Long-term Study of the Light Curve of PKS 1510-089 in GeV Energies

Prince, Raj; Majumdar, P.; Gupta, Nayantara

doi:10.3847/1538-4357/aa78f4

Cited by 34 publications

(39 citation statements)

References 28 publications

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“…These time instants are completely ignored in our fastest variability analysis. The shortest variability time is found to be t var = 1.08±0.01 hr between MJD 57761.47 -57761.53; which is consistent with the hour scale variability found for other FSRQ like PKS 1510-089 (Prince et al 2017). We also found that the variability time during flares in Fermi-LAT data varies in the range of 1 hour to several days.…”

Section: Variabilitysupporting

confidence: 88%

Fermi-Large Area Telescope Observations of the Brightest Gamma-Ray Flare Ever Detected from CTA 102

Prince¹,

Raman²,

Hahn³

et al. 2018

ApJ

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We present a multi-wavelength study of the FSRQ CTA 102 using Fermi-LAT and simultaneous Swift-XRT/UVOT observations. The Fermi-LAT telescope detected one of the brightest flares from this object during Sep, 2016 to Mar, 2017 In the 190 days of observation period the source underwent four major flares. A detailed analysis of the temporal and spectral properties of these flares indicates the flare at MJD 57751.594 has a γ-ray flux of (30.12±4.48)×10 −6 ph cm −2 s −1 (from 90 minutes binning) in the energy range of 0.1-300 GeV. This has been found to be the highest flux ever detected from CTA 102. Time dependent leptonic modelling of the pre-flare, rising state, flares and decaying state has been done. A single emission region of size 6.5 × 10 16 cm has been used in our work to explain the multi-wavelength spectral energy distributions. During flares the luminosity in electrons increases nearly seventy times compared to the pre-flare state.

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Section: Variabilitysupporting

confidence: 88%

Fermi-Large Area Telescope Observations of the Brightest Gamma-Ray Flare Ever Detected from CTA 102

Prince¹,

Raman²,

Hahn³

et al. 2018

ApJ

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“…It is located at a redshift of z = 0.361 (Tanner et al 1996) with black hole mass 5.4×10 8 M ⊙ and accretion rate approximately 0.5 M ⊙ /yr (Abdo et al 2010). A long term analysis of the light curve of PKS 1510-089 with the eight year Fermi-LAT data has been done by Prince et al (2017) earlier. They have observed five major flares during 2008-2016, and their temporal and spectral features have been studied in detail.…”

Section: Introductionmentioning

confidence: 99%

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

Prince

Gupta

Nalewajko

2019

ApJ

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PKS 1510-089 is one of the most variable blazars in the third Fermi-LAT source catalog. During 2015, this source has shown four flares identified as flare A, B, C, and D in between three quiescent states Q1, Q2, and Q3. The multiwavelength data from Fermi-LAT, Swift-XRT/UVOT, OVRO, and SMA Observatory are used in our work to model these states. Different flux doubling times have been observed in different energy bands which indicate there could be multiple emission zones. The flux doubling time from the gamma-ray and X-ray light curve are found to be 10.6 hr, 2.5 days, and the average flux doubling time in the optical/UV band is 1 day. It is possible that the gamma-ray and optical/UV emission are produced in the same region whereas X-ray emission is coming from a different region along the jet axis. We have also estimated the discrete correlations functions (DCFs) among the light curves of different energy bands to infer about their emission regions. However, our DCF analysis does not show significant correlation in different energy bands though it shows peaks in some cases at small time lags. We perform a two-zone multi-wavelength time-dependent modeling with one emission zone located near the outer edge of the broad line region (BLR) and another further away in the dusty/molecular torus (DT/MT) region to study this high state.

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“…3(Abdo et al 2011), PKS 1510-089(Prince et al 2017)). There are four scenarios that are usually used to explain the observed spectral curvature/break (see, e.g.,Georganopoulos et al 2001;Abdo et al 2009;Poutanen & Stern 2010;Ackermann et al 2010;Stern & Poutanen 2014): 1) the "cooling break" resulting from the radiative losses of highenergy electrons, 2) the attenuation of high-energy photons by the extragalactic background light (EBL), 3) the transition of Compton scattering cross-section from the Thomson regime to the Klein-Nishina (K-N) regime, and 4) the photon-photon pair absorption associated with the He II Lyman continuum (LyC) or H LyC.…”

mentioning

confidence: 99%

Exploring the Origin of Multiwavelength Activities of High-redshift Flat-spectrum Radio Quasar PKS 1502+106 during 2014–2018

Ding

Geng

et al. 2019

ApJ

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The origin of the multi-band activities (outbursts/flares) of blazars is still a heavily debated topic. Shock and magnetic reconnection have long been considered as possible triggers for the multi-band activities. In this paper, we present an exploration of the origin of multi-band activities for a high-redshift (z =1.8385) FSRQ PKS 1502+106. Utilizing multi-band data from radio to γ-ray and optical polarization observations, we investigate two dramatic activities in detail: a γ-ray dominated outburst in 2015 and an optical dominated outburst in 2017. Our main results are as follows. (I) A fast γ-ray flare with a flux-doubling time-scale as short as 1-hr in 2015 is discovered. Based on the variability time-scale, the physical parameters of the flaring region (e.g, minimum Doppler factor, emission region size, etc.) are constrained. At the peak of the flare, the γ-ray spectrum hardens to Γ γ = 1.82 ± 0.04 and exhibits an obvious curvature/break characteristic that is caused by the typical "cooling break". Modelings of multi-band SEDs reveal a very hard electronic energy spectrum with the electronic spectral index of 1.07 ± 0.53. This result suggests that this fast γ-ray flare may be triggered by magnetic reconnection. (II) During the outburst in 2017, the optical polarization degree and optical fluxes show a very tight correlation. By analyzing Stokes parameters of polarization observations, our results show that this outburst could be triggered by a transverse shock with a compression ratio of η > 2.2, and the magnetic field intensity of the shock emission region is about 0.032 G.

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Long-term Study of the Light Curve of PKS 1510-089 in GeV Energies

Cited by 34 publications

References 28 publications

Fermi-Large Area Telescope Observations of the Brightest Gamma-Ray Flare Ever Detected from CTA 102

Fermi-Large Area Telescope Observations of the Brightest Gamma-Ray Flare Ever Detected from CTA 102

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

Exploring the Origin of Multiwavelength Activities of High-redshift Flat-spectrum Radio Quasar PKS 1502+106 during 2014–2018

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