Extreme HBL behavior of Markarian 501 during 2012

被引：47

作者：

Ahnen, M. L. ^{[1
]}

Ansoldi, S. ^{[2
,3
,29
,30
,31
,32
]}

Antonelli, L. A. ^{[4
]}

Arcaro, C. ^{[5
,6
]}

Babic, A. ^{[7
,8
,9
,10
,11
]}

Banerjee, B. ^{[12
]}

Bangale, P. ^{[13
]}

Barres de Almeida, U. ^{[13
,36
]}

Barrio, J. A. ^{[14
]}

Gonzalez, J. Becerra ^{[15
]}

Bednarek, W. ^{[16
]}

Bernardini, E. ^{[17
,37
]}

Berti, A. ^{[2
,3
,38
]}

Bhattacharyya, W. ^{[17
]}

Blanch, O. ^{[18
]}

Bonnoli, G. ^{[19
,20
]}

Carosi, R. ^{[19
,20
]}

Carosi, A. ^{[4
]}

Chatterjee, A. ^{[12
]}

Colak, S. M. ^{[18
]}

Colin, P. ^{[13
]}

Colombo, E. ^{[15
]}

Contreras, J. L. ^{[14
]}

Cortina, J. ^{[18
]}

Covino, S. ^{[4
]}

Cumani, P. ^{[18
]}

Da Vela, P. ^{[19
,20
]}

Dazzi, F. ^{[4
]}

De Angelis, A. ^{[5
,6
]}

De Lotto, B. ^{[2
,3
]}

Delfino, M. ^{[18
,39
]}

Delgado, J. ^{[18
]}

Di Pierro, F. ^{[5
,6
]}

Doert, M. ^{[21
]}

Dominguez, A. ^{[14
]}

Prester, D. Dominis ^{[7
,8
,9
,10
,11
]}

Doro, M. ^{[5
,6
]}

Glawion, D. Eisenacher ^{[22
]}

Engelkemeier, M. ^{[21
]}

Ramazani, V. Fallah ^{[23
,24
,25
]}

Fernandez-Barral, A. ^{[18
]}

Fidalgo, D. ^{[14
]}

Fonseca, M. V. ^{[14
]}

Font, L. ^{[26
,27
]}

Fruck, C. ^{[13
]}

Galindo, D. ^{[28
]}

Lopez, R. J. Garcia ^{[15
]}

Garczarczyk, M. ^{[17
]}

Gaug, M. ^{[26
,27
]}

Giammaria, P. ^{[4
]}

机构：

[1] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland

[2] Univ Udine, I-33100 Udine, Italy

[3] INFN Trieste, I-33100 Udine, Italy

[4] Natl Inst Astrophys INAF, I-00136 Rome, Italy

[5] Univ Padua, I-35131 Padua, Italy

[6] INFN, I-35131 Padua, Italy

[7] Univ Rijeka, Croatian MAGIC Consortium, Rijeka 51000, Croatia

[8] Univ Split, FESB, Split 21000, Croatia

[9] Univ Zagreb, FER, Zagreb 10000, Croatia

[10] Univ Osijek, Osijek 31000, Croatia

[11] Rudjer Boskovic Inst, Zagreb 10000, Croatia

[12] HBNI, Saha Inst Nucl Phys, 1 AF Bidhannagar,Sect 1, Kolkata 700064, India

[13] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany

[14] Univ Complutense, E-28040 Madrid, Spain

[15] Univ La Laguna, Inst Astrofis Canarias, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain

[16] Univ Lodz, Dept Astrophys, PL-90236 Lodz, Poland

[17] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany

[18] BIST, IFAE, Bellaterra 08193, Spain

[19] Univ Siena, I-53100 Siena, Italy

[20] INFN Pisa, I-53100 Siena, Italy

[21] Tech Univ Dortmund, D-44221 Dortmund, Germany

[22] Univ Wurzburg, D-97074 Wurzburg, Germany

[23] Univ Turku, Finnish MAGIC Consortium, Tuorla Observ, Vaisalantie 20, FI-21500 Piikkio, Finland

