2017年期间对平谱射电类星体CTA 102进行了多波长研究。我们使用了全地球Blazar望远镜获得的无线电-光学数据，欧文斯谷射电天文台的15 GHz数据，阿塔卡马大型毫米波阵列的91和103 GHz数据，快速眼监视器望远镜的近红外数据，以及来自theSwift的数据在这方面，我们将利用光学紫外线和X射线卫星以及费米（γ射线）卫星来研究通量和光谱可变性以及不同波长通量变化之间的相互关系。在2016年11月至2017年2月期间观察到前所未有的γ射线耀斑活动，有四次主要爆发。在2016年12月28日达到峰值通量（2158 ± 63）× 10− 8 ph cm−2s−1，对应光度（2.2 ± 0.1）× 1050 erg s−1。这四次γ射线爆发在近红外、光学和紫外波段都有相应的事件，峰值在同一时间被观测到。X射线和γ射线的活动性基本一致，γ射线通量变化与光学通量变化具有很强的相关性，两个波段之间没有时间滞后，变化幅度相当。这种γ射线/光学关系与成功解释低能通量和光谱行为的几何模型一致，表明长期通量变化主要是由于发射区视角变化产生的多普勒因子的变化。射电和高能辐射之间的行为差异，可以归因于产生它们的发射的喷流区域的不同视角。
We present a multiwavelength study of the flat-spectrum radio quasar CTA 102 during 2013–2017. We use radio-to-optical data obtained by the Whole Earth Blazar Telescope, 15 GHz data from the Owens Valley Radio Observatory, 91 and 103 GHz data from the Atacama Large Millimeter Array, near-infrared data from the Rapid Eye Monitor telescope, as well as data from theSwift(optical-UV and X-rays) andFermi(γ-rays) satellites to study flux and spectral variability and the correlation between flux changes at different wavelengths. Unprecedented γ-ray flaring activity was observed during 2016 November–2017 February, with four major outbursts. A peak flux of (2158 ± 63) × 10−8ph cm−2s−1, corresponding to a luminosity of (2.2 ± 0.1) × 1050erg s−1, was reached on 2016 December 28. These four γ-ray outbursts have corresponding events in the near-infrared, optical, and UV bands, with the peaks observed at the same time. A general agreement between X-ray and γ-ray activity is found. The γ-ray flux variations show a general, strong correlation with the optical ones with no time lag between the two bands and a comparable variability amplitude. This γ-ray/optical relationship is in agreement with the geometrical model that has successfully explained the low-energy flux and spectral behaviour, suggesting that the long-term flux variations are mainly due to changes in the Doppler factor produced by variations of the viewing angle of the emitting regions. The difference in behaviour between radio and higher energy emission would be ascribed to different viewing angles of the jet regions producing their emission.