Discovery of TeV γ-ray emission from the pulsar wind nebula 3C 58 by MAGIC

被引：27

作者：

Aleksic, J. ^{[1
]}

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

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

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

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

Bangale, P. ^{[9
]}

Barrio, J. A. ^{[10
]}

Becerra Gonzalez, J. ^{[11
,34
,35
]}

Bednarek, W. ^{[12
]}

Bernardini, E. ^{[13
]}

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

Biland, A. ^{[14
]}

Blanch, O. ^{[1
]}

Bonnefoy, S. ^{[10
]}

Bonnoli, G. ^{[4
]}

Borracci, F. ^{[9
]}

Bretz, T. ^{[15
]}

Carmona, E. ^{[16
]}

Carosi, A. ^{[4
]}

Colin, P. ^{[9
]}

Colombo, E. ^{[11
]}

Contreras, J. L. ^{[10
]}

Cortina, J. ^{[1
]}

Covino, S. ^{[4
]}

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

Dazzi, F. ^{[9
]}

De Angelis, A. ^{[2
,3
]}

De Caneva, G. ^{[13
]}

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

de Ona Wilhelmi, E. ^{[17
]}

Delgado Mendez, C. ^{[16
]}

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

Dorner, D. ^{[15
]}

Doro, M. ^{[18
,19
]}

Einecke, S. ^{[20
]}

Eisenacher, D. ^{[15
]}

Elsaesser, D. ^{[15
]}

Fonseca, M. V. ^{[10
]}

Font, L. ^{[21
,22
]}

Frantzen, K. ^{[20
]}

Fruck, C. ^{[9
]}

Galindo, D. ^{[23
]}

Garcia Lopez, R. J. ^{[11
]}

Garczarczyk, M. ^{[13
]}

Garrido Terrats, D. ^{[21
,22
]}

Gaug, M. ^{[21
,22
]}

Godinovic, N. ^{[7
,8
]}

Gonzalez Munoz, A. ^{[1
]}

Gozzini, S. R. ^{[13
]}

Hadasch, D. ^{[17
]}

机构：

[1] IFAE, Bellaterra 08193, Spain

[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, I-53100 Siena, Italy

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

[7] Univ Rijeka, Rudjer Boskovic Inst, Croatian MAGIC Consortium, Zagreb 10000, Croatia

[8] Univ Split, Zagreb 10000, Croatia

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

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

[11] Inst Astrofis Canarias, Tenerife 38200, Spain

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

[13] DESY, D-15738 Zeuthen, Germany

[14] ETH, CH-8093 Zurich, Switzerland

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

[16] Ctr Invest Energet Medioambientales & Tecnol, Madrid 28040, Spain

[17] Inst Space Sci, Barcelona 08193, Spain

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

[19] INFN, I-35131 Padua, Italy

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

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

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

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

[24] Kyoto Univ, Div Phys & Astron, Japanese MAGIC Consortium, Kyoto 6068501, Japan

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

[26] Univ Oulu, Dept Phys, SF-90100 Oulu, Finland

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

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

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

[30] ICREA, Barcelona 08193, Spain

[31] Inst Space Sci, Barcelona 08193, Spain

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

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

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

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

[36] INAF Trieste, Trieste, Italy

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

[38] Univ Zaragoza, Fac Ciencias, Dept Fis Teor, E-50009 Zaragoza, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 567卷

基金：

芬兰科学院;

关键词：

gamma rays: general; pulsars: general; ISM: supernova remnants; LARGE-AREA TELESCOPE; SUPERNOVA-REMNANTS; SPECTRAL EVOLUTION; CONSTRAINTS; EXPANSION; DISTANCE; CATALOG; MODEL; 3C-58;

D O I：

10.1051/0004-6361/201424261

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The pulsar wind nebula (PWN) 3C 58 is one of the historical very high-energy (VHE; E > 100 GeV) gamma-ray source candidates. It is energized by one of the highest spin-down power pulsars known (5% of Crab pulsar) and it has been compared with the Crab nebula because of their morphological similarities. This object was previously observed by imaging atmospheric Cherenkov telescopes (Whipple, VERITAS and MAGIC), although it was not detected, with an upper limit of 2.3% Crab unit (C. U.) at VHE. It was detected by the Fermi Large Area Telescope (LAT) with a spectrum extending beyond 100 GeV. Aims. We aim to extend the spectrum of 3C 58 beyond the energies reported by the Fermi Collaboration and probe acceleration of particles in the PWN up to energies of a few tens of TeV. Methods. We analyzed 81 h of 3C 58 data taken in the period between August 2013 and January 2014 with the MAGIC telescopes. Results. We detected VHE gamma-ray emission from 3C 58 with a significance of 5.7 sigma and an integral flux of 0.65% C. U. above 1 TeV. According to our results, 3C 58 is the least luminous VHE gamma-ray PWN ever detected at VHE and has the lowest flux at VHE to date. The differential energy spectrum between 400 GeV and 10 TeV is well described by a power-law function d phi/dE = f(0)(E/1 TeV)(-r) with f(0) = (2.0 + 0.4(stat) + 0.6(sys)) X 10(-13) cm(-2) S-1 TeV-1 and F = 2.4 +/- 0.2(stat) +/- 0.2(sys). The skymap is compatible with an unresolved source. Conclusions. We report the first significant detection of PWN 3C 58 at TeV energies. We compare our results with the expectations of time-dependent models in which electrons upscatter photon fields. The best representation favors a distance to the PWN of 2 kpc and far-infrared (FIR) values similar to cosmic microwave background photon fields. If we consider an unexpectedly high FIR density, the data can also be reproduced by models assuming a 3.2 kpc distance. A low magnetic field, far from equipartition, is required to explain the VHE data. Hadronic contribution from the hosting supernova remnant (SNR) requires an unrealistic energy budget given the density of the medium, disfavoring cosmic-ray acceleration in the SNR as origin of the VHE gamma-ray emission.

引用

页数：5

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