Time-dependent simulations of emission from the FSRQ PKS 1510−089: multiwavelength variability of external Compton and synchrotron self-Compton models

Chen, Xuhui; Fossati, G.; Böttcher, M.; Liang, Edison

doi:10.1111/j.1365-2966.2012.21283.x

Cited by 46 publications

(49 citation statements)

References 56 publications

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“…It was suggested that the inverse Compton (IC) emission in FSRQ was produced through the synchrotron self-Compton (SSC) mechanism or from external seed photons from the BLRs. These photons would be up-scattered by the synchrotron electrons (e.g., Chen et al 2012). The longstanding unified scheme for radio-loud AGN proposes that the Fanaroff-Riley I and II radio galaxies (Fanaroff & Riley 1974) are the underlying progenitors of BL Lacs and FSRQs galaxies (Bicknell 1995;Fossati et al 1998).…”

Section: Introductionmentioning

confidence: 99%

Anatomy of a blazar in the (sub-)millimeter: ALMA observations of PKS 0521-365

Léon

Cortés

Guerard

et al. 2016

A&A

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Aims. We aim at analyzing the (sub-)millimeter emission in a nearby blazar, PKS 0521-365, to study the synchrotron and thermal emission in the different components detected at low frequency. Methods. We analyzed the archive public data of the ALMA Cycle 0 where PKS 0521-365 is used as a calibrator. A total of 13 projects with 23 dataset were analyzed in Bands 3, 6, and 7 and combined. The whole set of data was combined and wavelet-filtered to obtain a deep image toward PKS 0521-365, reaching a dynamic range of 47 000. The individual emission flux was measured on different dates over a period of 11 months in various components. Finally we analyzed the spectral energy distribution (SED) in each different component, including the radio jet and counter jet. Results. The point sources detected in the field follow a similar distribution to previous studies. The blazar flux shows large variation especially in Band 3. Different components are observed: core, radio jet, and newly detected counter jet, hot spot (HS), and a disky structure roughly perpendicular to the jet. The HS emission is formed by a point source surrounded by an extended emission. The viewing angle of the jet is about 30• with a Doppler factor of δ = 1.6. The HS is at a distance of 19 kpc from the center. The SED analysis shows a strong variation in the core spectral index, especially in Band 3. The two components in the radio jet have roughly a flat spectral index in Bands 6 and 7. Conclusions. The different weak and extended components in PKS 0521-365 are detected with the ALMA data. The analysis of both jets constrains the geometrical distance of the HS to the center. The SED presents a different shape in time and frequency for each component. Finally, a new structure is detected roughly perpendicular to the radio jet. and a thermal emission origin is currently favored. Further observations at higher spatial resolution are needed to confirm that hypothesis.

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Section: Introductionmentioning

confidence: 99%

Anatomy of a blazar in the (sub-)millimeter: ALMA observations of PKS 0521-365

Léon

Cortés

Guerard

et al. 2016

A&A

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“…( Abdo et al 2009a( Abdo et al , 2010bAcero et al 2015;Ackermann et al 2011aAckermann et al ,b, 2015Aller et al 2011;Bai, et al 1998;Bastieri et al 2011;Chen et al, 2012;Fan & Xie 1996;Fan et al 2011;Ghisellini et al 2010;Gu 2014;Gu & Li 2013;Gupta 2011;Gupta et al 2012;Hu, et al 2006;Marscher et al 2011;Nolan et al 2012;Romero et al 2002;Urry 2011;Wills et al 1992;Wu, et al 2007;Yang et al 2010aYang et al ,b, 2012aYang et al ,b, 2014You & Cao, 2014). Quite recently, Massaro et al (2015) published the largest blazar sample (The 5th edition of the Roma-BZCAT, see the BZCAT 5.0 (http://www.asdc.asi.it/bzcat/).…”

