Rapid and multiband variability of the TeV bright active nucleus of the galaxy IC 310-猫眼课题宝

DOI：

10.1051/0004-6361/201321938

发表时间：

2013-05

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：

T. M. C. J. Aleksi'c;L. A. Antonelli;P. Antoranz;A. Babić;U. D. Almeida;J. Barrio;J. Gonz'alez;W. Bednarek;K. Berger;E. Bernardini;A. Biland;O. Blanch;R. Bock;A. Boller;S. Bonnefoy;G. Bonnoli;D. Tridon;F. Borracci;T. Bretz;E. Carmona;A. Carosi;D. Fidalgo;P. Colin;E. Colombo;J. Contreras;J. Cortina;L. Cossio;S. Covino;P. D. Vela;F. Dazzi;A. Angelis;G. Caneva;C. Mendez;B. Lotto;M. Doert;A. Domínguez;D. Prester;D. Dorner;M. Doro;D. Eisenacher;D. Elsaesser;E. Farina;D. Ferenc;M. V. Fonseca;L. Font;C. Fruck;R. L'opez;M. Garczarczyk;D. G. Terrats;M. Gaug;G. Giavitto;N. Godinovi'c;A. G. Muñoz;S. Gozzini;A. Hadamek;D. Hadasch;D. Hafner;A. Herrero;J. Hose;D. Hrupec;W. Idec;V. Kadenius;M. Knoetig;T. Krahenbuhl;J. Krause;J. Kushida;A. Barbera;D. Lelas;N. Lewandowska;E. Lindfors;S. Lombardi;R. L'opez-Coto;M. L'opez;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;J. Masbou;D. Mazin;M. Meucci;J. Miranda;R. Mirzoyan;J. Mold'on;A. Moralejo;P. Munar-Adrover;D. Nakajima;A. Niedźwiecki;K. Nilsson;N. Nowak;R. Orito;A. Overkemping;S. Paiano;M. Palatiello;D. Paneque;R. Paoletti;J. Paredes;S. Partini;M. Persic;F. Prada;P. Moroni;E. Prandini;S. Preziuso;I. Puljak;I. Reichardt;R. Reinthal;W. Rhode;M. Rib'o;J. Rico;S. Rugamer;A. Saggion;K. Saito;T. 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;S. Spiro;V. Stamatescu;A. Stamerra;B. Steinke;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;M. Uellenbeck;P. Vogler;R. Wagner;Q. Weitzel;F. Zandanel;R. Zanin;T. Dauser;P. Fortin;M. Kadler;F. Krauß;S. Wilbert;J. W. Ifae;Edifici Cn.;Campus Uab;Bellaterra;Spain.;I. I. F. Astrophysics-I.;Italy.;U. Siena;I. Pisa;Croatian Magic Consortium;Rudjer Boskovic Institute;University of Rijeka;University of Split;Croatia.;M. F. Physik;Munchen;H Germany;U. Complutense;Madrid;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;La Laguna;Tenerife;University of L'od'z;Poland;D. Astrof'isica;U. L. Laguna;D. Elektronen-Synchrotron;Zeuthen;E. Zurich;Switzerland.;U. Wurzburg;Centro de Investigaciones Energ'eticas;Medioambientales y Tecnol'ogicas;U. Udine;I. Trieste;Technische Universitat Dortmund;Inst. de Astrof'isica de Andaluc'ia-Inst.-de-Astrof'isica-de-Andaluc'ia-102813830;Granada;U. Padova;Infn;Unitat de F'isica de les Radiacions-Unitat-de-F'isica-de-les-Radiacions-1381421020;D. D. F'isica-D.;CERES-IEEC;U. Barcelona;Universita' dell'Insubria;Como;Institut de Ci'encies de l'Espai-Institut-de-Ci'encies-de-l'Espai-123080358;T. Observatory;U. Turku;Piikkio;Finland.;Japanese Magic Consortium;D. Physics;Astronomy;Kyoto University;Japan.;Inst. for Nucl. Research;Nucl. Energy;Sofía;Bulgaria.;U. Barcelona;Barcelona;INAF-Osservatorio Astronomico;Trieste;U. Pisa;I. Pisa;Icrea;N. C. E. P. F. D. Lausanne;Lausanne;supported by Infn Padova;now at Department of PhysicsAstronomy;Uc Riverside;Usa;N. Eso;A. M. D. D. F. Teorica-A.-M.-D.-D.-F.-Teorica-1381421114;Uamcsic;Now at Grappa Institute;U. Amsterdam;Netherlands.;Dr-Karl-Remeis-Observatory;Erlangen Centre for Astroparticle Physics;Bamberg;Fred Lawrence Whipple Observatory;H. C. F. Astrophysics;Amado;Az

