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∼3.5נ10⁸–5.5נ10⁹ M _⊙.

我们对2009年5月12日至2019年9月17日（MJD 54963−58743）的γ射线（0.1–300 GeV）波段的Blazar PKS 1424−418进行了准周期振荡（QPO）分析。Bhatta＆Dhital使用光谱域方法报告说，该源在γ射线通量中具有353天的周期性通量振荡。采用时域方法，我们确认了先前的发现，即约355天的γ射线QPO具有较高的显着性水平。时域和频谱域两种方法的结合为QPO的存在提供了更有力的证据。特别是在最强的耀斑之后，γ与整个观察期相比，射线光曲线具有更强的周期性意义。假设QPO在一个超大二进制黑洞系统来自轨道运动，主黑洞于此源的质量估计作为中号~3.5נ10 ⁸ -5.5נ10 ⁹ 中号 _⊙。