MAGIC observations and multifrequency properties of the flat spectrum radio quasar 3C 279 in 2011-猫眼课题宝

DOI：

10.1051/0004-6361/201323036

发表时间：

2013-11

期刊：

Astronomy and Astrophysics

影响因子：

6.5

通讯作者：

中科院分区：

物理与天体物理2区

文献类型：

作者：

J. Aleksi'c;S. Ansoldi;L. A. Antonelli;P. Antoranz;A. Babić;P. Bangale;U. D. Almeida;J. Barrio;J. Gonz'alez;W. Bednarek;K. Berger;E. Bernardini;A. Biland;O. Blanch;R. Bock;S. Bonnefoy;G. Bonnoli;F. Borracci;T. Bretz;E. Carmona;A. Carosi;D. Fidalgo;P. Colin;E. Colombo;J. Contreras;J. Cortina;S. Covino;P. D. Vela;F. Dazzi;A. Angelis;G. Caneva;B. Lotto;C. Mendez;M. Doert;A. Domínguez;D. D. Prester-D.;D. Dorner;M. Doro;S. Einecke;D. Eisenacher;D. Elsaesser;E. Farina;D. Ferenc;M. V. Fonseca;L. Font;K. Frantzen;C. Fruck;R. L'opez;M. Garczarczyk;D. G. Terrats;M. Gaug;G. Giavitto;N. Godinovi'c;A. G. Muñoz;S. Gozzini;D. Hadasch;A. Herrero;D. Hildebrand;J. Hose;D. Hrupec;W. Idec;V. Kadenius;H. Kellermann;M. Knoetig;K. Kodani;Y. Konno;J. Krause;H. Kubo;J. Kushida;A. Barbera;D. Lelas;N. Lewandowska;E. Lindfors;S. Lombardi;M. L'opez;R. L'opez-Coto;A. L'opez-Oramas;E. Lorenz;I. Lozano;M. Makariev;K. Mallot;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;B. Marcote;M. Mariotti;M. Mart'inez;D. Mazin;U. Menzel;M. Meucci;J. Miranda;R. Mirzoyan;A. Moralejo;P. Munar-Adrover;D. Nakajima;A. Niedźwiecki;K. Nilsson;K. Nishijima;N. Nowak;R. Orito;A. Overkemping;S. Paiano;M. Palatiello;D. Paneque;R. Paoletti;J. Paredes;X. Paredes-Fortuny;S. Partini;M. Persic;F. Prada;P. Moroni;E. Prandini;S. Preziuso;I. Puljak;R. Reinthal;W. Rhode;M. Rib'o;J. Rico;J. Garcia;S. Rugamer;A. Saggion;T. Saito;K. Saito;M. Salvati;K. Satalecka;V. Scalzotto;V. Scapin;C. Schultz;T. Schweizer;S. Shore;A. Sillanpaa;J. Sitarek;I. Šnidarić;D. Sobczynska;F. Spanier;V. Stamatescu;A. Stamerra;T. Steinbring;J. Storz;S. Sun;T. Suri'c;L. Takalo;H. Takami;F. Tavecchio;P. Temnikov;T. Terzi'c;D. Tescaro;M. Teshima;J. Thaele;O. Tibolla;D. Torres;T. Toyama;A. Treves;P. Vogler;R. Wagner;F. Zandanel;R. Z. A. Berdyugin;T. Vornanen;for the Kva Telescope;A. Lahteenmaki;J. Tammi;M. Tornikoski;for the Ages team Arecibo Observatory;T. Hovatta;W. Max-Moerbeck;A. Readhead;J. Richards;for the Ages team Arecibo Observatory;M. Hayashida;D. Sanchez;on behalf of the Fermi-LAT;A. Marscher;S. J. Ifae;Edifici Cn.;Campus Uab;E-08193 Bellaterra;Spain.;U. Udine;I. Trieste;I. Udine;Italy.;I. I. F. Astrophysics-I.;I. Rome;U. Siena;I. Pisa;I-53100 Siena;Croatian Magic Consortium;Rudjer Boskovic Institute;University of Rijeka;University of Split;HR-10000 Zagreb;Croatia.;M. F. Physik;D-80805 Munchen;H Germany;U. Complutense;E. Madrid;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;E-38200 La Laguna;Tenerife;University of L'od'z;PL-90236 Lodz;Poland;D. Elektronen-Synchrotron;D. Zeuthen;E. Zurich;CH-8093 Zurich;Switzerland.;U. Wurzburg;D-97074 Wurzburg;Centro de Investigaciones Energ'eticas;Medioambientales y Tecnol'ogicas;U. Padova;Infn;I-35131 Padova;Technische Universitat Dortmund;D. Dortmund;Inst. de Astrof'isica de Andaluc'ia-Inst.-de-Astrof'isica-de-Andaluc'ia-102813830;E. Granada;Universita' dell'Insubria;Como;I-22100 Como;Unitat de F'isica de les Radiacions-Unitat-de-F'isica-de-les-Radiacions-1381421020;D. D. F'isica-D.;CERES-IEEC;U. Barcelona;Institut de Ci'encies de l'Espai-Institut-de-Ci'encies-de-l'Espai-123080358;Japanese Magic Consortium;D. Physics;Astronomy;Kyoto University;Japan.;Finnish Magic Consortium;T. Observatory;U. Turku;D. Physics;U. Oulu;Finland.;Inst. for Nucl. Research;Nucl. Energy;BG-1784 Sofia;Bulgaria.;U. Barcelona;E. Barcelona;U. Pisa;I. Pisa;N. C. E. P. F. D. Lausanne;Lausanne;now at Department of PhysicsAstronomy;Uc Riverside;CA 92521;Usa;N. Eso;Turku;also at INAF-Trieste;A. M. D. D. F. Teorica-A.-M.-D.-D.-F.-Teorica-1381421114;Uamcsic;E. Madrid;now at Stockholm University;Oskar Klein Centre for Cosmoparticle Physics;S. Stockholm;Sweden.;Now at Grappa Institute;U. Amsterdam;1098XH Amsterdam;Netherlands.;A. L. M. R. Observatory;Metsahovintie 114;02540;Kylmala;Cahill Center for AstronomyAstrophysics;Caltech;1. E. C. Blvd.;Pasadena;Ca;91125;U.S.A.;Inst. for Nucl. Research;U. Tokyo;Kashiwa;Chiba;277-8582;Kipac;S. N. Laboratory;Stanford;94025;Laboratoire d'Annecy-le-Vieux de Physique des Particules-Laboratoire-d'Annecy-le-Vieux-de-Physique-des-134323232;Universit'e de Savoie;CNRSIN2p3;F-74941 Annecy-le-Vieux;France.;Inst. for Nucl. Research;Boston University

