Detection of a high-confidence quasi-periodic oscillation in radio light curve of the high redshift FSRQ PKS J0805–0111

Ren, Guo-Wei; Zhang, Haojing; Zhang, Xiong; Ding, Nan; Yang, Xing; Li, Fu-Ting; Pei-lin, YAN; Xu, Xiaolin

doi:10.1088/1674-4527/21/3/075

Cited by 11 publications

(8 citation statements)

References 44 publications

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“…Unlike those found in gamma-ray, these X-ray QPO signals oscillate on timescales of hours or days, and no reliable QPO signals have been reported on long timescales (year-like oscillation) (Stella & Vietri 1998;Gierliński et al 2008;Lin et al 2013;Pan et al 2016;Zhang et al 2017bZhang et al , 2018. FSRQ J1359+4011, PKS J0805-0111 and BL Lac PKS 0219-164, PKS J2134-0153 are reported to have QPO signals in the radio band, most of which are on the timescale of years (King et al 2013;Bhatta 2017;Ren et al 2021aRen et al , 2021b. S5 0716+714 is a very famous BL Lac object, which has been monitored by many telescopes for a long time, and has a redshift of z = 0.31 (Donato et al 2001).…”

Section: Introductionmentioning

confidence: 89%

A 31.3 day Transient Quasiperiodic Oscillation in Gamma-ray Emission from Blazar S5 0716+714

Chen

Gong

et al. 2022

ApJ

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We systematically search for quasiperiodic oscillatory (QPO) signals on the month timescale among the 1525 sources given in the Fermi Large Area Telescope Light Curve Repository. We find a transient QPO of 31.3 ± 1.8 days in the gamma-ray band light curve of the TeV blazar S5 0716+714, which has seven cycles (MJD 55918–56137) for the first time by weighted wavelet Z-transform and Lomb–Scargle periodogram methods. Monte Carlo simulations based on the power spectral density and probability distribution function were used to evaluate the confidence level of the QPO, and the result is ∼4.1σ. Seasonal autoregressive integrated moving average modeling of the light curve revealed it is a significant physical QPO. The physical models to explain the sporadic month-timescale QPOs in the blazar were discussed. Our studies indicate that the helical jet model and blob move helically in a curved jet model to properly explain this kind of transient QPO.

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Section: Introductionmentioning

confidence: 89%

A 31.3 day Transient Quasiperiodic Oscillation in Gamma-ray Emission from Blazar S5 0716+714

Chen

Gong

et al. 2022

ApJ

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“…in which f j is the frequency of the QPO being attempted in units of 1 day −1 (Ren et al 2021a(Ren et al , 2021b, P x (ω j ) is the power spectrum ((…”

Section: Lsp Methodsmentioning

confidence: 99%

“…The blazar spectral energy distribution (SED) is double peaked. The peaks ranging from X-rays to γrays are produced by the inverse Compton (IC) process, whereas the peaks ranging from radio to X-rays are produced by the synchrotron radiation of relativistic electrons within the jet (Ren et al 2021a(Ren et al , 2021b. According to the location of the SED peak, the blazars are divided into three types: low synchrotron peaked (Lomb-Scargle periodogram (LSP)) (ν peak < 10 14 Hz), intermediate synchrotron peaked (ISP) (10 14 Hz ν peak 10 15 Hz), and high synchrotron peaked (HSP) (ν peak > 10 15 Hz) (Abdo et al 2010;Hong et al 2017;Iyida et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Research on a 44 Day Quasi-periodic Oscillation of Optical Bands for BL Lac S5 0716+714

