Quasiperiodic Behavior in the γ-Ray Light Curve of the Blazar PKS 0405-385

Gong, Yunlu; Zhou, Liancheng; Yuan, Min; Zhang, Haiyun; Yi, Ting-Feng; Fang, Jun

doi:10.3847/1538-4357/ac6c8c

Cited by 10 publications

(7 citation statements)

References 84 publications

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“…PG 1553+113 is the first blazar for which a quasiperiodic oscillation with a period of ∼2.18 ± 0.08 yr has been observed in its γ-ray light curve (Ackermann et al 2015). Quasiperiodic oscillations are generally thought to result of the helical motion within a jet (e.g., Raiteri et al 2015;Zhou et al 2018) or supermassive black hole binary system (e.g., Caproni et al 2017;Gong et al 2022). Since the black hole binary system may generate helical motion, there is no contradiction between the previous two scenarios.…”

Section: Discussionmentioning

confidence: 99%

A Geometric Model to Interpret the γ-Ray Quasiperiodic Oscillation of PG 1553+113

Gao

Qin

et al. 2023

ApJ

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We propose a jet helical motion model to explain the γ-ray quasiperiodic oscillation of PG 1553+113. In this model, we hypothesize that a relativistic jet with constant angular velocity rotates around the axis, causing the Doppler factor of the jet to vary over time, leading to periodic changes in flux. In addition, we consider that the parameters of the emission field vary slightly during the observation period and can be obtained by directly fitting their multiwavelength spectra. Then, we use the resulting emission field information and the model to reproduce the light curve. Our model successfully explains the 2.18 ± 0.08 yr γ quasiperiodic oscillation of PG 1553+113, which is consistent with previous studies. Most importantly, we notice an upward trend in the light curve, and we suggest that this upward trend is due to long-term variability with a timescale of ∼42 yr.

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Section: Discussionmentioning

confidence: 99%

A Geometric Model to Interpret the γ-Ray Quasiperiodic Oscillation of PG 1553+113

Gao

Qin

et al. 2023

ApJ

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“…Blazar light curves can also be modeled by an autoregressive (AR) process. We further fit the selected radio light curve with an independent method called autoregressive integrated moving average (ARIMA) model (e.g., Zhang et al 2017b;Feigelson et al 2018;Caceres et al 2019;Tarnopolski et al 2020;Sarkar et al 2021;Gong et al 2022) to check the reliability of this year-like QPO signal and assess whether the time series is consistent with a stochastic origin of the AR noise. An ARIMA process combined an autoregressive (AR) process and a moving average (MA) process after differencing a nonstationary time series.…”

Section: Light-curve Modelingmentioning

confidence: 99%

Radio and γ-Ray Variability in Blazar S5 0716+714: A Year-like Quasi-periodic Oscillation in the Radio Light Curve

Yang

Cai

et al. 2023

ApJ

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The nearly 33 yr long-term radio light curve obtained with the Metsähovi Radio Observatory 14 m telescope at 37 GHz and the recent 12.7 yr γ-ray light curve of the blazar S5 0716+714 at 0.1–300 GeV from the Fermi Large Area Telescope (Fermi-LAT) were analyzed by using the Lomb–Scargle periodogram and the weighted wavelet Z-transform techniques. In the radio light curve, we discovered a possible quasi-periodic oscillation (QPO) signal of about 352 ± 23 days at a confidence level of ∼3σ. We recalculated the periodicity and its significance in a chosen time range that has higher variability and denser sampling, and then found that the significance had increased to a confidence level of 99.996% (∼4.1σ). This QPO component was further confirmed by fitting a linear autoregressive integrated moving average model to the selected radio light curve. A possible QPO of 960 ± 80 days at a 99.35% level (∼2.7σ) was found in the γ-ray light curve, which generally agrees with the earlier QPO claims of S5 0716+714. This paper discusses possible mechanisms for this potential year-like QPO. One possibility is a pure geometrical scenario with blobs moving helically inside the jet. Another is a supermassive binary black hole involving a gravitational wave-driven regime. In the latter scenario, we derived a milliparsec separation in the binary system that undergoes coalescence within a century due to the emission of low-frequency gravitational waves.

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“…It should be noted that helical jet models have been linked to blazar variability in other objects, e.g., OJ 287 (Valtonen & Pihajoki 2013), CTA 102 (Sarkar et al 2020), AO 0235+164 (Wang & Jiang 2020), 0405-385 (Gong et al 2022), 0716+714 (Hong et al 2018), and3FGL J0449.4-4350 (Yang et al 2020). They have also been invoked to explain oscillations in the polarization variability of the prototype radio galaxy M87 (Perlman et al 2011).…”

Section: Disk-jet Couplingmentioning

confidence: 99%

A QPO in Mkn 421 from Archival RXTE Data

Smith¹,

Oramas²,

Perlman³

2023

ApJ

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We report a 325(−7, +8) day quasi-periodic oscillation (QPO) in the X-ray emission of the blazar Mkn 421 based on data obtained with the Rossi X-ray Timing Explorer satellite. The QPO is seen prominently in the ASM data (at least 15 cycles) due to the fact that it has had near-continuous sampling for more than a decade. The PCA data, where the sampling is not uniform and shows many large gaps, provide supporting evidence at lower significance. The QPOs are an important observable in accretion disks, can be modulated by various orbital timescales, and may be generated by a number of mechanisms. They have been studied extensively in X-ray binaries and should be present in active galactic nuclei (AGN) if they are governed by a common set of physical principles. In jetted sources, QPOs can probe jet–disk interactions or helical oscillations. This QPO has previously been claimed intermittently in X-ray, radio, and gamma-ray data, but the continuous, 15 yr extent (1996–2011) of the ASM observations (in which Mkn 421 is the brightest AGN observed) provides a unique window. The QPO appears to be present for nearly the entire extent of the ASM observations. We explore various physical origins and modulating mechanisms, particularly interpretations of the QPO as a result of disk–jet interactions, due to either an accretion disk limit cycle, jet instabilities, or helical motions. Limit cycle oscillations would not interact with either Keplerian or Lense–Thirring modulated oscillations; however, those associated with jet instabilities or helical motions in the jet would likely be modulated by Lense–Thirring precession.

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Quasiperiodic Behavior in the γ-Ray Light Curve of the Blazar PKS 0405-385

Cited by 10 publications

References 84 publications

A Geometric Model to Interpret the γ-Ray Quasiperiodic Oscillation of PG 1553+113

A Geometric Model to Interpret the γ-Ray Quasiperiodic Oscillation of PG 1553+113

Radio and γ-Ray Variability in Blazar S5 0716+714: A Year-like Quasi-periodic Oscillation in the Radio Light Curve

A QPO in Mkn 421 from Archival RXTE Data

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