Analyzing polarization swings in 3C 279

Kiehlmann, S.; Savolainen, Tuomas; Jorstad, S. G.; Sokolovsky, K. V.; Schinzel, F. K.; Agudo, I.; Arkharov, A. A.; Benítez, E.; Berdyugin, A.; Blinov, D.; Bochkarev, N. G.; Borman, G. A.; Burenkov, A. N.; Casadio, C.; Doroshenko, V. T.; Ефимова, Н. В.; Fukazawa, Yasushi; Gómez, J. L.; Hagen-Thorn, V. A.; Heidt, J.; Hiriart, D.; Itoh, R.; Joshi, M.; Kimeridze, G. N.; Константинова, Т. С.; Kopatskaya, E. N.; Korobtsev, I.; Kovalev, Y. Y.; Krajci, Tom; Kurtanidze, O. M.; Kurtanidze, S. O.; Ларионов, В. М.; Ларионова, Е. Г.; Larionova, L.; Lindfors, E.; López, Erick Gómez Tagle; Marscher, A. P.; McHardy, I. M.; Molina, S. N.; Morozova, D. A.; Назаров, С. В.; Nikolashvili, M. G.; Nilsson, K.; Pulatova, N. G.; Reinthal, R.; Sadun, A. C.; Сергеев, С. Г.; Sigua, L. A.; Sorcia, M.; Spiridonova, O. I.; Takalo, L. O.; Taylor, B.; Troitsky, I. S.; Ugolkova, L. S.; Zensus, J. A.; Zhdanova, V. E.

doi:10.1051/epjconf/20136106003

Cited by 12 publications

(8 citation statements)

References 13 publications

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“…The results of our simulations are different from those reported by Kiehlmann et al (2013) because they assumed variability due to random effects, used a large number of components (30), and attributed random values for Q and U instead of intensity, PD, and PA, as in our case. The analysis was carried out based on a sample with a regular small time interval of three days and, as was also pointed by the authors, poorer sampled light curves can introduce large artificial rotations.…”

Section: Stokes Parameters Of a New Componentcontrasting

confidence: 82%

Multiwavelength flaring activity of PKS 1510-089

Beaklini

Dominici

Abraham

2017

A&A

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Aims. In this work, we analyse the multiwavelength brightness variations and flaring activity of FSRQ PKS1510-089, aiming to constrain the position of the emission sources. Methods. We report 7 mm (43 GHz) radio and R-band polarimetric observations of PKS1510-089. The radio observations were performed at the Itapetinga Radio Observatory, while the polarimetric data were obtained at the Pico dos Dias Observatory. The 7 mm observations cover the period between 2011 and 2013, while the optical polarimetric observations were made between 2009 and 2012.Results. At 7 mm, we detected a correlation between four radio and γ-ray flares with a delay of about 54 days between them; the higher frequency counterpart occurred first. Using optical polarimetry, we detected a large variation in polarization angle (PA) within two days associated with the beginning of a γ-ray flare. Complementing our data with other data obtained in the literature, we show that PA presented rotations associated with the occurrence of flares. Conclusions. Our results can be explained by a shock-in-jet model, in which a new component is formed in the compact core producing an optical and/or γ-ray flare, propagates along the jet, and after some time becomes optically thin and is detected as a flare at radio frequencies. The variability in the polarimetric parameters can also be reproduced; we can explain large variation in both PA and polarization degree (PD), in only one of them, or in neither, depending on the differences in PA and PD between the jet and the new component.

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Section: Stokes Parameters Of a New Componentcontrasting

confidence: 82%

Multiwavelength flaring activity of PKS 1510-089

Beaklini

Dominici

Abraham

2017

A&A

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“…We have three seasons of polarimetric data and four seasons of photometric data. Having the same data as Kiehlmann et al (2013) we see the same behaviour. In the third and fourth seasons we see rotations that rotate in one direction and then back on themselves.…”

