Detection of a quasi-periodic oscillation in γ-ray light curve of the high redshift blazar B2 1520+31

Gupta, Alok C.; Tripathi, Ashutosh; Wiita, Paul J.; Kushwaha, Pankaj; Zhang, Zhongli; Bambi, Cosimo

doi:10.1093/mnras/stz395

Cited by 56 publications

(58 citation statements)

References 87 publications

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“…Another clue of the jet physics will come from polarization models, as evidenced by the promising but simplistic cylindrical relativistic polarization signatures of the EVPA, DOP, and Doppler boosted flux profiles, as predicted by [51]; this will be an additional and useful tool to extract jet properties by doing detailed fits to polarization observations. There is an oscillatory behavior seen in both γ-ray and optical light curves [11][12][13][14][15][16]66,67] that supports the above trend. There is also evidence of the radio structure that is supported by the basic model of [52] as observed by [68,69].…”

Section: Relativistic Jet Model For the Optical And γ Ray Qpossupporting

confidence: 63%

A Relativistic Orbit Model for Temporal Properties of AGN

Rana¹,

Mangalam²

2020

Galaxies

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We present a unified model for X-ray quasi-periodic oscillations (QPOs) seen in Narrow-line Seyfert 1 (NLSy1) galaxies, γ-ray and optical band QPOs that are seen in Blazars. The origin of these QPOs is attributed to the plasma motion in corona or jets of these AGN. In the case of X-ray QPOs, we applied the general relativistic precession model for the two simultaneous QPOs seen in NLSy1 1H 0707-945 and deduce orbital parameters, such the radius of the emission region, and spin parameter a for a circular orbit; we obtained the Carter’s constant Q, a, and the radius in the case of a spherical orbit solution. In other cases where only one X-ray QPO is seen, we localized the orbital parameters for NLSy1 galaxies REJ 1034+396, 2XMM J123103.2+110648, MS 2254.9-3712, Mrk 766, and MCG-06-30-15. By applying the lighthouse model, we found that a kinematic origin of the jet based γ-ray and optical QPOs, in a relativistic MHD framework, is possible. Based on the inbuilt Hamiltonian formulation with a power-law distribution in the orbital energy of the plasma consisting of only circular or spherical trajectories, we show that the resulting Fourier power spectral density (PSD) has a break corresponding to the energy at ISCO. Further, we derive connection formulae between the slopes in the PSD and that of the energy distribution. Overall, given the preliminary but promising results of these relativistic orbit models to match the observed QPO frequencies and PSD at diverse scales in the inner corona and the jet, it motivates us to build detailed models, including a transfer function for the energy spectrum in the corona and relativistic MHD jet models for plasma flow and its polarization properties.

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Section: Relativistic Jet Model For the Optical And γ Ray Qpossupporting

confidence: 63%

A Relativistic Orbit Model for Temporal Properties of AGN

Rana¹,

Mangalam²

2020

Galaxies

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“…One possible model (for QPOs with tens of days period) involve hotspots rotating in the innermost stable circular orbit (ISCO) orbit of the SMBH (e.g., Zhang & Bao 1991;Gupta et al 2009). Here the optical periodic flux modulation comes from the circular motion of the hotspot which modulates the seed photon field for the external Compton (EC) interaction with the particles in the jet, thereby producing modulation in the γ-ray flux (Gupta et al 2009(Gupta et al , 2019. This model is not favored, firstly since blazar emissions are mostly jet dominated in the optical band as well.…”

Section: Discussionmentioning

confidence: 99%

“…Blazar multi-wavelength (MW) flux variability is, in general, stochastic, but quasi-periodic variations (QPOs) have been reported occasionally (Valtaoja et al 1985;Carrasco et al 1985;Quirrenbach et al 1991;Urry et al 1993;Sillanpaa et al 1996;Heidt & Wagner 1996;Raiteri et al 2003;Espaillat et al 2008;Gupta et al 2008Gupta et al , 2009Gupta et al , 2019Lachowicz et al 2009;King et al 2013;Sandrinelli et al 2014Sandrinelli et al , 2016Sandrinelli et al , 2017Gupta 2014Gupta , 2018Ackermann et al 2015;Bhatta 2017Bhatta , 2019Zhang et al 2017;Hong et al 2018, and references therein). The suggested QPO time scales also have a huge range, similar to the variability time scales shown by blazars, that is, from a few tens of minutes to hours, days, months and even years.…”