Section: Introductionmentioning

confidence: 99%

The Spectral Energy Distributions of Fermi Blazars

Jiang¹,

Yang²,

Liu³

et al. 2016

ApJS

162

180

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In this paper, multi-wavelength data are compiled for a sample of 1425 Fermi blazars to calculate their spectral energy distributions (SEDs). A parabolic function, log(νF ν ) = P 1 (logν − P 2 ) 2 + P 3 , is used for SED fitting. Synchrotron peak frequency (logν p ), spectral curvature (P 1 ), peak flux (ν p F νp ), and integrated flux (νF ν ) are successfully obtained for 1392 blazars (461 flat spectrum radio quasarsFSRQs, 620 BL Lacs-BLs and 311 blazars of uncertain type-BCUs, 999 sources have known redshifts). Monochromatic luminosity at radio 1.4 GHz, optical R band, X-ray at 1 keV and γ-ray at 1 GeV, peak luminosity, integrated luminosity and effective spectral indexes of radio to optical (α RO ), and optical to X-ray (α OX ) are calculated. The "Bayesian classification" is employed to logν p in the rest frame for 999 blazars with available redshift and the results show that 3 components are enough to fit the logν p distribution, there is no ultra high peaked subclass. Based on the 3 components, the subclasses of blazars using the acronyms of Abdo et al. (2010a) are classified, and some mutual correlations are also studied. Conclusions are finally drawn as follows: (1) SEDs are successfully obtained for 1392 blazars. The fitted peak frequencies are compared with common sources from samples available ( Sambruna et al. 1996, Nieppola et al. 2006, 2008, Abdo et al. 2010a. (2) -2 -peak sources (ISPs) if 14.0 < log ν p (Hz) ≤ 15.3, and high synchrotron peak sources (HSPs) if log ν p (Hz) > 15.3. (3) γ-ray emissions are strongly correlated with radio emissions. γ-ray luminosity is also correlated with synchrotron peak luminosity and integrated luminosity. (4) There is an anti-correlation between peak frequency and peak luminosity within the whole blazar sample. However, there is a marginally positive correlation for HBLs, and no correlations for FSRQs or LBLs. (5) There are anti-correlations between the monochromatic luminosities (γ-ray and radio bands) and the peak frequency within the whole sample and BL Lacs. (6) The optical to X-ray (α OX ) and radio to optical (α RO ) spectral indexes are strongly anti-correlated with peak frequency (log ν p ) within the whole sample, but the correlations for subclasses of FSRQs, LBLs, and HBLs are different.

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“…4.1), we find γγ-pair production being negligible for the parameter set used for the above model fits and below the last LAT data point (Barnacka 2013). Chen et al (2012) modelled the last flare in the extended early 2009 flaring episode of this source by using a time-dependent Monte Carlo Fokker-Planck code, where the emission region is treated as an extended cylindrical volume within the jet. In addition to a particle "pick-up" term in the Fokker-Planck equation, they also included a stochastic acceleration term and took into account all external and internal target photon fields.…”

Section: Modeling the Pks 1510-089 Multifrequency Sedmentioning

confidence: 99%

Shaping the GeV-spectra of bright blazars

Reimer¹

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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Aims. The non-thermal spectra of jetted active galactic nuclei (AGN) show a variety of shapes and degree of curvature in their low-and high energy components. From some of the brightest Fermi-LAT blazars, prominent spectral breaks at a few GeV have been regularly detected, which is inconsistent with conventional cooling effects. We study the effects of continuous time-dependent injection of electrons into the jet with differing rates, durations, locations, and power-law spectral indices, and evaluate its impact on the ambient emitting particle spectrum that is observed at a given snapshot time in the framework of a leptonic blazar emission model. With this study, we provide a basis for analyzing ambient electron spectra in terms of injection requirements, with implications for particle acceleration modes. Methods. The emitting electron spectrum is calculated by Compton cooling the continuously injected electrons, where target photons are assumed to be provided by the accretion disk and broad line region (BLR). From this setup, we calculate the non-thermal photon spectra produced by inverse Compton scattering of these external target radiation fields using the full Compton cross-section in the head-on approximation.Results. By means of a comprehensive parameter study we present the resulting ambient electron and photon spectra, and discuss the influence of each injection parameter individually. We found that varying the injection parameters has a notable influence on the spectral shapes, which in turn can be used to set interesting constraints on the particle injection scenarios. By applying our model to the flare state spectral energy distribution (SED) of 3C 454.3, we confirm a previous suggestion that explained the observed spectral changes at a few GeV by a combination of the Compton-scattered disk and BLR radiation. We determine the required injection parameters for this scenario. We also show that this spectral turn-over can also be understood as Compton-scattered BLR radiation only, and provide the corresponding injection parameters. Here the spectral turn-over is explained by a corresponding break in the ambient electron spectrum. In a similar way, we also applied our model to the FSRQ PKS 1510-089, and present two possible model fits. Here, the GeVspectrum is either dominated by Compton-scattered accretion disk radiation or is a combination of Compton-scattered disk and BLR radiation. We provide the required injection parameters for these fits. In all four scenarios, we found that impulsive particle injection is disfavored. Conclusions. The presented injection model that is embedded in a leptonic blazar emission model for external Comptonloss dominated jets of AGN aims towards bridging jet emission with acceleration models using a phenomenological approach. Blazar spectral data can be analyzed with this model to constrain injection parameters, in addition to the conventional parameter values of steady-state emission models, if sufficient broad multifrequency coverage is provided.

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Time-dependent simulations of emission from the FSRQ PKS 1510−089: multiwavelength variability of external Compton and synchrotron self-Compton models

Cited by 46 publications

References 56 publications

Anatomy of a blazar in the (sub-)millimeter: ALMA observations of PKS 0521-365

Anatomy of a blazar in the (sub-)millimeter: ALMA observations of PKS 0521-365

The Spectral Energy Distributions of Fermi Blazars

Shaping the GeV-spectra of bright blazars

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