MAGIC upper limits to the VHE gamma-ray flux of 3C 454.3 in high emission state

被引：16

作者：

Anderhub, H. ^{[1
]}

Antonelli, L. A. ^{[2
]}

Antoranz, P. ^{[3
]}

Backes, M. ^{[4
]}

Baixeras, C. ^{[5
]}

Balestra, S. ^{[3
]}

Barrio, J. A. ^{[3
]}

Bartko, H. ^{[6
]}

Bastieri, D. ^{[7
,8
]}

Gonzalez, J. Becerra ^{[9
]}

Becker, J. K. ^{[4
]}

Bednarek, W. ^{[10
]}

Berger, K. ^{[10
]}

Bernardini, E. ^{[11
]}

Biland, A. ^{[1
,3
,12
]}

Bock, R. K. ^{[6
,7
,8
]}

Bonnoli, G. ^{[12
,13
]}

Bordas, P. ^{[14
]}

Tridon, D. Borla ^{[6
]}

Bosch-Ramon, V. ^{[14
]}

Bretz, T. ^{[15
]}

Britvitch, I. ^{[1
]}

Camara, M. ^{[3
]}

Carmona, E. ^{[6
]}

Commichau, S. ^{[1
]}

Contreras, J. L. ^{[3
]}

Cortina, J. ^{[32
]}

Costado, M. T. ^{[9
,33
]}

Covino, S. ^{[2
]}

Curtef, V. ^{[4
]}

Dazzi, F. ^{[7
,8
]}

De Angelis, A. ^{[16
,17
]}

del Pozo, E. De Cea ^{[18
]}

de los Reyes, R. ^{[3
]}

De Lotto, B. ^{[16
,17
]}

De Maria, M. ^{[16
,17
]}

De Sabata, F. ^{[16
,17
]}

Mendez, C. Delgado ^{[9
]}

Dominguez, A. ^{[19
]}

Dorner, D. ^{[1
]}

Doro, M. ^{[7
,8
]}

Elsaesser, D. ^{[15
]}

Errando, M. ^{[32
]}

Ferenc, D. ^{[20
]}

Fernandez, E. ^{[32
]}

Firpo, R. ^{[32
]}

Fonseca, M. V. ^{[3
]}

Font, L. ^{[5
]}

Galante, N. ^{[6
]}

Lopez, R. J. Garcia ^{[9
,33
]}

机构：

[1] ETH, CH-8093 Zurich, Switzerland

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

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

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

[5] Univ Autonoma Barcelona, Bellaterra 08193, Spain

[6] Max Planck Inst Phys & Astrophys, D-80805 Munich, 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 Lodz, PL-90236 Lodz, Poland

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

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

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

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

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

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

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

[18] CSIC, IEEC, Inst Ciencies Espai, Bellaterra 08193, Spain

[19] Inst Astrofis Andalucia, E-18080 Granada, Spain

[20] Univ Calif Davis, Davis, CA 95616 USA

[21] Turku Univ, Tuorla Observ, Piikkio 21500, Finland

[22] Inst Nucl Energy Res, Sofia 1784, Bulgaria

[23] Humboldt Univ, D-12489 Berlin, Germany

[24] INFN, I-34143 Trieste, Italy

[25] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy

[26] ICREA, E-08010 Barcelona, Spain

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

[28] Ist Nazl Fis Nucl, I-56126 Pisa, Italy

[29] INAF IASF Milano, I-20133 Milan, Italy

[30] INAF IASF Roma, I-00133 Rome, Italy

[31] Univ Roma Tor Vergata, Dip Fis, I-00133 Rome, Italy

[32] IFAE, Bellaterra, Spain

[33] Univ Tenerife, Depto Astrofis, Tenerife, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2009年 / 498卷 / 01期

关键词：

galaxies: quasars: individual 3C 454.3; gamma rays: observations; gamma rays: theory; EXTRAGALACTIC BACKGROUND LIGHT; HIGH-ENERGY EMISSION; BROAD-LINE REGION; BL-LACERTAE; ABSORPTION; RADIATION; SPECTRA; JET; BLAZARS; FLARE;

D O I：

10.1051/0004-6361/200811326

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. We report upper limits to the very high energy flux (E > 100 GeV) of the flat spectrum radio quasar 3C454.3 (z = 0.859) derived by the Cherenkov telescope MAGIC during the high states of July/August and November/December 2007. We compare the upper limits derived in both time slots with the available quasi-simultaneous MeV-GeV data from the AGILE gamma-ray satellite and interpret the observational results in the context of leptonic emission models. Methods. The source was observed with the MAGIC telescope during the active phases of July-August 2007 and November-December 2007 and the data were analyzed with the MAGIC standard analysis tools. For the periods around the ends of July and November, characterized by the most complete multifrequency coverage, we constructed the spectral energy distributions using our data together with nearly simultaneous multifrequency (optical, UV, X-ray and GeV) data. Results. Only upper limits can be derived from the MAGIC data. The upper limits, once corrected for the expected absorption by the extragalactic background light, together with nearly simultaneous multifrequency data, allow us to constrain the spectral energy distribution of 3C 454.3. The data are consistent with the model expectations based on inverse Compton scattering of the ambient photons from the broad line region by relativistic electrons, which robustly predicts a sharp cut-off above 20-30 GeV.

引用

页码：83 / 87

页数：5

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