Two-zone Emission Modeling of PKS 1510-089 during the High State of 2015

Prince, Raj; Gupta, Nayantara; Nalewajko, Krzysztof

doi:10.3847/1538-4357/ab3afa

Cited by 27 publications

(25 citation statements)

References 53 publications

(70 reference statements)

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“…They estimated the disk contribution at 5100 Å to the total flux during one quiescent state (Q2 between MJD = 57 180−57 208; see Fig. 3 of Prince et al 2019). The disk contribution is found to be ∼44% of the total flux at 5100 Å, lower than that estimated from the NTD but consistent within the margin of error.…”

Section: Size-luminosity Relationmentioning

confidence: 76%

“…Similar to other radio-loud AGNs, PKS 1510-089 shows strong flux variation across the entire electromagnetic spectrum from radio to γ ray (e.g., Malkan & Moore 1986;Tavecchio et al 2000;Bach et al 2007;Abdo et al 2010a;Marscher et al 2010;Orienti et al 2013;H.E.S.S. Collaboration 2013;Kushwaha et al 2016;Beaklini et al 2017;Castignani et al 2017;Prince et al 2019). However, the BLR of PKS 1510-089 remains poorly studied due to its strong radio emission, although the size of its BLR is an important model parameter in the multi-band SED fitting.…”

Section: Introductionmentioning

confidence: 73%

“…This contribution can also be roughly estimated from the broad-band SED. Prince et al (2019) studied the broad-band SED of PKS 1510-089 in several active and quiescent states in 2015 (MJD = 57 000−57 350). They modeled the broad-band SED using a time-dependent two-zone emission model and estimated the synchrotron, synchrotron self-Compton (SSC), and inverse-Compton emission.…”

Section: Size-luminosity Relationmentioning

confidence: 99%

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Broad line region and black hole mass of PKS 1510-089 from spectroscopic reverberation mapping

Rakshit

2020

A&A

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Reverberation results of the flat spectrum radio quasar PKS 1510-089 from 8.5 years of spectroscopic monitoring carried out at Steward Observatory over nine observing seasons between December 2008 and June 2017 are presented. Optical spectra show strong Hβ, Hγ, and Fe II emission lines overlying on a blue continuum. All the continuum and emission line light curves show significant variability with fractional root-mean-square variations of 37.30 ± 0.06% (f5100), 11.88 ± 0.29% (Hβ), and 9.61 ± 0.71% (Hγ); however, along with thermal radiation from the accretion disk, non-thermal emission from the jet also contributes to f5100. Several methods of time series analysis (ICCF, DCF, von Neumann, Bartels, JAVELIN, χ2) are used to measure the lag between the continuum and line light curves. The observed frame broad line region size is found to be 61.1−3.2+4.0 (64.7−10.6+27.1) light-days for Hβ (Hγ). Using the σline of 1262 ± 247 km s−1 measured from the root-mean-square spectrum, the black hole mass of PKS 1510-089 is estimated to be 5.71−0.58+0.62 × 107 M⊙.

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Section: Size-luminosity Relationmentioning

confidence: 76%

Section: Introductionmentioning

confidence: 73%

Section: Size-luminosity Relationmentioning

confidence: 99%

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Broad line region and black hole mass of PKS 1510-089 from spectroscopic reverberation mapping

Rakshit

2020

A&A

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“…Both light curves exhibit similar flux variations of about a factor two. While this correlation can provide insights for modelling attempts, it is noteworthy that it is not a common feature in flares in PKS 1510-089 (e.g., Nalewajko et al 2012;Ahnen et al 2017;Prince et al 2019).…”

Section: Comparison Between the Multiwavelength Light Curvesmentioning

confidence: 99%

H.E.S.S. and MAGIC observations of a sudden cessation of a very-high-energyγ-ray flare in PKS 1510−089 in May 2016

