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Fast Optical Variability of the TeV Blazar PKS 1725+123 Observed by SVOM-VT and Insights from Multiwavelength Follow-up Observations

  • Authors: Shuo-Yu Liu, Yu-Wei Yu, Ji-Shun Lian, Xin-Ke Hu, Alexis Coleiro, Zhu-Heng Yao, Li-Ping Xin, Jing Wang, Hua-Li Li, Zi-Qi Wang, Jin Zhang, Floriane Cangemi, Bertrand Cordier, Antoine Foisseau, Olivier Godet, Andrea Goldwurm, Diego Götz, Sébastien Guillot, Xu-Hui Han, Ning Jiang, Cyril Lachaud, Sébastien Le Stum, En-Wei Liang, Pierre Maggi, Yu-Lei Qiu, Jérôme Rodriguez, Lian Tao, Jian-Yan Wei, Chao Wu, Liang Zhang, Shuang-Nan Zhang, Shi-Jie Zheng

Shuo-Yu Liu et al 2026 The Astrophysical Journal Letters 1005 .

  • Provider: AAS Journals

Caption: Figure 7.

Light curves of PKS 1725+123 observed by Fermi-LAT in the 0.1–1000 GeV band. If TS < 9, an upper limit (represented by open inverted triangles) is provided for that time bin. Panel (a): the 17 yr long-term light curve, derived with a time bin of 30 days. The red horizontal dashed line denotes the ∼17 yr average flux, i.e., F0.1−1000 GeV = (2.12 ± 0.10) × 10−11 erg cm−2 s−1. Panel (b): the 3 month light curve with a time bin of 1 day, covering the period from 2025 July 6 to 2025 October 1. The blue horizontal dashed line denotes the weighted average flux of 2.65 × 10−10 erg cm−2 s−1, which is derived using Equation (1). The two black vertical lines represent the capture time interval of the three time-resolved spectra in Figure 5.

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