Multiwavelength behaviour of the blazar OJ 248 from radio to γ-rays★
M. I. CarnereroUniversidad de La Laguna, San Cristóbal de La Laguna, SpainC. M. RaiteriNational Institute for Astrophysics, Rome, ItalyM. VillataNational Institute for Astrophysics, Rome, ItalyJ. A. Acosta‐PulidoConsejo Superior de Investigaciones Científicas, Madrid, SpainF. D’AmmandoNational Institute for Astrophysics, Rome, ItalyPaul S. SmithUniversity of Arizona, Tucson, United StatesV. M. LarionovSt Petersburg University, Saint Petersburg, RussiaI. AgudoConsejo Superior de Investigaciones Científicas, Madrid, SpainM. J. ArévaloConsejo Superior de Investigaciones Científicas, Madrid, SpainA. A. Arkharov16 Southampton, SO17 1BJ, United KingdomU. BachMax Planck Society, Munich, GermanyR. BachevBulgarian Academy of Sciences, Sofia, BulgariaE. BenítezUniversidad Nacional Autónoma de México, Mexico City, MexicoD. BlinovUniversity of Crete, Rethymno, GreeceV. BozhilovSofia University "St. Kliment Ohridski", Sofia, BulgariaC. S. BuemiNational Institute for Astrophysics, Rome, ItalyA. BuenoConsejo Superior de Investigaciones Científicas, Madrid, SpainD. CarosatiNational Institute for Astrophysics, Rome, ItalyC. CasadioConsejo Superior de Investigaciones Científicas, Madrid, SpainWen-Ping ChenGraduate Inst. of Astronomy, National Central University, 300 Zhongda Road, 32001 Zhongli, TaiwanG. DamljanovićAstronomical Observatory, Volgina 7, 11060 Belgrade, SerbiaA. Di PaolaNational Institute for Astrophysics, Rome, ItalyН. В. Ефимова16 Southampton, SO17 1BJ, United KingdomSh. A. EhgamberdievMaidanak Observatory of the Ulugh Beg Astronomical Institute, 100052 UzbekistanM. GirolettiNational Institute for Astrophysics, Rome, ItalyJosé L. GómezConsejo Superior de Investigaciones Científicas, Madrid, SpainP. A. González-MoralesUniversidad de La Laguna, San Cristóbal de La Laguna, SpainAna Belén Griñón-MarínConsejo Superior de Investigaciones Científicas, Madrid, SpainT. S. GrishinaSt Petersburg University, Saint Petersburg, RussiaMark GurwellHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USAD. HiriartInstituto de Astronoma, Universidad Nacional Autnoma de Mxico, En-senada, B.C. 22800, MexicoH. Y. HsiaoGraduate Inst. of Astronomy, National Central University, 300 Zhongda Road, 32001 Zhongli, TaiwanS. IbryamovBulgarian Academy of Sciences, Sofia, BulgariaS. G. JorstadInstitute for Astrophysical Research, Boston University, 725 Common-wealth Avenue, Boston, MA 02215, USAM. JoshiInstitute for Astrophysical Research, Boston University, 725 Common-wealth Avenue, Boston, MA 02215, USAE. N. KopatskayaSt Petersburg University, Saint Petersburg, RussiaO. M. Kurtanidze16 Southampton, SO17 1BJ, United KingdomS. O. Kurtanidze16 Southampton, SO17 1BJ, United KingdomA. LähteenmäkiAalto University, Espoo, FinlandЕ. Г. ЛарионоваSt Petersburg University, Saint Petersburg, RussiaL. V. LarionovaSt Petersburg University, Saint Petersburg, RussiaC. LázaroConsejo Superior de Investigaciones Científicas, Madrid, SpainP. LetoNational Institute for Astrophysics, Rome, ItalyChien-Cheng LinGraduate Inst. of Astronomy, National Central University, 300 Zhongda Road, 32001 Zhongli, TaiwanH. C. LinGraduate Inst. of Astronomy, National Central University, 300 Zhongda Road, 32001 Zhongli, TaiwanA. Manilla-RoblesDepartment of Physics & Astronomy, University of Canterbury, Private Bag 4800, Christchurch 8140, New ZealandAlan P. MarscherInstitute for Astrophysical Research, Boston University, 725 Common-wealth Avenue, Boston, MA 02215, USAI. McHardyDepartment