The blazar PG 1553+113 is hypothesized to harbor a supermassive black hole binary system, a scenario that aligns with its observed physical characteristics. In this study, we re-examine the authenticity of the periodicity of PG 1553+113 by conducting a comprehensive analysis of multi-wavebands periodic light variations, using the updated light curve data of more than 15 years. We used two methods to search for the light curves data of this blazar in gamma-ray, X-ray, optical and radio bands. The multi-wavebands analysis approach enables a thorough verification of the observed periodic patterns. The result of gamma-ray detection showed a quasi-periodic oscillation (QPO) of 2.16 years, which verified the results given by Ackermann et al. (2015). And the optical band shows a QPO of 2.24 years. We analyzed the correlation among gamma-ray, optical and radio bands, and we found that there is a strong correlation among them, and the emission of different bands coming from the same region (the same electron group). Finally, we estimated the black hole mass of PG 1553+113 to be M similar or equal to 4.3 x 10(9) M-circle dot based on the binary black hole model.

In this work, we report for the first time two repeated transient quasiperiodic oscillations (QPOs) in the γ -ray light curve of the TeV blazar 3C 279. We search for the periodicity in the light curve and estimate its confidence level using the weighted wavelet Z-transform, the Lomb–Scargle periodogram, and the REDFIT techniques. The main results are as follows: (1) a QPO of ∼33 days (>2.5 σ ) is found during the flare of 117 days (MJD 55008–55125) from 2009 June to November. Interestingly, the same QPO (∼39 days) reappeared in the flaring duration from MJD 59430 to 59585, with the confidence level of > 4 σ . (2) Another transient QPO of ∼91 days with a significance of >3.8 σ is found during a period with 455 days (MJD 58430–58985) from 2019 February to 2020 May. Under the premise of considering the QPOs reported in the literature, the QPO of ∼40 days is repeated three times and the QPO of ∼91 days is repeated twice. We discuss several physical models explaining the QPOs of this blazar. Our study may suggest that the two QPOs originate from the twin jets of the binary black holes at the center of 3C 279. The repeated occurrence of QPOs of a similar scale strongly supports the geometric scenario of a blob spiraling within the jet. Furthermore, the hypothesis of a sheath in the jet may also be a potential explanation for the repetitive γ -ray flare patterns observed in the light curve.

We report the results of time series analysis of blazar PKS 1440-389, observed by the Transiting Exoplanet Survey Satellite (TESS) in two sectors. We find that the source has a quasi-periodic oscillation (QPO) of about 3.1 days for sector 11 and around 3.7 days for sector 38 in the optical band. We use two methods to assess the QPO and its confidence level: Lomb–Scargle periodogram and weighted wavelet Z-transforms. We explore various potential explanations for these rapid quasi-periodic variations and propose that their source most likely resides within the innermost region of the accretion disk. Within this framework, we estimate the mass of the central black hole of this blazar. We obtain black hole masses of 6.65 × 108M⊙ (Schwarzschild black hole) and 4.22 × 109M⊙ (maximally rotating Kerr black hole), with a main period of 3.7 days. Finally, we utilize the kink instability model to explain the QPO.

多波段相关性分析对研究耀变体(Blazar)的物理模型和辐射机制具有重要意义。为了研究TeV耀变体的物理模型，依据4FGL-DR3目录中78个TeV耀变体的对应体的名称及坐标， 对他们的γ 射线波段数据和光学波段数据进行了搜索和整理，发现同时具有光学波段和γ 射线波段数据的TeV耀变体共56 个。利用离散相关函数计算每个耀变体光学和γ射线的相关性，计算结果显示，有20个源表现出弱的γ 射线-光学相关性，有30个源表现出强的γ 射线-光学相关性，有6个源没有表现出相关性。在表现出强相关性的源中，光学波段和γ 射线波段间还表现出不同程度的时间延迟。这些结果支持了TeV 耀变体高能光子主要来自轻子模型的同步自康普顿辐射。但是同时还发现不管是光学波段还是γ 射线波段，存在一些“孤峰”，这些“孤峰”可能暗示了低能光子的来源不是唯一的。

Fermi-LAT LCR provides continuous and regularly sampled gamma-ray light curves, spanning about 14 yr, for a large sample of blazars. The log-normal flux distribution and linear rms–flux relation of the light curves for a few Fermi blazars have been examined in previous studies. However, the probability that blazars exhibit the log-normal flux distribution and linear rms–flux relation in their gamma-ray light curves has not been systematically explored. In this study, we comprehensively research the distribution of γ -ray flux and the statistical characteristics on a large sample of 1414 variable blazars from the Fermi-LAT LCR catalog, including 572 FSRQs, 477 BL Lacs, and 365 BCUs, and statistically compare their flux distributions with normal and log-normal distributions. The results indicate that the probability of not rejecting log-normal is 42.05% for the large sample, and there is still a 2.05% probability of not rejecting normality, based on the joint of Kolmogorov–Smirnov, Shapiro–Wilk, and Normality tests. We further find that the probability that BL Lacs conform to the log-normal distribution is higher than that of FSRQs. Besides, after removing sources with less than 200 data points from this large sample, a sample of 549 blazars, which is still a large sample compared to the previous studies, was obtained. Based on dividing the light curves into segments every 20 points (or 40 points, or one year), we fitted the linear rms–flux relation of these three different sets and found that the Pearson correlation coefficients are all close to 1 for most blazars. This result indicates a strong linear correlation between the rms and the flux of these 549 blazars. The log-normal distribution and linear rms–flux relation indicate that the variability of the γ -ray flux for most blazars is a non-linear and multiplicative process.

凌日系外行星巡天卫星(Transiting Exoplanet Survey Satellite，TESS)观测到的耀变体PKS 0422+004(α =04 24 46. 8421990080，δ =+00 36 06. 329375028)的光学波段光变曲线在第32扇区存在约7.4天的准周期振荡( Quasiperiodic Oscillation, QPO)。 使用LSP( Lomb Scargle Periodogram)方法寻找显著性周期，并用加权小波Z变换(Weight Wavelet Z-transform，WWZ)方法进行时频域分析进一步验证。最后，基于施瓦西黑洞(a =0)和极端克尔黑洞(a =0. 998 2)两种模型，估算了这个耀变体中心黑洞的质量。以7. 4天为主周期， 得到黑洞质量分别为1. 11 × 109M☉(施瓦西黑洞)和7. 07 × 109M☉(极端克尔黑洞)。