Observation of the black widow B1957+20 millisecond pulsar binary system with the MAGIC telescopes

被引：5

作者：

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

Ansoldi, S. ^{[2
,3
,4
,5
]}

Antonelli, L. A. ^{[6
]}

Arcaro, C. ^{[7
,8
]}

Babic, A. ^{[9
]}

Banerjee, B. ^{[10
]}

Bangale, P. ^{[11
]}

Barres de Almeida, U. ^{[11
,12
]}

Barrio, J. A. ^{[13
]}

Becerra Gonzalez, J. ^{[14
,15
,16
,17
,18
]}

Bednarek, W. ^{[19
]}

Bernardini, E. ^{[20
,21
]}

Berti, A. ^{[2
,3
,22
,23
]}

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

Biland, A. ^{[1
]}

Blanch, O. ^{[24
]}

Bonnefoy, S. ^{[13
]}

Bonnoli, G. ^{[25
,26
]}

Borracci, F. ^{[11
]}

Bretz, T. ^{[27
]}

Carosi, R. ^{[25
,26
]}

Carosi, A. ^{[6
]}

Chatterjee, A. ^{[10
]}

Colin, P. ^{[11
]}

Colombo, E. ^{[14
,15
]}

Contreras, J. L. ^{[13
]}

Cortina, J. ^{[24
]}

Covino, S. ^{[6
]}

Cumani, P. ^{[24
]}

Da Vela, P. ^{[25
,26
]}

Dazzi, F. ^{[6
]}

De Angelis, A. ^{[7
,8
]}

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

de Ona Wilhelmi, E. ^{[28
]}

Di Pierro, F. ^{[6
]}

Doert, M. ^{[29
]}

Dominguez, A. ^{[13
]}

Prester, D. Dominis ^{[9
]}

Dorner, D. ^{[27
]}

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

Einecke, S. ^{[29
]}

Glawion, D. Eisenacher ^{[27
]}

Elsaesser, D. ^{[29
]}

Engelkemeier, M. ^{[29
]}

Ramazani, V. Fallah ^{[30
,31
]}

Fernandez-Barral, A. ^{[24
]}

Fidalgo, D. ^{[13
]}

Fonseca, M. V. ^{[13
]}

Font, L. ^{[34
]}

Fruck, C. ^{[11
]}

机构：

[1] ETH, CH-8093 Zurich, Switzerland

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

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

[4] Univ Tokyo, Dept Phys, Japanese MAGIC Consortium, ICRR, Tokyo, Japan

[5] Univ Tokushima, Kyoto Univ, Tokai Univ, Hakubi Ctr, Tokushima, Japan

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

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

[8] INFN, I-35131 Padua, Italy

[9] Univ Osijek, Univ Rijeka, Univ Split FESB,Rudjer Boskovic Ins, Univ Zagreb FER,Croatian MAGIC Consortium, Osijek, Croatia

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

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

[12] Ctr Brasileiro Pesquisas Fisicas CBPF MCTI, R Dr Xavier Sigaud 150, BR-22290180 Rio De Janeiro, RJ, Brazil

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

[14] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain

[15] Univ La Laguna, Dpto Astrofis, San Cristobal la Laguna, Tenerife, Spain

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

[17] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

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

[19] Univ Lodz, Dept Astrophys, Ul Pomorska 149-153, PL-90236 Lodz, Poland

[20] Deutsches Elekt Synchrotron DESY, D-15738 Zeuthen, Germany

[21] Humboldt Univ, Inst Phys Newtonstr 15, D-12489 Berlin, Germany

[22] Univ Trieste, I-34127 Trieste, Italy

[23] INFN Trieste, I-34127 Trieste, Italy

[24] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain

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

[26] INFN Pisa, I-53100C Siena, Italy

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

[28] Inst Space Sci CSIC IEEC, E-08193 Barcelona, Spain

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

[30] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, Turku, Finland

[31] Univ Oulu, Astron Div, Finnish Ctr Astron ESO FINCA, Oulu, Finland

[32] Univ Autonoma Barcelona, Unitat Fis Radiac, Dept Fis, E-08193 Bellaterra, Spain

[33] Univ Autonoma Barcelona, CERES IEES, E-08193 Bellaterra, Spain

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

[35] Japanese MAGIC Consortium, Kyoto, Japan

[36] Inst Nucl Energy Res, Sofia, Bulgaria

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

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

[39] ICREA, E-08193 Barcelona, Spain

[40] Inst Space Sci CSIC IEEC, E-08193 Barcelona, Spain

[41] Univ Orleans, CNRS, LPC2E, Lab Phys & Chim Environm Espace, F-45071 Orleans, France

[42] CNRS, INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancy, France

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2017年 / 470卷 / 04期

关键词：

radiation mechanisms: non-thermal; binaries: close; pulsars: general; pulsars: individual: B1957+20; gamma-rays: general; HIGH-ENERGY EMISSION; GAMMA-RAY EMISSION; CRAB PULSAR; ECLIPSING BINARY; MAJOR UPGRADE; PSR 1957+20; NEBULA; ACCELERATION; WIND; DISCOVERY;

D O I：

10.1093/mnras/stx1405

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

B1957+20 is a millisecond pulsar located in a black-widow-type compact binary system with a low-mass stellar companion. The interaction of the pulsar wind with the companion star wind and/or the interstellar plasma is expected to create plausible conditions for acceleration of electrons to TeV energies and subsequent production of very high-energy gamma-rays in the inverse Compton process. We performed extensive observations with the Major Atmospheric Gamma Imaging Cherenkov Telescopes (MAGIC) telescopes of B1957+20. We interpret results in the framework of a few different models, namely emission from the vicinity of the millisecond pulsar, the interaction of the pulsar and stellar companion wind region or bow shock nebula. No significant steady very high-energy gamma-ray emission was found. We derived a 95 per cent confidence level upper limit of 3.0 x 10(-12) cm(-2) s(-1) on the average gamma-ray emission from the binary system above 200 GeV. The upper limits obtained with the MAGIC constrain, for the first time, different models of the high-energy emission in B1957+20. In particular, in the inner mixed wind nebula model with mono-energetic injection of electrons, the acceleration efficiency of electrons is constrained to be below similar to 2-10 per cent of the pulsar spin-down power. For the pulsar emission, the obtained upper limits for each emission peak are well above the exponential cut-off fits to the Fermi-LAT data, extrapolated to energies above 50 GeV. The MAGIC upper limits can rule out a simple power-law tail extension through the sub-TeV energy range for the main peak seen at radio frequencies.

引用

页码：4608 / 4617

页数：10

共 12 条

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