Quasi-periodic Oscillation of Blazar PKS 1424–418 in γ-Ray Band
Quasi-periodic Oscillation of Blazar PKS 1424–418 in γ-Ray Band
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DOI：
10.1088/1538-3873/abd152
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发表时间：
2021-02
影响因子：
3.5
通讯作者：
Jianping Yang;G. Cao;B. Zhou;Long-hua Qin
中科院分区：
文献类型：
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作者：
Jianping Yang;G. Cao;B. Zhou;Long-hua Qin
本文对2009年5月12日至2019年9月17日的耀变体PKS 1424−418 (MJD 54963−58743)γ射线（0.1-300 GeV）波段的准周期振荡（QPO）进行了分析。利用谱域方法，Bhatta & Dhital报告说，该源在γ射线通量中具有353天的周期通量振荡。采用时域方法，我们证实了之前检测到的可能的γ射线QPO为~ 355天，具有高显著性水平。结合时域和谱域两种方法，为QPO的存在提供了更有力的证据。特别是在最强耀斑之后，γ射线光曲线与整个观测周期相比具有更强的周期显著性。假设QPO来自于超大质量双黑洞系统的轨道运动，该源主黑洞的质量估计为M ~ 3.5 × 108-5.5 × 109 M⊙。
We perform the quasi-periodic oscillation (QPO) analysis of blazar PKS 1424−418 in the γ-ray (0.1–300 GeV) band from 2009 May 12 to 2019 September 17 (MJD 54963−58743). Using the spectral domain methods, Bhatta & Dhital reported that this source has 353 days periodic flux oscillations in the γ-ray flux. Adopting time domain methods, we confirm the previous detection that a possible γ-ray QPO of ∼355 days with the high significance level. Combining two methods of time domain and spectral domain provides stronger evidence for the existence of the QPO. Especially, after the strongest flare, γ-ray light-curve exhibits stronger periodic significance compared with the whole observation period. Assuming that the QPO is come from the orbital motion in a supermassive binary black hole system, the mass of primary black hole for this source is estimate as M ∼ 3.5 × 108–5.5 × 109 M ⊙.