Section: C 279supporting

confidence: 62%

“…In the period prior to the the start of the RINGO2 program the source showed a rapid decline in magnitude over the period of ∼1 month synchronous with an increase in polarisation degree and a 180 • rotation of the position angle ((Abdo et al 2010b). Kiehlmann et al (2013), using data from RINGO2 and KVA-60 amongst other instruments, showed there was an increase in flux and degree of polarisation along with a ∼150 • rotation of the position angle in May 2011 (MJD 55700) the addition of Fermi data showed that during this period of ∼2 months the γ-ray flux decreases by ∼100 [10 −8 cm −2 s −1 ] (Aleksić et al 2014a). Aleksić et al (2014a) interpreted this optical outburst with a rotation of the position angle and the increase in the degree of polarisation as geometric and relativistic aberration effects such as an emission knot's trajectory bending such that it crosses the observer's line of sight (for full description see Aleksić et al (2014a)).…”

Section: C 279mentioning

confidence: 98%

The RINGO2 and DIPOL optical polarization catalogue of blazars

Jermak¹,

Steele²,

Lindfors³

et al. 2016

Mon. Not. R. Astron. Soc.

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We present ∼2000 polarimetric and ∼3000 photometric observations of 15 γ-ray bright blazars over a period of 936 days (11/10/2008 -26/10/2012) using data from the Tuorla blazar monitoring program (KVA DIPOL) and Liverpool Telescope (LT) RINGO2 polarimeters (supplemented with data from SkyCamZ (LT) and Fermi-LAT γ-ray data). In 11 out of 15 sources we identify a total of 19 electric vector position angle (EVPA) rotations and 95 flaring episodes. We group the sources into subclasses based on their broadband spectral characteristics and compare their observed optical and γ-ray properties. We find that (1) the optical magnitude and γ-ray flux are positively correlated, (2) EVPA rotations can occur in any blazar subclass, 4 sources show rotations that go in one direction and immediately rotate back, (3) we see no difference in the γ-ray flaring rates in the sample; flares can occur during and outside of rotations with no preference for this behaviour, (4) the average degree of polarisation (DoP), optical magnitude and γ-ray flux are lower during an EVPA rotation compared with during non-rotation and the distribution of the DoP during EVPA rotations is not drawn from the same parent sample as the distribution outside rotations, (5) the number of observed flaring events and optical polarisation rotations are correlated, however we find no strong evidence for a temporal association between individual flares and rotations and (6) the maximum observed DoP increases from ∼10% to ∼30% to ∼40% for subclasses with synchrotron peaks at high, intermediate and low frequencies respectively.

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“…(2007), Kiehlmann et al (2013), Blinov et al (2015), and Kiehlmann et al (2016), we assumed that some amount of magnetic turbulence is at work in the optical emitting region and we ran Monte Carlo simulations to see whether we can reproduce a photopolarimetric behaviour resembling that shown in Fig. 8.…”

Section: Discussionmentioning

confidence: 99%

Synchrotron emission from the blazar PG 1553+113. An analysis of its flux and polarization variability

Raiteri

Nicastro

Stamerra

et al. 2016

Mon. Not. R. Astron. Soc.

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In 2015 July 29 -September 1 the satellite XMM-Newton pointed at the BL Lac object PG 1553+133 six times, collecting data for 218 hours. During one of these epochs, simultaneous observations by the Swift satellite were requested to compare the results of the X-ray and optical-UV instruments. Optical, near-infrared and radio monitoring was carried out by the Whole Earth Blazar Telescope (WEBT) collaboration for the whole observing season. We here present the results of the analysis of all these data, together with an investigation of the source photometric and polarimetric behaviour over the last three years. The 2015 EPIC spectra show slight curvature and the corresponding light curves display fast X-ray variability with a time scale of the order of 1 hour. In contrast to previous results, during the brightest X-ray states detected in 2015 the simple log-parabolic model that best-fits the XMM-Newton data also reproduces reasonably well the whole synchrotron bump, suggesting a peak in the near-UV band. We found evidence of a wide rotation of the polarization angle in 2014, when the polarization degree was variable, but the flux remained almost constant. This is difficult to interpret with deterministic jet emission models, while it can be easily reproduced by assuming some turbulence of the magnetic field.

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Analyzing polarization swings in 3C 279

Cited by 12 publications

References 13 publications

Multiwavelength flaring activity of PKS 1510-089

Multiwavelength flaring activity of PKS 1510-089

The RINGO2 and DIPOL optical polarization catalogue of blazars

Synchrotron emission from the blazar PG 1553+113. An analysis of its flux and polarization variability

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