Abdalla¹,

Adam²,

Aharonian³

et al. 2021

A&A

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The flat spectrum radio quasar (FSRQ) PKS 1510−089 is known for its complex multiwavelength behaviour and it is one of only a few FSRQs detected in very-high-energy (VHE, E > 100 GeV) γ rays. The VHE γ-ray observations with H.E.S.S. and MAGIC in late May and early June 2016 resulted in the detection of an unprecedented flare, which revealed, for the first time, VHE γ-ray intranight variability for this source. While a common variability timescale of 1.5 h has been found, there is a significant deviation near the end of the flare, with a timescale of ∼20 min marking the cessation of the event. The peak flux is nearly two orders of magnitude above the low-level emission. For the first time, a curvature was detected in the VHE γ-ray spectrum of PKS 1510–089, which can be fully explained by the absorption on the part of the extragalactic background light. Optical R-band observations with ATOM revealed a counterpart of the γ-ray flare, even though the detailed flux evolution differs from the VHE γ-ray light curve. Interestingly, a steep flux decrease was observed at the same time as the cessation of the VHE γ-ray flare. In the high-energy (HE, E > 100 MeV) γ-ray band, only a moderate flux increase was observed with Fermi-LAT, while the HE γ-ray spectrum significantly hardens up to a photon index of 1.6. A search for broad-line region (BLR) absorption features in the γ-ray spectrum indicates that the emission region is located outside of the BLR. Radio very-long-baseline interferometry observations reveal a fast-moving knot interacting with a standing jet feature around the time of the flare. As the standing feature is located ∼50 pc from the black hole, the emission region of the flare may have been located at a significant distance from the black hole. If this is indeed a true correlation, the VHE γ rays must have been produced far down in the jet, where turbulent plasma crosses a standing shock.

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“…These hadronic models require very high magnetic fields (∼100 G) and much harder proton spectrum, which seems to be unnatural (Bottacini et al 2016). Some studies invoked multiple emission regions in order to get more satisfactory fit (Berger et al 2011;Tavecchio et al 2012;Boettcher & Baring 2019;Prince, Gupta & Nalewajko 2019). Time-dependant leptonic and hadronic models were used by some authors to calculate the radiating particle distribution solving the Fokker-Planck equation considering various acceleration processes and these models are helpful to understand the evolution of blazar SED during significant flux variations (Zheng et al 2013;Saito et al 2015;Asano & Hayashida 2018;Das, Prince & Gupta 2020).…”

mentioning

confidence: 99%

Multiwavelength study of the quiescent states of six brightest flat-spectrum radio quasars detected by Fermi-LAT

Roy

Patel

Sarkar

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The regular monitoring of flat-spectrum radio quasars (FSRQs) in γ-rays by Fermi-LAT since past 12 years indicated six sources who exhibited extreme γ-ray outbursts crossing daily flux of 10−5 photons cm−2 s−1. We obtained nearly-simultaneous multi-wavelength data of these sources in radio to γ-ray waveband from OVRO, Steward Observatory, SMARTS, Swift-UVOT, Swift-XRT and Fermi-LAT. The time-averaged broadband Spectral Energy Distributions (SEDs) of these sources in quiescent states were studied to get an idea about the underlying baseline radiation processes. We modeled the SEDs using one-zone leptonic synchrotron and inverse-Compton emission scenario from broken power-law electron energy distribution inside a spherical plasma blob, relativistically moving down a conical jet. The model takes into account inverse-Compton scattering of externally and locally originated seed photons in the jet. The big blue bumps visible in quiescent state SEDs helped to estimate the accretion disk luminosities and central black hole masses. We found a correlation between the magnetic field inside the emission region and the ratio of emission region distance to disk luminosity, which implies that the magnetic field decreases with an increase in emission region distance and decrease in disk luminosity, suggesting a disk-jet connection. The high-energy index of the electron distribution was also found to be correlated with observed γ-ray luminosity as γ-rays are produced by high energy particles. In most cases, kinetic power carried by electrons can account for jet radiation power as jets become radiatively inefficient during quiescent states.

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Two-zone Emission Modeling of PKS 1510-089 during the High State of 2015

Cited by 27 publications

References 53 publications

Broad line region and black hole mass of PKS 1510-089 from spectroscopic reverberation mapping

Broad line region and black hole mass of PKS 1510-089 from spectroscopic reverberation mapping

H.E.S.S. and MAGIC observations of a sudden cessation of a very-high-energyγ-ray flare in PKS 1510−089 in May 2016

Multiwavelength study of the quiescent states of six brightest flat-spectrum radio quasars detected by Fermi-LAT

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