Section: Introductionmentioning

confidence: 99%

“…Further, given the complex physics and not yet fully understood connections between different constituents and jets of AGNs, their imprints, if any, are expected to be reflected in the jet emission. In this context, the continuous monitoring capability of the Fermi-LAT instrument provides an excellent facility to explore bright extragalactic γ-ray sources, most of which are blazars, on both short and long time scales (e.g., Shukla et al 2018;Kushwaha et al 2017;Gupta et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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Multi-waveband quasi-periodic oscillations in the light curves of blazar CTA 102 during its 2016–2017 optical outburst

Sarkar

Kushwaha

Gupta

et al. 2020

A&A

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Context. Quasi-periodic fluctuations in the light curves of blazars can provide insight into the underlying emission process. This type of flux modulation hints at periodic physical processes that result in emission. CTA 102, a flat spectrum radio quasar at a redshift of 1.032, has displayed significant activity since 2016. The multi-waveband light curve of CTA 102 shows signs of quasi-periodic oscillations during the 2016–2017 flare. Aims. Our goal is to rigorously quantify the presence of any possible periodicity in the emitted flux during the mentioned period and to explore the possible causes that can give rise to it. Methods. Techniques such as the Lomb-Scargle periodogram and weighted wavelet z-transform were employed to observe the power emitted at different frequencies. To quantify the significance of the dominant period, Monte-Carlo techniques were employed to consider an underlying smooth bending power-law model for the power spectrum. In addition, the light curve was modeled using an autoregressive process (AR1) to analytically obtain the significance of the dominant period. Lastly, the light curve was modeled using a generalized autoregressive integrated moving average (ARIMA) process to check whether introducing a seasonal (periodic) component results in a statistically preferable model. Results. Highly significant, simultaneous quasi-periodic oscillations (QPOs) were observed in the γ-ray and optical fluxes of blazar CTA 102 during its highest optical activity episode in 2016–2017. The periodic flux modulation had a dominant period of ∼7.6 days and lasted for ∼8 cycles (MJD 57710–57770). All of the methods used point toward significant (> 4σ) quasi-periodic modulation in both γ-ray and optical fluxes. Conclusions. Several possible models were explored while probing the origin of the periodicity, and by extension, the 2016–2017 optical flare. The best explanation for the detected QPO appears to be a region of enhanced emission (blob), moving helically inside the jet.

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“…where the upper limit corresponds to models that imply a high BH mass (low QPO excitation radius) and the lower limit to models giving a low BH mass (high QPO excitation radius, Goluchová et al, 2019). Finally, we also note that, very recently, Gupta et al (2019) discussed a gamma ray QPO in the high-redshift blazar B2 1520+31. Using the ISCO frequency relation, they found the upper limit on the BH mass to be M ≈ 10 10 M .…”

Section: Discussionmentioning

confidence: 76%

Exploring the X-ray universe via timing: mass of the active galactic nucleus black hole XMMUJ134736.6+173403

Šrámková¹,

Goluchová²,

Török³

et al. 2019

Proc. IAU

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A strong quasi-periodic modulation has recently been revealed in the X-ray flux of the X-ray source XMMUJ134736.6+173403. The two observed twin-peak quasiperiodic oscillations (QPOs) exhibit a 3:1 frequency ratio and strongly support the evidence for the presence of an active galactic nucleus black hole (AGN BH). It has been suggested that detections of twin-peak QPOs with commensurable frequency ratios and scaling of their periods with BH mass could provide the basis for a method intended to determine the mass of BH sources, such as AGNs. Assuming the orbital origin of QPOs, we calculate the upper and lower limit on the AGN BH mass M, reaching M ≍ 107–109M⊙. Compared to mass estimates of other sources, XMMUJ134736.6+173403 appears to be the most massive source with commensurable QPO frequencies, and its mass represents the current observational upper limit on the AGN BH mass obtained from the QPO observations.

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Detection of a quasi-periodic oscillation in γ-ray light curve of the high redshift blazar B2 1520+31

Cited by 56 publications

References 87 publications

A Relativistic Orbit Model for Temporal Properties of AGN

A Relativistic Orbit Model for Temporal Properties of AGN

Multi-waveband quasi-periodic oscillations in the light curves of blazar CTA 102 during its 2016–2017 optical outburst

Exploring the X-ray universe via timing: mass of the active galactic nucleus black hole XMMUJ134736.6+173403

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