Optical microvariability of EGRET blazars

Romero, Gustavo E.; Cellone, S. A.; Combi, J. A.; Andruchow, I.

doi:10.1051/0004-6361:20020743

Cited by 123 publications

(141 citation statements)

References 30 publications

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“…Timescales for 3C 279 flares at gamma rays seem to have similar duration as the optical timescales here reported, suggesting a common origin. In the case of CTA 102, although we have found no intra-night variability, such events were reported in the past (Romero et al 2002). It could be the case that the emission region is more compact and the gamma rays are produced at larger distances, e.g.…”

Section: Discussioncontrasting

confidence: 49%

Optical Variability Monitoring for Gamma ray Blazars: preliminary results

Combi¹,

Andruchow²,

Cellone³

et al. 2009

Proceedings of Workshop on Blazar Variability Across the Electromagnetic Spectrum — PoS(BLAZARS2008)

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Section: Discussioncontrasting

confidence: 49%

Optical Variability Monitoring for Gamma ray Blazars: preliminary results

Combi¹,

Andruchow²,

Cellone³

et al. 2009

Proceedings of Workshop on Blazar Variability Across the Electromagnetic Spectrum — PoS(BLAZARS2008)

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“…CTA 102 also shows a jet with superluminal motions of up to 21 c, derived from VLBI observations (see, Jorstad et al 2001;Rantakyrö et al 2003;Jorstad et al 2005). Its history of optical variability can be tracked back to 1973 (Pica et al 1988), with sporadic detections afterwards (see, for example, Wilkes et al 1994;Ghosh et al 2000;Véron-Cetty & Véron 2001;Romero et al 2002). We report here a clear internight variability in both R and V bands.…”

Section: Pks 1510−089supporting

confidence: 50%

“…Its emission spans from radio wavelengths to gamma-rays, including optical and X-ray bands (Kataoka et al 2008;Cusumano et al 2010). This quasar has an extensive history of long and short-term variability at optical bands (see, for example, Liller & Liller 1975;Pica et al 1988;Villata et al 1997;Romero et al 2002;Cellone et al 2007), with continuous changes in brightness over long periods of time. Moreover, optical polarization has been detected with variability both in P and in position angle θ (Andruchow et al 2005), as well as a rapid variation in γ-rays (D' Ammando et al 2009).…”

Section: Pks 1510−089mentioning

confidence: 99%

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Optical flux behaviour of a sample ofFermiblazars

Marchesini

Andruchow

Cellone

et al. 2016

A&A

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Aims. We aim at investigating the time-behaviour of a sample of gamma-ray blazars. We present the results from a 13 monthlong optical photometry monitoring campaign of the blazars PKS 0048−097, PKS 0754+100, [HB89] 0827+243, PKS 0851+202, PKS 1253−055, PKS 1510−089, PKS 1749+096, PKS 2230+114 and PKS 2251+158. Methods. We analyse the variability of each object, focusing on different time-scales (long term, short term, and microvariability), in an attempt to achieve a statistical comparison of the results. Results. After applying a geometric model to explain the variability results, we found that it is possible that a slight change in the direction of the jet generates the variations detected in some objects during this campaign.

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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

166

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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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Optical microvariability of EGRET blazars

Cited by 123 publications

References 30 publications

Optical Variability Monitoring for Gamma ray Blazars: preliminary results

Optical Variability Monitoring for Gamma ray Blazars: preliminary results

Optical flux behaviour of a sample ofFermiblazars

The Spectral Energy Distributions of Fermi Blazars

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