目标。我们研究类星体 3C 279 的多频发射和光谱特性，旨在识别源中发生的辐射过程。方法。 2011 年，我们使用 MAGIC 望远镜首次以立体模式观测到了极高能（VHE，E> 100 GeV）射线中的 3C 279。我们将这些测量结果与其他能带的观测结果结合起来：来自费米-LAT 的高能 (HE, E > 100 MeV) 射线；来自 RXTE 的 X 射线；来自 KVA 望远镜的光学；以及来自 VLBA、Metsahovi 和 OVRO 射电望远镜的 43 GHz、37 GHz 和 15 GHz 射电，以及来自 KVA 和 Liverpool 望远镜的光学偏振测量。我们检查了相应的光变曲线和宽带光谱能量分布，并将 MAGIC 观测时期 3C 279 的多频特性与从历史观测中推断出的特性进行了比较。结果。在MAGIC观测期间（2011年2月8日至4月11日）3C 279的光学、X射线和γ射线均处于低状态。 MAGIC 观察没有产生显着的检测结果。推导的上限与费米-LAT 的 HE 射线光谱的外推一致，并针对 EBL 吸收进行了校正。 2011 年 MAGIC 观测的第二部分是由光学和射线波段的高活动状态触发的。在光爆发期间，光电矢量位置角（EVPA）显示出~180°的旋转。与之前的情况不同，43 GHz 无线电极化角没有同时旋转。 MAGIC 未检测到 VHE 射线，得出的上限表明费米-LAT 和 MAGIC 带之间存在光谱断裂或曲率。对于 VHE 源，组合上限是迄今为止最强的，并且低于之前检测到的通量水平约 2 倍。包括同步加速器和逆康普顿发射的辐射模型与光学射线数据相匹配，假设宽线区域内的发射分量尺寸为 R = 1.1× 10 16 cm，磁场 B = 1.45 G 负责高能发射，另一个发射分量位于宽线区域和红外环面 (R = 1.5× 10 17 cm 且 B = 0.8 G) 引起光学和低能量发射。我们还研究了光学偏振

Aims. We study the multifrequency emission and spectral properties of the quasar 3C 279 aimed at identifying the radiation processes taking place in the source. Methods. We observed 3C 279 in very-high-energy (VHE, E> 100 GeV) -rays, with the MAGIC telescopes during 2011, for the first ti me in stereoscopic mode. We combined these measurements with observations at other energy bands: in high-energy (HE, E > 100 MeV) -rays from Fermi-LAT; in X-rays from RXTE; in the optical from the KVA telescope; and in the radio at 43 GHz, 37 GHz, and 15 GHz from the VLBA, Metsahovi, and OVRO radio telescopes - along with optical polarisation measurements from the KVA and Liverpool telescopes. We examined the corresponding light curves and broadband spectral energy distribution and we compared the multifrequency properties of 3C 279 at the epoch of the MAGIC observations with those inferred from historical observations. Results. During the MAGIC observations (2011 February 8 to April 11) 3C 279 was in a low state in optical, X-ray, and -rays. The MAGIC observations did not yield a significant detection. The deri ved upper limits are in agreement with the extrapolation of the HE -ray spectrum, corrected for EBL absorption, from Fermi-LAT. The second part of the MAGIC observations in 2011 was triggered by a high-activity state in the optical and -ray bands. During the optical outburst the optical electri c vector position angle (EVPA) showed a rotation of∼ 180 ◦ . Unlike previous cases, there was no simultaneous rotation of the 43 GHz radio polarisation angle. No VHE -rays were detected by MAGIC, and the derived upper limits suggest the presence of a spectral break or curvature between the Fermi-LAT and MAGIC bands. The combined upper limits are the strongest derived to date for the source at VHE and below the level of the previously detected flux by a factor of ∼ 2. Radiation models that include synchrotron and inverse Compton emissions match the optical to -ray data, assuming an emission component inside the broad line region with size R = 1.1× 10 16 cm and magnetic field B = 1.45 G responsible for the high-energy emission, and another one outside the broad line region and the infrared torus (R = 1.5× 10 17 cm and B = 0.8 G) causing the optical and low-energy emission. We also study the optical polarisation in

MAGIC observations and multifrequency properties of the flat spectrum radio quasar 3C 279 in 2011

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