of Physics and Astronomy, Univ. of Southampton, Southamp-ton SO17 1BJ, UKY. MetodievaArmagh Observatory, College Hill, Armagh BT61 9DG, UKD. O. MirzaqulovMaidanak Observatory of the Ulugh Beg Astronomical Institute, 100052 UzbekistanA. A. MokrushinaSt Petersburg University, Saint Petersburg, RussiaS. N. MolinaConsejo Superior de Investigaciones Científicas, Madrid, SpainD. A. MorozovaSt Petersburg University, Saint Petersburg, RussiaM. G. NikolashviliAbastumani Observatory, Mt. Kanobili, 0301 Abastumani, GeorgiaM. OrientiNational Institute for Astrophysics, Rome, ItalyE. OvcharovSofia University "St. Kliment Ohridski", Sofia, BulgariaNeelam PanwarGraduate Inst. of Astronomy, National Central University, 300 Zhongda Road, 32001 Zhongli, TaiwanA. Pastor YabarUniversidad de La Laguna, San Cristóbal de La Laguna, SpainI. Puerto GiménezConsejo Superior de Investigaciones Científicas, Madrid, SpainVenkatessh RamakrishnanAalto University Metshovi Radio Observatory, Metshovintie 114, FI-02540 Kylml, FinlandG. M. RichterAstrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, GermanyMario Rossini16 Southampton, SO17 1BJ, United KingdomL. A. SiguaAbastumani Observatory, Mt. Kanobili, 0301 Abastumani, GeorgiaA. StrigachevBulgarian Academy of Sciences, Sofia, BulgariaBrian TaylorInstitute for Astrophysical Research, Boston University, 725 Common-wealth Avenue, Boston, MA 02215, USAM. TornikoskiAalto University Metshovi Radio Observatory, Metshovintie 114, FI-02540 Kylml, FinlandC. TrigilioNational Institute for Astrophysics, Rome, ItalyYu. V. TroitskayaSt Petersburg University, Saint Petersburg, RussiaI. S. TroitskySt Petersburg University, Saint Petersburg, RussiaG. UmanaNational Institute for Astrophysics, Rome, ItalyA. ValchevaSofia University "St. Kliment Ohridski", Sofia, BulgariaS. VelascoConsejo Superior de Investigaciones Científicas, Madrid, SpainO. VinceAstronomical Observatory, Volgina 7, 11060 Belgrade, SerbiaA. E. WehrleSpace Science Institute, Boulder, CO 80301, USAH. WiesemeyerMax Planck Society, Munich, Germany
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Аннотация
We present an analysis of the multiwavelength behaviour of the blazar OJ 248 at z = 0.939 in the period 2006-2013. We use low-energy data (optical, near-infrared, and radio) obtained by 21 observatories participating in the Gamma-Ray Large Area Space Telescope (GLAST)-AGILE Support Program of the Whole Earth Blazar Telescope, as well as data from the Swift (optical-UV and X-rays) and Fermi ( -rays) satellites, to study flux and spectral variability and correlations among emissions in different bands. We take into account the effect of absorption by the Damped Lyman intervening system at z = 0.525. Two major outbursts were observed in 2006-2007 and in 2012-2013 at optical and near-IR wavelengths, while in the high-frequency radio light curves prominent radio outbursts are visible peaking at the end of 2010 and beginning of 2013, revealing a complex radio-optical correlation. Crosscorrelation analysis suggests a delay of the optical variations after the -ray ones of about a month, which is a peculiar behaviour in blazars. We also analyse optical polarimetric and spectroscopic data. The average polarization percentage P is less than 3 per cent, but it reaches 19 per cent during the early stage of the 2012-2013 outburst. A vague correlation of P with brightness is observed. There is no preferred electric vector polarization angle and during
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