[24] Univ Turku, Finnish Ctr Astron ESO FINCA, Vaisalantie 20, FI-21500 Piikkio, Finland

[25] Univ Oulu, Astron Div, Oulu 90014, Finland

[26] Univ Autonoma Barcelona, Dept Fis, Bellaterra 08193, Spain

[27] Univ Autonoma Barcelona, CERES, IEEC, Bellaterra 08193, Spain

[28] Univ Barcelona, ICC, IEEC, E-08028 Barcelona, Spain

[29] Univ Tokyo, ICRR, Japanese MAGIC Consortium, Chiba 2778582, Japan

[30] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan

[31] Tokai Univ, Hiratsuka, Kanagawa 2591292, Japan

[32] Univ Tokushima, Tokushima 7708502, Japan

[33] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BU-1784 Sofia, Bulgaria

[34] Univ Pisa, I-56126 Pisa, Italy

[35] INFN Pisa, I-56126 Pisa, Italy

[36] URCA, CBPF, BR-22290180 Rio De Janeiro, Brazil

[37] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany

[38] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy

[39] PIC, Bellaterra 08193, Spain

[40] INAF Trieste, Trieste, Italy

[41] Univ Bologna, Dept Phys & Astron, Bologna, Italy

[42] Univ Geneva, ISDC Data Ctr Astrophys, Chemin Ecogia 16, CH-1290 Versoix, Switzerland

[43] Rhein Westfal TH Aachen, Phys Inst A 3, Aachen, Germany

[44] Washington Univ, Dept Phys, St Louis, MO 63130 USA

[45] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA

[46] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA

[47] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany

[48] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA

[49] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA

[50] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 620卷

基金：

美国国家航空航天局; 英国科学技术设施理事会; 俄罗斯科学基金会; 美国国家科学基金会; 加拿大自然科学与工程研究理事会;

关键词：

astroparticle physics; acceleration of particles; radiation mechanisms: non-thermal; BL Lacertae objects: general; BL Lacertae objects: individual: Mrk501; EXTRAGALACTIC BACKGROUND LIGHT; ACTIVE GALACTIC NUCLEI; GAMMA-RAY EMISSION; BL-LAC OBJECTS; X-RAY; MULTIWAVELENGTH OBSERVATIONS; TEV BLAZARS; 3C; 454.3; ENERGY; VARIABILITY;

D O I：

10.1051/0004-6361/201833704

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. We aim to characterize the multiwavelength emission from Markarian 501 (Mrk 501), quantify the energy-dependent variability, study the potential multiband correlations, and describe the temporal evolution of the broadband emission within leptonic theoretical scenarios. Methods. We organized a multiwavelength campaign to take place between March and July of 2012. Excellent temporal coverage was obtained with more than 25 instruments, including the MAGIC, FACT and VERITAS Cherenkov telescopes, the instruments on board the Swift and Fermi spacecraft, and the telescopes operated by the GASP-WEBT collaboration. Results. Mrk 501 showed a very high energy (VHE) gamma-ray flux above 0.2 TeV of similar to 0.5 times the Crab Nebula flux (CU) for most of the campaign. The highest activity occurred on 2012 June 9, when the VHE flux was similar to 3 CU, and the peak of the high-energy spectral component was found to be at similar to 2 TeV. Both the X-ray and VHE gamma-ray spectral slopes were measured to be extremely hard, with spectral indices <2 during most of the observing campaign, regardless of the X-ray and VHE flux. This study reports the hardest Mrk 501 VHE spectra measured to date. The fractional variability was found to increase with energy, with the highest variability occurring at VHE. Using the complete data set, we found correlation between the X-ray and VHE bands; however, if the June 9 flare is excluded, the correlation disappears (significance <3 sigma) despite the existence of substantial variability in the X-ray and VHE bands throughout the campaign. Conclusions. The unprecedentedly hard X-ray and VHE spectra measured imply that their low- and high-energy components peaked above 5 keV and 0.5 TeV, respectively, during a large fraction of the observing campaign, and hence that Mrk 501 behaved like an extreme high-frequency-peaked blazar (EHBL) throughout the 2012 observing season. This suggests that being an EHBL may not be a permanent characteristic of a blazar, but rather a state which may change over time. The data set acquired shows that the broadband spectral energy distribution (SED) of Mrk 501, and its transient evolution, is very complex, requiring, within the framework of synchrotron self-Compton (SSC) models, various emission regions for a satisfactory description. Nevertheless the one-zone SSC scenario can successfully describe the segments of the SED where most energy is emitted, with a significant correlation between the electron energy density and the VHE gamma-ray activity, suggesting that most of the variability may be explained by the injection of high-energy electrons. The one-zone SSC scenario used reproduces the behavior seen between the measured X-ray and VHE gamma-ray fluxes, and predicts that the correlation becomes stronger with increasing energy of the X-rays.

