Mrk 421 active state in 2008: the MAGIC view, simultaneous multi-wavelength observations and SSC model constrained

被引:46
作者
Aleksic, J. [1 ]
Alvarez, E. A. [2 ]
Antonelli, L. A. [3 ]
Antoranz, P. [4 ,5 ]
Asensio, M. [2 ]
Backes, M. [6 ]
Barrio, J. A. [2 ]
Bastieri, D. [7 ,8 ]
Becerra Gonzalez, J. [9 ,10 ]
Bednarek, W. [11 ]
Berdyugin, A. [12 ]
Berger, K. [9 ,10 ]
Bernardini, E. [13 ]
Biland, A. [14 ]
Blanch, O. [1 ]
Bock, R. K. [15 ]
Boller, A. [14 ]
Bonnoli, G. [3 ]
Tridon, D. Borla [15 ]
Braun, I. [14 ]
Bretz, T. [16 ]
Canellas, A. [17 ]
Carmona, E. [15 ]
Carosi, A. [3 ]
Colin, P. [15 ]
Colombo, E. [9 ]
Contreras, J. L. [2 ]
Cortina, J. [1 ]
Cossio, L. [18 ,19 ]
Covino, S. [3 ]
Dazzi, F. [18 ,19 ]
De Angelis, A. [18 ,19 ]
De Caneva, G. [13 ]
De Cea del Pozo, E. [20 ]
De Lotto, B. [18 ,19 ]
Delgado Mendez, C. [9 ]
Diago Ortega, A. [9 ,10 ]
Doert, M. [6 ]
Dominguez, A. [21 ]
Prester, D. Dominis [22 ,23 ]
Dorner, D. [14 ]
Doro, M. [24 ]
Elsaesser, D. [16 ]
Ferenc, D. [22 ,23 ]
Fonseca, M. V. [2 ]
Font, L. [24 ]
Fruck, C. [15 ]
Garcia Lopez, R. J. [9 ,10 ]
Garczarczyk, M. [9 ]
Garrido, D. [24 ]
机构
[1] IFAE, Bellaterra 08193, Spain
[2] Univ Complutense, E-28040 Madrid, Spain
[3] INAF Natl Inst Astrophys, I-00136 Rome, Italy
[4] Univ Siena, I-53100 Siena, Italy
[5] INFN Pisa, I-53100 Siena, Italy
[6] Tech Univ Dortmund, D-44221 Dortmund, Germany
[7] Univ Padua, I-35131 Padua, Italy
[8] Ist Nazl Fis Nucl, I-35131 Padua, Italy
[9] Inst Astrofis Canarias, Tenerife 38200, Spain
[10] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Spain
[11] Univ Lodz, PL-90236 Lodz, Poland
[12] Univ Turku, Tuorla Observ, Piikkio 21500, Finland
[13] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany
[14] ETH, CH-8093 Zurich, Switzerland
[15] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany
[16] Univ Wurzburg, D-97074 Wurzburg, Germany
[17] Univ Barcelona ICC IEEC, Barcelona 08028, Spain
[18] Univ Udine, I-33100 Udine, Italy
[19] INFN Trieste, I-33100 Udine, Italy
[20] Inst Ciencies Espai IEEC CSIC, Bellaterra 08193, Spain
[21] Inst Astrofis Andalucia CSIC, Granada 18080, Spain
[22] Univ Rijeka, Croatian MAGIC Consortium, Rudjer Boskovic Inst, Zagreb 10000, Croatia
[23] Univ Split, Zagreb 10000, Croatia
[24] Univ Autonoma Barcelona, Bellaterra 08193, Spain
[25] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BU-1784 Sofia, Bulgaria
[26] INAF Osservatorio Astron, I-34143 Trieste, Italy
[27] Ist Nazl Fis Nucl, I-34143 Trieste, Italy
[28] Univ Insubria, I-22100 Como, Italy
[29] Univ Pisa, I-56126 Pisa, Italy
[30] Ist Nazl Fis Nucl, I-56126 Pisa, Italy
[31] ICREA, Barcelona 08010, Spain
基金
芬兰科学院;
关键词
radiation mechanisms: non-thermal; BL Lacertae objects: individual: Mrk 421; FAST TEV VARIABILITY; GAMMA-RAY EMISSION; SELF-COMPTON MODEL; BL-LAC OBJECTS; X-RAY; ELECTRON ACCELERATION; BACKGROUND-RADIATION; SPECTRAL VARIABILITY; FLARING ACTIVITY; XMM-NEWTON;
D O I
10.1051/0004-6361/201117442
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Context. The blazar Markarian 421 is one of the brightest TeV gamma-ray sources of the northern sky. From December 2007 until June 2008 it was intensively observed in the very high energy (VHE, E > 100 GeV) band by the single-dish Major Atmospheric Gamma-ray Imaging Cherenkov telescope (MAGIC-I). Aims. We aimed to measure the physical parameters of the emitting region of the blazar jet during active states. Methods. We performed a dense monitoring of the source in VHE with MAGIC-I, and also collected complementary data in soft X-rays and optical-UV bands; then, we modeled the spectral energy distributions (SED) derived from simultaneous multi-wavelength data within the synchrotron self-Compton (SSC) framework. Results. The source showed intense and prolonged.-ray activity during the whole period, with integral fluxes (E > 200 GeV) seldom below the level of the Crab Nebula, and up to 3.6 times this value. Eight datasets of simultaneous optical-UV (KVA, Swift/UVOT), soft X-ray (Swift/XRT) and MAGIC-I VHE data were obtained during different outburst phases. The data constrain the physical parameters of the jet, once the spectral energy distributions obtained are interpreted within the framework of a single-zone SSC leptonic model. Conclusions. The main outcome of the study is that within the homogeneous model high Doppler factors (40 <= delta <= 80) are needed to reproduce the observed SED; but this model cannot explain the observed short time-scale variability, while it can be argued that inhomogeneous models could allow for less extreme Doppler factors, more intense magnetic fields and shorter electron cooling times compatible with hour or sub-hour scale variability.
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页数:11
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