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RoboPol: first season rotations of optical polarization plane in blazars

D. BlinovAstronomical Institute, St Petersburg State University,Universitetsky pr. 28, Petrodvoretz, 198504 St Petersburg, RussiaV. PavlidouDepartment of Physics and Institute for Plasma Physics, University of Crete, GR-71003 Heraklion, GreeceI. E. PapadakisDepartment of Physics and Institute for Plasma Physics, University of Crete, GR-71003 Heraklion, GreeceS. KiehlmannMax-Planck-Institut fr Radioastronomie, Auf dem Hgel 69, D-53121 Bonn, GermanyG. V. PanopoulouDepartment of Physics and Institute for Plasma Physics, University of Crete, GR-71003 Heraklion, GreeceIoannis LiodakisDepartment of Physics and Institute for Plasma Physics, University of Crete, GR-71003 Heraklion, GreeceO. G. KingCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, MC 249-17, Pasadena, CA 91125, USAE. AngelakisMax-Planck-Institut fr Radioastronomie, Auf dem Hgel 69, D-53121 Bonn, GermanyMislav BalokovićCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, MC 249-17, Pasadena, CA 91125, USAH. DasInter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune 411 007, IndiaR. FeilerToru Centre for Astronomy, Nicolaus Copernicus University, Faculty of Physics, Astronomy and Informatics, Grudziadzka 5, PL-87-100 Toru, PolandL. FuhrmannMax-Planck-Institut fr Radioastronomie, Auf dem Hgel 69, D-53121 Bonn, GermanyT. HovattaAalto University Metshovi Radio Observatory, Metshovintie 114, FL-02540 Kylml, FinlandPravin KhodadeInter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune 411 007, IndiaA. J. KusToru Centre for Astronomy, Nicolaus Copernicus University, Faculty of Physics, Astronomy and Informatics, Grudziadzka 5, PL-87-100 Toru, PolandN. D. KylafisDepartment of Physics and Institute for Plasma Physics, University of Crete, GR-71003 Heraklion, GreeceAshish A MahabalCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, MC 249-17, Pasadena, CA 91125, USAI. MyserlisMax-Planck-Institut fr Radioastronomie, Auf dem Hgel 69, D-53121 Bonn, GermanyDeepa ModiInter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune 411 007, IndiaB. PazderskaToru Centre for Astronomy, Nicolaus Copernicus University, Faculty of Physics, Astronomy and Informatics, Grudziadzka 5, PL-87-100 Toru, PolandE. PazderskiToru Centre for Astronomy, Nicolaus Copernicus University, Faculty of Physics, Astronomy and Informatics, Grudziadzka 5, PL-87-100 Toru, PolandJ. PapamastorakisDepartment of Physics and Institute for Plasma Physics, University of Crete, GR-71003 Heraklion, GreeceT. J. PearsonCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, MC 249-17, Pasadena, CA 91125, USAChaitanya RajarshiInter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune 411 007, IndiaA. N. RamaprakashInter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune 411 007, IndiaP. ReigDepartment of Physics and Institute for Plasma Physics, University of Crete, GR-71003 Heraklion, GreeceA. C. S. ReadheadCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, MC 249-17, Pasadena, CA 91125, USAKonstantinos TassisDepartment of Physics and Institute for Plasma Physics, University of Crete, GR-71003 Heraklion, GreeceJ. A. ZensusMax-Planck-Institut fr Radioastronomie, Auf dem Hgel 69, D-53121 Bonn, Germany

2015en

ABI

Annotatsiya

We present first results on polarization swings in optical emission of blazars obtained by RoboPol, a monitoring programme of an unbiased sample of gamma-ray bright blazars specially designed for effective detection of such events. A possible connection of polarization swing events with periods of high activity in gamma-rays is investigated using the data set obtained during the first season of operation. It was found that the brightest gamma-ray flares tend to be located closer in time to rotation events, which may be an indication of two separate mechanisms responsible for the rotations. Blazars with detected rotations during non-rotating periods have significantly larger amplitude and faster variations of polarization angle than blazars without rotations. Our simulations show that the full set of observed rotations is not a likely outcome (probability 1.5 10 -2 ) of a random walk of the polarization vector simulated by a multicell model. Furthermore, it is highly unlikely (5 10 -5 ) that none of our rotations is physically connected with an increase in gamma-ray activity.

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DOI: 10.1093/mnras/stv1723

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