引用

页数：23

共 118 条

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← 1 2 3 4 5 6 7 8 9 10 →

共 118 条

[1] INSIGHTS INTO THE HIGH-ENERGY γ-RAY EMISSION OF MARKARIAN 501 FROM EXTENSIVE MULTIFREQUENCY OBSERVATIONS IN THE FERMI ERA [J].

Abdo, A. A. ;

Ackermann, M. ;

Ajello, M. ;

Allafort, A. ;

Baldini, L. ;

Ballet, J. ;

Barbiellini, G. ;

Baring, M. G. ;

Bastieri, D. ;

Bechtol, K. ;

Bellazzini, R. ;

Berenji, B. ;

Blandford, R. D. ;

Bloom, E. D. ;

Bonamente, E. ;

Borgland, A. W. ;

Bouvier, A. ;

Brandt, T. J. ;

Bregeon, J. ;

Brez, A. ;

Brigida, M. ;

Bruel, P. ;

Buehler, R. ;

Buson, S. ;

Caliandro, G. A. ;

Cameron, R. A. ;

Cannon, A. ;

Caraveo, P. A. ;

Carrigan, S. ;

Casandjian, J. M. ;

Cavazzuti, E. ;

Cecchi, C. ;

Celik, O. . ;

Charles, E. ;

Chekhtman, A. ;

Cheung, C. C. ;

Chiang, J. ;

Ciprini, S. ;

Claus, R. ;

Cohen-Tanugi, J. ;

Conrad, J. ;

Cutini, S. ;

Dermer, C. D. ;

de Palma, F. ;

do Couto e Silva, E. ;

Drell, P. S. ;

Dubois, R. ;

Dumora, D. ;

Favuzzi, C. ;

Fegan, S. J. .

ASTROPHYSICAL JOURNAL, 2011, 727 (02)

[2] TeV AND MULTI-WAVELENGTH OBSERVATIONS OF Mrk 421 IN 2006-2008 [J].

Acciari, V. A. ;

Aliu, E. ;

Arlen, T. ;

Aune, T. ;

Beilicke, M. ;

Benbow, W. ;

Boltuch, D. ;

Bradbury, S. M. ;

Buckley, J. H. ;

Bugaev, V. ;

Byrum, K. ;

Cannon, A. ;

Cesarini, A. ;

Ciupik, L. ;

Cui, W. ;

Dickherber, R. ;

Duke, C. ;

Falcone, A. ;

Finley, J. P. ;

Finnegan, G. ;

Fortson, L. ;

Furniss, A. ;

Galante, N. ;

Gall, D. ;

Gillanders, G. H. ;

Godambe, S. ;

Grube, J. ;

Guenette, R. ;

Gyuk, G. ;

Hanna, D. ;

Holder, J. ;

Hui, C. M. ;

Humensky, T. B. ;

Imran, A. ;

Kaaret, P. ;

Karlsson, N. ;

Kertzman, M. ;

Kieda, D. ;

Konopelko, A. ;

Krawczynski, H. ;

Krennrich, F. ;

Lang, M. J. ;

Maier, G. ;

McArthur, S. ;

McCutcheon, M. ;

Moriarty, P. ;

Ong, R. A. ;

Otte, A. N. ;

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