Multiwavelength intraday variability of the BL Lacertae S5 0716+714

Gupta, Alok C.; Krichbaum, T. P.; Wiita, Paul J.; Rani, Bindu; Sokolovsky, K. V.; Mohan, Prashanth; Mangalam, A.; Marchili, N.; Fuhrmann, L.; Agudo, I.; Bach, U.; Bachev, R.; Böttcher, M.; Gabányi, K. É.; Gaur, Haritma; Hawkins, Keith; Kimeridze, G. N.; Kurtanidze, O. M.; Kurtanidze, S. O.; Lee, Chung-Uk; Liu, X; McBreen, B.; Nesci, R.; Nestoras, G; Nikolashvili, M. G.; Ohlert, J.; Palma, N.; Peneva, S.; Pursimo, T.; Semkov, E.; Strigachev, A.; Webb, J. R.; Wiesemeyer, H.; Zensus, J. A.

doi:10.1111/j.1365-2966.2012.21550.x

Cited by 61 publications

(43 citation statements)

References 82 publications

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“…S5 0716+714 is a prominent blazar in optical bands and has shown variability on diverse timescales from minutes through hours to days (e.g. Heidt & Wagner 1996;Nesci et al 1998;Giommi et al 1999;Raiteri et al 1999;Raiteri et al 2003;Gupta et al 2008;Gupta et al 2012;Agarwal et al 2016) in radio to X ray bands (e.g. Wagner et al 1996;Raiteri et al 2003 and references therein).…”

Section: S5 0716+714mentioning

confidence: 99%

Core shift effect in blazars

Agarwal

Mohan

Gupta

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We studied the pc-scale core shift effect using radio light curves for three blazars, S5 0716+714, 3C 279 and BL Lacertae, which were monitored at five frequencies (ν) between 4.8 GHz and 36.8 GHz using the University of Michigan Radio Astronomical Observatory (UMRAO), the Crimean Astrophysical Observatory (CrAO), and Metsahovi Radio Observatory for over 40 years. Flares were Gaussian fitted to derive time delays between observed frequencies for each flare (∆t), peak amplitude (A), and their half width. Using A ∝ ν α we infer α in the range −16.67 to 2.41 and using ∆t ∝ ν 1/kr , we infer k r ∼ 1, employed in the context of equipartition between magnetic and kinetic energy density for parameter estimation. From the estimated core position offset (Ω rν ) and the core radius (r core ), we infer that opacity model may not be valid in all cases. The mean magnetic field strength at 1 pc (B 1 ) and at the core (B core ), are in agreement with previous estimates. We apply the magnetically arrested disk model to estimate black hole spins in the range 0.15 − 0.9 for these blazars, indicating that the model is consistent with expected accretion mode in such sources. The power law shaped power spectral density has slopes −1.3 to −2.3 and is interpreted in terms of multiple shocks or magnetic instabilities.

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Section: S5 0716+714mentioning

confidence: 99%

Core shift effect in blazars

Agarwal

Mohan

Gupta

et al. 2017

Monthly Notices of the Royal Astronomical Society

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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

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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“…It shows optical variabilities in the whole electromagnetic band with timescales from minutes to years. Intra-day variabilities (IDVs) have been studied by many authors (Poon et al 2009;Liu et al 2012;Gupta et al 2012;Bhatta et al 2013;Man et al 2016;Lee et al 2016, etc.). Gupta et al (2009) obtained timescales of 25 min; Rani et al (2010) obtained timescales of 15 min; Man et al (2016) obtained timescales of 17.6 min; and Bhatta et al (2016) displayed the variability based on the A&A 605, A43 (2017) peak-to-peak variations of 30% and "bluer-when-brighter" spectral evolution.…”

Section: Introductionmentioning

confidence: 99%

Optical monitoring of BL Lac object S5 0716+714 and FSRQ 3C 273 from 2000 to 2014

Yuan

Fan

Tao

et al. 2017

A&A

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Context. Using the 1.56 m telescope at the Shanghai Observatory (ShAO), China, we monitored two sources, BL Lac object S5 0716+714 and flat spectrum radio quasar (FSRQ) 3C 273. For S5 0716+714, we report 4969 sets of CCD (Charge-coupled Device) photometrical optical observations (1369 for V band, 1861 for R band and 1739 for I band) in the monitoring time from Results. The two sources both show IDV properties for S5 0716+714. The timescales are in the range from 17.3 min to 4.82 h; for 3C 273, the timescale is ∆T = 35.6 min. Based on the periodic analysis methods, we find the periods P V = 24.24 ± 1.09 days, P R = 24.12 ± 0.76 days, P I = 24.82 ± 0.73 days for S5 0716+714, and P = 12.99 ± 0.72, 21.76 ± 1.45 yr for 3C 273. The two sources displayed the "bluer-when-brighter" spectral evolution properties. Conclusions. S5 0716+714 and 3C 273 are frequently studied objects. The violent optical variability and IDV may come from the jet. Gaussian fitting can be used to analyze IDVs. The relations between brightness (flux density) and spectrum are strongly influenced by the frequency.

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Multiwavelength intraday variability of the BL Lacertae S5 0716+714

Cited by 61 publications

References 82 publications

Core shift effect in blazars

Core shift effect in blazars

The Spectral Energy Distributions of Fermi Blazars

Optical monitoring of BL Lac object S5 0716+714 and FSRQ 3C 273 from 2000 to 2014

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