Phase-resolved energy spectra of the Crab pulsar in the range of 50-400 GeV measured with the MAGIC telescopes

被引：83

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
]}

Dominis Prester, D. ^{[22
,23
]}

Dorner, D. ^{[14
]}

Doro, M. ^{[24
]}

Eisenacher, D. ^{[16
]}

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
]}

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, Depto 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, E-08028 Barcelona, Spain

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

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

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

[21] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain

[22] Univ Rijeka, Rudjer Boskovic Inst, Croatian MAG Consortium, 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] INFN Pisa, I-56126 Pisa, Italy

[31] ICREA, Barcelona 08010, Spain

[32] ASIAA Natl Tsing Hua Univ TIARA, Taipei, Taiwan

来源：

ASTRONOMY & ASTROPHYSICS | 2012年 / 540卷

基金：

芬兰科学院;

关键词：

pulsars: individual: Crab pulsar; gamma rays: stars; GAMMA-RAY EMISSION; OUTER MAGNETOSPHERE; SLOT GAPS; RADIATION; ACCELERATION; NEBULA; WIND;

D O I：

10.1051/0004-6361/201118166

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We use 73 h of stereoscopic data taken with the MAGIC telescopes to investigate the very high-energy (VHE) gamma-ray emission of the Crab pulsar. Our data show a highly significant pulsed signal in the energy range from 50 to 400 GeV in both the main pulse (P1) and the interpulse (P2) phase regions. We provide the widest spectra to date of the VHE components of both peaks, and these spectra extend to the energy range of satellite-borne observatories. The good resolution and background rejection of the stereoscopic MAGIC system allows us to cross-check the correctness of each spectral point of the pulsar by comparison with the corresponding (strong and well-known) Crab nebula flux. The spectra of both P1 and P2 are compatible with power laws with photon indices of 4.0 +/- 0.8 (P1) and 3.42 +/- 0.26 (P2), respectively, and the ratio P1/P2 between the photon counts of the two pulses is 0.54 +/- 0.12. The VHE emission can be understood as an additional component produced by the inverse Compton scattering of secondary and tertiary e(+/-) pairs on IR-UV photons.

引用

页数：6

共 15 条

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