Evidence of jet-caused 12-year optical periodicity of blazar OJ 287

The variability data for the BL Lacertae object TXS 1902+556 in the optical and γ-ray wavebands were obtained from the 0.76 m Katzman Automatic Imaging Telescope and the Fermi Large Area Telescope (Fermi-LAT), covering periods of 14.4 years and 14.7 years, respectively. The variability properties were systematically analyzed, with particular emphasis on the first comprehensive investigation of radiation variation in the optical waveband. Four well-established techniques were employed for this purpose: the Lomb-Scargle periodogram, REDFIT program, Jurkevich method, and discrete correlation function (DCF) approach. The optical waveband exhibits quasi-periodic oscillations (QPO) with a timescale of PO = 276.8 ± 6.1 days at a significance level 3.87σ, while the γ-ray waveband does not exhibit any significant periodicity. However, it should be noted that the QPO timescale is consistent with the Sun-gaps in the optical light curve within 2σ uncertainties. The optical QPO behavior is most likely attributed to the helical motion of the jet driven by the orbital motion in a supermassive black hole binary system. Moreover, we have provided an explanation for the absence of QPO in the γ-ray light curves. Furthermore, utilizing the DCF method, a weak correlation between the variability in the optical and γ-ray wavebands was observed, suggesting that the emission of TXS 1902+556 may be generated through a combination of synchrotron self-Compton (SSC) and external Compton (EC) processes, or a leptonic-hadronic hybrid process.

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Correlation and evolution of the blazar S5 1803+784 short-term variability properties during 01.2022-01.2023

Butuzova,

Gorbachev,

Guseva

et al. 2024

Modern Astronomy: From the Early Universe to Exoplanets and Black Holes

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The blazar S5 1803+784 has a unique high temporal resolution data series for about a year provided by the TESS satellite. By performing our aperture photometry of summarized on 10-30 the full-frame image cuts to reduce Poisson noise, we obtained the blazar light curve from 01.2022 to 01.2023. Using a new method for determining the shortest characteristic variability time and supplementing the study with data from long-term multiband ZTF and AZT-8 observations, we trace the evolution of the micro-variability parameters and their correlation to the long-term variability characteristics. We draw a conclusion regarding the mechanism, forming the S5 1803+784 micro-variability.

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Evidence of jet-caused 12-year optical periodicity of blazar OJ 287

Cited by 4 publications

References 63 publications

A new method for studying the blazar variability on the shortest time scales and its application to S5 1803+784

A new method for studying the blazar variability on the shortest time scales and its application to S5 1803+784

Optical and γ-ray variability analysis of BL Lacertae object TXS 1902+556

Correlation and evolution of the blazar S5 1803+784 short-term variability properties during 01.2022-01.2023

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