MAGIC observations of the February 2014 flare of 1ES 1011+496 and ensuing constraint of the EBL density

被引：46

作者：

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

Ansoldi, S. ^{[2
,3
]}

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

Antoranz, P. ^{[5
,6
]}

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

Banerjee, B. ^{[10
]}

Bangale, P. ^{[11
]}

de Almeida, U. Barres ^{[11
,38
]}

Barrio, J. A. ^{[12
]}

Becerra Gonzalez, J. ^{[13
,14
,39
,40
]}

Bednarek, W. ^{[15
]}

Bernardini, E. ^{[16
,41
]}

Biasuzzi, B. ^{[2
,3
]}

Biland, A. ^{[1
]}

Blanch, O. ^{[17
]}

Bonnefoy, S. ^{[12
]}

Bonnoli, G. ^{[4
]}

Borracci, F. ^{[11
]}

Bretz, T. ^{[18
,42
]}

Carmona, E. ^{[19
]}

Carosi, A. ^{[4
]}

Chatterjee, A. ^{[10
]}

Clavero, R. ^{[13
,14
]}

Colin, P. ^{[11
]}

Colombo, E. ^{[13
,14
]}

Contreras, J. L. ^{[12
]}

Cortina, J. ^{[17
]}

Covino, S. ^{[4
]}

Da Vela, P. ^{[5
,6
]}

Dazzi, F. ^{[11
]}

De Angelis, A. ^{[20
,21
]}

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

de Ona Wilhelmi, E. ^{[22
]}

Delgado Mendez, C. ^{[19
]}

Di Pierro, F. ^{[4
]}

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

Dorner, D. ^{[18
]}

Doro, M. ^{[11
,43
]}

Einecke, S. ^{[23
]}

Glawion, D. Eisenacher ^{[18
]}

Elsaesser, D. ^{[18
]}

Fernandez-Barral, A. ^{[17
]}

Fidalgo, D. ^{[12
]}

Fonseca, M. V. ^{[12
]}

Font, L. ^{[24
,25
]}

Frantzen, K. ^{[23
]}

Fruck, C. ^{[11
]}

Galindo, D. ^{[26
]}

Garcia Lopez, R. J. ^{[13
,14
]}

Garczarczyk, M. ^{[16
]}

机构：

[1] ETH, CH-8093 Zurich, Switzerland

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

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

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

[5] Univ Siena, Via Laterina 8, I-53100 Siena, Italy

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

[7] Univ Rijeka, Rudjer Boskovic Inst, Croatian MAGIC Consortium, Zagreb, Croatia

[8] Univ Split, Zagreb, Croatia

[9] Univ Zagreb, Zagreb 41000, Croatia

[10] Saha Inst Nucl Phys, 1-AF Bidhannagar,Salt Lake,Sector 1, Kolkata 700064, India

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

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

[13] Inst Astrofis Canarias, Tenerife 38200, Spain

[14] Univ La Laguna, Dpt Astrofis, E-38206 Tenerife, Spain

[15] Univ Lodz, PL-90236 Lodz, Poland

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

[17] IFAE, Campus UAB, Bellaterra 08193, Spain

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

[19] Ctr Invest Energet Medioambient & Tecnol, Madrid 28040, Spain

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

[21] Ist Nazl Fis Nucl, I-35131 Padua, Italy

[22] CSIC IEEC, Inst Space Sci, Barcelona 08193, Spain

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

[24] Univ Autonoma Barcelona, Unitat Fis Radiac, Dept Fis, Bellaterra 08193, Spain

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

[26] Univ Barcelona, ICC, IEEC UB, E-08028 Barcelona, Spain

[27] Univ Tokyo, Tokyo 1138654, Japan

[28] Tokai Univ, Kyoto Univ, Univ Tokushima, Hakubi Ctr,KEK, Hiratsuka, Kanagawa 25912, Japan

[29] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, SF-20500 Turku, Finland

