Simultaneous optical g, r, i monitoring and IDV periodic analysis for quasar 3C 454.3
Simultaneous optical g, r, i monitoring and IDV periodic analysis for quasar 3C 454.3
复制标题
类星体 3C 454.3 的同步光学 g、r、i 监测和 IDV 周期性分析
DOI：
10.1088/1674-4527/19/10/142
复制
发表时间：
2019
影响因子：
1.8
通讯作者：
Minfeng Gu
中科院分区：
文献类型：
--
作者：
Jun-Hui Fan;Yu-Hai Yuan;Hong Wu;Feng Wang;Jun Tao;Minfeng Gu
利用位于中国科学院国家天文台兴隆站的1.26米国家天文台-广州大学红外/光学望远镜（NAGIOT），我们在2016年10月23日至2016年12月15日的15个夜晚，首次获得了419组g，r和i波段的同时观测数据，目标是类星体3C 454.3。根据我们的观测结果，我们研究了太阳的光变、亮度与色指数的关系以及周期性变化。分析表明：1。在g、r和i波段的最大变化为Δ mg| max = 1.015 ± 0.042 mag，Δ mr| max = 1.188 ± 0.050 mag和Δ mi| max = 1.305 ± 0.057 mag。2.在我们的15个夜间监测项目中，在一个晚上（11月2日）检测到日内变异。此外，亮度增加了A = 15.86%，超过50.8分钟，然后下降了A = 22.42%，超过40.1分钟。经过一个小的明亮状态，其亮度再次增加了18.1%，超过55分钟的g波段。类似的现象也发生在r和i波段。2016年11月2日三个波段的日内变化表明周期为105分钟，这意味着黑洞质量为MBH =（0.3 $> 1.85）× 109 M⊙。3.颜色指数和星等之间存在反相关性，这表明当光源变亮时，它会变得更红。
With the 1.26 m National Astronomical Observatory-Guangzhou University Infrared/Optical Telescope (NAGIOT) at Xinglong Station of National Astronomical Observatories, Chinese Academy of Sciences, we obtained 419 groups of simultaneous observations at g, r and i bands, for the first time, targeting quasar 3C 454.3 during 15 nights from 2016 October 23 to 2016 December 15. Based on our observations, we investigate the optical variabilities, the relation between brightness and color index, and the periodicity variability. The presented analyses demonstrate that: 1. The maximum variations at the g, r and i bands are Δ mg|max = 1.015 ± 0.042 mag, Δ mr|max = 1.188 ± 0.050 mag and Δ mi|max = 1.305 ± 0.057 mag respectively. 2. During our 15 night monitoring program, intra-day variability was detected on one night (Nov. 2). Also, the brightness increased by A = 15.86% over 50.8 min, then decreased by A = 22.42% over 40.1 min. After a small bright state, its brightness increased again by 18.1% over 55 min at the g band. Similar phenomena happened at r and i bands. The intra-day variabilities at the three bands on 2016 November 2 indicate a period of 105 min, which implies a black hole mass of MBH = (0.3 ∼ 1.85) × 109 M⊙. 3. There is an anti-correlation between color index and magnitude, suggesting the source becomes redder when it brightens.