Lu,

Sun,

Fang

et al. 2024

ApJ

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By means of astronomical observation data from the 60 cm Telescope at Yunnan Observatory, optical data in the g, r, and i bands were collected for BL Lac S5 0716+714, spanning from 2017 November 10 to 2018 May 15. The original data set contains 21,396 quasi-simultaneous multiband points, with 7132 data points for each band. The Lomb–Scargle periodogram method and the weighted wavelet Z-transform method were used to search for a quasi-periodic oscillation (QPO) signal in the data. For the first time, we report a QPO signal at 44 ± 6 days with a final significance of 3.98σ. Further analysis of the spectrum index reveals that the 44 day QPO signal is most likely explained by a helical motion of a blob with velocity β in the jet, where the viewing angle of the emission region in the jet undergoes periodic variations. In addition, we employed the hypothesis testing method (the null hypothesis) to analyze the flux distribution and determined that a double log-normal distribution provides a better fit; thus, there may be two radiative mini-regions within a jet in this source, so this 44 day QPO signal may be superimposed on a longer-term outburst.

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“…Recently, many interesting cases of quasiperiodic oscillation (QPO) have been detected in the electromagnetic emissions of AGNs at multiple wavelengths from radio frequencies to GeV γ-rays. The periods of these QPO signals span the timescale range from minutes to years (Kidger et al 1992;Fan & Lin 2000;Valtonen et al 2006Valtonen et al , 2008Valtonen et al , 2023Gierliński et al 2008;King et al 2013;Lin et al 2013;Sandrinelli et al 2014Sandrinelli et al , 2016Ackermann et al 2015;Pan et al 2016;B.-K. Zhang et al 2014, J. Zhang et al 2017a, P. Zhang et al 2017b, P.-f. Zhang et al 2017c, 2017d, 2018Bhatta 2017Bhatta , 2018Li et al 2017;Yan et al 2018;Zhou et al 2018;Ren et al 2021;Yang et al 2021;Zhang & Wang 2021;Chen et al 2022;Gong et al 2022, 2023, andreferences therein). Several special cases of them are summarized here; for example, Zhang & Wang (2021) claimed a discovery of a QPO of 176 days of the NLSy1 galaxy J0849 +5108 in the 11 yr radio light curve obtained with the Owens Valley Radio Observatory 40 m telescope at 15 GHz.…”

Section: Introductionmentioning

confidence: 99%

A Possible Optical Quasiperiodic Oscillation of 134 days in the Radio-loud Narrow-line Seyfert 1 Galaxy TXS 1206+549 at z = 1.34

Ren,

Sun,

Zhang

2024

ApJ

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Here we report an optical quasiperiodic oscillation (QPO) with a period of ∼134 days detected in g- and r-band light curves of the narrow-line Seyfert 1 galaxy TXS 1206+549 at a redshift of 1.34 with data from observations at the Zwicky Transient Facility (ZTF). After considering the trial factor, the significance levels in the two bands are 3.1σ and 2.6σ, respectively. The QPO signal presents about 10 cycles ranging from 2018 March to 2021 December, thus lasting ∼4 yr. A nearly sinusoidal profile also appears in the folded light curves by using a phase-resolved analysis. Interestingly, in the simultaneous light curve with the timescale of ZTF observations, a potential periodic signal with a similar period is detected in the o-band light curve from Asteroid Terrestrial-impact Last Alert System data; additionally, a weak peak is also detected at a similar period in the γ-ray light curve obtained from Fermi Gamma-ray Space Telescope data. Some potential origins of periodicities in active galactic nuclei are discussed for the QPO reported here.

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Detection of a high-confidence quasi-periodic oscillation in radio light curve of the high redshift FSRQ PKS J0805–0111

Cited by 11 publications

References 44 publications

A 31.3 day Transient Quasiperiodic Oscillation in Gamma-ray Emission from Blazar S5 0716+714

A 31.3 day Transient Quasiperiodic Oscillation in Gamma-ray Emission from Blazar S5 0716+714

Research on a 44 Day Quasi-periodic Oscillation of Optical Bands for BL Lac S5 0716+714

A Possible Optical Quasiperiodic Oscillation of 134 days in the Radio-loud Narrow-line Seyfert 1 Galaxy TXS 1206+549 at z = 1.34

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