[30] Univ Oulu, Dept Phys, Oulu 90014, Finland

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

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

[33] INFN, I-56126 Pisa, Italy

[34] ICREA, Barcelona 08193, Spain

[35] Inst Space Sci CSIC IEEC, Barcelona 08193, Spain

[36] Univ Insubria, I-22100 Como, Italy

[37] INFN Milano Bicocca, I-22100 Como, Italy

[38] Ctr Brasileiro Pesquisas Fis CBPF MCTI, 150 Urca, BR-22290180 Rio De Janeiro, RJ, Brazil

[39] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[40] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[41] Humboldt Univ, Ist Phys Newtonstr 15, D-12489 Berlin, Germany

[42] Ecole Polytech Fed Lausanne, CH-1015 Lausanne, Switzerland

[43] Ist Nazl Fis Nucl, I-35131 Padua, Italy

[44] CEA, DSM IRFU, Lab AIM, Serv Astrophys, F-91191 Gif Sur Yvette, France

[45] Finnish Ctr Astron ESO FINCA, Turku 20014, Finland

[46] INAF, Trieste, Italy

[47] ISDC Sci Data Ctr Astrophys, Versoix 1290, Geneva, Switzerland

[48] Univ Nacl Autonoma Mexico, Inst Fis, Apartado Postal 20364, Mexico City 01000, DF, Mexico

来源：

ASTRONOMY & ASTROPHYSICS | 2016年 / 590卷

基金：

芬兰科学院;

关键词：

BL Lacertae objects: general; intergalactic medium; cosmic background radiation; EXTRAGALACTIC BACKGROUND LIGHT; TELESCOPE IMAGING SPECTROGRAPH; SPITZER-SPACE-TELESCOPE; MICRON SOURCE COUNTS; ENERGY GAMMA-RAYS; DIRBE MINUS 2MASS; 3.5; MU-M; NUMBER COUNTS; GALAXY COUNTS; TEV BLAZARS;

D O I：

10.1051/0004-6361/201527256

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. During February-March 2014, the MAGIC telescopes observed the high-frequency peaked BL Lac 1ES 1011 + 496 (z = 0.212) in flaring state at very-high energy (VHE, E > 100 GeV). The flux reached a level of more than ten times higher than any previously recorded flaring state of the source. Aims. To describe the characteristics of the flare presenting the light curve and the spectral parameters of the night-wise spectra and the average spectrum of the whole period. From these data we aim to detect the imprint of the extragalactic background light (EBL) in the VHE spectrum of the source, to constrain its intensity in the optical band. Methods. We analyzed the gamma-ray data from the MAGIC telescopes using the standard MAGIC software for the production of the light curve and the spectra. To constrain the EBL, we implement the method developed by the H.E.S.S. collaboration, in which the intrinsic energy spectrum of the source is modeled with a simple function (<= 4 parameters), and the EBL-induced optical depth is calculated using a template EBL model. The likelihood of the observed spectrum is then maximized, including a normalization factor for the EBL opacity among the free parameters. Results. The collected data allowed us to describe the night-wise flux changes and also to produce differential energy spectra for all nights in the observed period. The estimated intrinsic spectra of all the nights could be fitted by power-law functions. Evaluating the changes in the fit parameters, we conclude that the spectral shape for most of the nights were compatible, regardless of the flux level, which enabled us to produce an average spectrum from which the EBL imprint could be constrained. The likelihood ratio test shows that the model with an EBL density 1.07 (-0.20, + 0.24)(stat+sys), relative to the one in the tested EBL template, is preferred at the 4.6 sigma level to the no-EBL hypothesis, with the assumption that the intrinsic source spectrum can be modeled as a log-parabola. This would translate into a constraint of the EBL density in the wavelength range [0.24 mu m, 4.25 mu m], with a peak value at 1.4 mu m of lambda F-lambda = 12. 27(-2.29)(+2.75) nWm(-2) sr(-1), including systematics.

引用

页数：8

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