上下文。射电星系IC310最近被确认为γ射线发射体，这是基于用费米-LAT和魔术望远镜在GeV能量和非常高的能量(Vhe，E&GT；100GeV)下的观测得出的结论。最初被归类为头部-尾部射电星系，这个天体的性质是有争议的，因为它的核心表现出类似blazar的行为。目标。为了了解IC310的性质和VHE发射的来源，我们研究了IC310从X射线波段到VHEγ光区的光谱和通量变化。方法：研究方法。用魔术望远镜从2009年10月到2010年2月测量了IC310在300GeV以上的光曲线。还分析了10-500GeV能量范围内的同期费米-LAT数据(2008-2011年)。在X射线系统中，研究了2003年至2007年用XMM-牛顿、钱德拉和SWIFT-XRT在0.5-10keV波段进行的档案观测。结果。VHE光曲线显示了几个高幅度和持续时间较短的耀斑。每天的通量变异性明显存在(&gt；5σ)。在低通量和高通量状态下，120GeV到8TeV之间的光子指数都保持在∼2.0。VHE谱的形状没有明显的变化，而在1TeV处的通量变化了S的∼7倍。在三年的观测中，费米-LAT只探测到了10GeV-500GeV能量范围内的8个γ射线事件。在费米-拉特范围内测得的光子指数=1.3±0.5是非常困难的。X射线测量表明，通量和光子指数都有很强的可变性。后者在1.76±0.07~2.55±0.07之间变化。结论。在γ-射线和X射线中测量到的快速变化证实了IC310类似blazar的行为。多TeVγ射线的发射似乎来自于其取向角为10◦−38◦的FR I射电喷流致密核心内小于80个Schwarzschild半径的尺度(黑洞质量为2×108M)。光谱能量分布类似于extreme blazar，尽管光度大于2。

Context. The radio galaxy IC 310 has recently been identified as a γ-ray emitter based on observations at GeV energies with Fermi-LAT and at very high energies (VHE, E>100 GeV) with the MAGIC telescopes. Originally classified as a head-tail radio galaxy, the nature of this object is subject of controversy since its nucleus shows blazar-like behavior. Aims. In order to understand the nature of IC 310 and the origin of the VHE emission we studied the spectral and flux variability of IC 310 from the X-ray band to the VHEγ-ray regime. Methods. The light curve of IC 310 above 300 GeV has been measured with the MAGIC telescopes from October 2009 to February 2010. Contemporaneous Fermi-LAT data (2008‐2011) in the 10‐500 GeV energy range were also analyzed. In the X-ray regime, archival observations from 2003 to 2007 with XMM-Newton, Chandra, and Swift-XRT in the 0.5‐10 keV band were studied. Results. The VHE light curve reveals several high-amplitude and short-duration flares. Day-to-day flux variability is clearly pr esent (> 5σ). The photon index between 120 GeV and 8 TeV remains at the value ∼ 2.0 during both low and high flux states. The VHE spectral shape d oes not show significant variability, whereas the flux at 1 TeV change s by a factor of∼ 7. Fermi-LAT detected only eightγ-ray events in the energy range 10 GeV‐500 GeV in three years of observation. The measured photon index of = 1.3± 0.5 in the Fermi-LAT range is very hard. The X-ray measurements show strong variability in both flux and photon index. The latter varied from 1.76± 0.07 to 2.55± 0.07. Conclusions. The rapid variability measured inγ-rays and X-rays confirms the blazar-like behavior of IC 310. The multi-TeVγ-ray emission seems to originate from scales of less than 80 Schwarzschild radii (for a black hole mass of 2× 10 8 M⊙) within the compact core of its FR I radio jet with orientation angle 10 ◦ − 38 ◦ . The spectral energy distribution resembles that of an extr eme blazar, albeit the luminosity is more than two

Rapid and multiband variability of the TeV bright active nucleus of the galaxy IC 310

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