Статья

LOCATION OF γ-RAY FLARE EMISSION IN THE JET OF THE BL LACERTAE OBJECT OJ287 MORE THAN 14 pc FROM THE CENTRAL ENGINE

I. AgudoInstitute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA; [email protected]S. G. JorstadAstronomical Institute, St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St. Petersburg, RussiaAlan P. MarscherInstitute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA; [email protected]V. M. LarionovAstronomical Institute, St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St. Petersburg, RussiaJosé L. GómezInstituto de Astrofísica de Andalucía, CSIC, Apartado 3004, 18080, Granada, SpainA. LähteenmäkiAalto University Metsähovi Radio Observatory, Metsähovintie 114, FIN-02540 Kylmälä, FinlandMark GurwellHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAPaul S. SmithSteward Observatory, University of Arizona, Tucson, AZ 85721-0065, USAH. WiesemeyerInstituto de Radio Astronomía Milimétrica, Avenida Divina Pastora, 7, Local 20, E-18012 Granada, SpainClemens ThumInstitut de Radio Astronomie Millimétrique, 300 Rue de la Piscine, 38406 St. Martin d’Hères, FranceJ. HeidtD. BlinovAstronomical Institute, St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St. Petersburg, RussiaFrancesca D’ArcangeloInstitute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA; [email protected]V. A. Hagen‐ThornAstronomical Institute, St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St. Petersburg, RussiaD. A. MorozovaAstronomical Institute, St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St. Petersburg, RussiaElina NieppolaAalto University Metsähovi Radio Observatory, Metsähovintie 114, FIN-02540 Kylmälä, FinlandMar Roca-SogorbInstituto de Astrofísica de Andalucía, CSIC, Apartado 3004, 18080, Granada, SpainGary D. SchmidtNational Science Foundation, 4201 Wilson Boulevard, Arlington, VA 22230, USABrian TaylorInstitute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA; [email protected]M. TornikoskiAalto University Metsähovi Radio Observatory, Metsähovintie 114, FIN-02540 Kylmälä, FinlandI. S. TroitskyAstronomical Institute, St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St. Petersburg, Russia

2010en

ABI

Аннотация

We combine time-dependent multi-waveband flux and linear polarization observations with sub-milliarcsecond-scale polarimetric images at lambda=7mm of the BL Lacertae-type blazar OJ287 to locate the gamma-ray emission in prominent flares in the jet of the source >14pc from the central engine. We demonstrate a highly significant correlation between the strongest gamma-ray and millimeter-wave flares through Monte-Carlo simulations. The two reported gamma-ray peaks occurred near the beginning of two major mm-wave outbursts, each of which is associated with a linear polarization maximum at millimeter wavelengths. Our Very Long Baseline Array observations indicate that the two mm-wave flares originated in the second of two features in the jet that are separated by >14 pc. The simultaneity of the peak of the higher-amplitude gamma-ray flare and the maximum in polarization of the second jet feature implies that the gamma-ray and mm-wave flares are co-spatial and occur >14 pc from the central engine. We also associate two optical flares, accompanied by sharp polarization peaks, with the two gamma-ray events. The multi-waveband behavior is most easily explained if the gamma-rays arise from synchrotron self-Compton scattering of optical photons from the flares. We propose that flares are triggered by interaction of moving plasma blobs with a standing shock. The gamma-ray and optical emission is quenched by inverse Compton losses as synchrotron photons from the newly shocked plasma cross the emission region. The mm-wave polarization is high at the onset of a flare, but decreases as the electrons emitting at these wavelengths penetrate less polarized regions.

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Идентификаторы

DOI: 10.1088/2041-8205/726/1/l13

Цитирования и источники

Цитирований: 3Использованных источников: 0

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