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Detection of the Characteristic Pion-Decay Signature in Supernova Remnants

Cosmic rays are particles (mostly protons) accelerated to relativistic speeds. Despite wide agreement that supernova remnants (SNRs) are the sources of galactic cosmic rays, unequivocal evidence for the acceleration of protons in these objects is still lacking. When accelerated protons encounter int... Full description

Journal Title: Science 2013, Vol.339(6121), pp.807-811
Main Author: Ackermann, M.
Other Authors: Jackson, Miranda S. , Zimmer, S. , Et Al., M. , Ajello, A. , Allafort, L. , Baldini, J. , Ballet, G. , Barbiellini, M. G. , Baring, D. , Bastieri, K. , Bechtol, R. , Bellazzini, R. D. , Blandford, E. D. , Bloom, E. , Bonamente, A. W. , Borgland, E. , Bottacini, T. J. , Brandt, J. , Bregeon
Format: Electronic Article Electronic Article
Language: English
Subjects:
ID: ISSN: 0036-8075 ; ISSN: 0036-8075 ; DOI: 10.1126/science.1231160
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recordid: swepuboai:DiVA.org:su-88281
title: Detection of the Characteristic Pion-Decay Signature in Supernova Remnants
format: Article
creator:
  • Ackermann, M.
  • Jackson, Miranda S.
  • Zimmer, S.
  • Et Al., M.
  • Ajello, A.
  • Allafort, L.
  • Baldini, J.
  • Ballet, G.
  • Barbiellini, M. G.
  • Baring, D.
  • Bastieri, K.
  • Bechtol, R.
  • Bellazzini, R. D.
  • Blandford, E. D.
  • Bloom, E.
  • Bonamente, A. W.
  • Borgland, E.
  • Bottacini, T. J.
  • Brandt, J.
  • Bregeon
subjects:
  • Natural Sciences
  • Physical Sciences
  • Naturvetenskap
  • Fysik
  • Gamma-Ray Emission
  • Large-Area Telescope
  • Ic 443
  • Cosmic-Rays
  • Fermi Lat
  • Snr W44
  • Acceleration
  • Clouds
  • Discovery
  • Radiation
ispartof: Science, 2013, Vol.339(6121), pp.807-811
description: Cosmic rays are particles (mostly protons) accelerated to relativistic speeds. Despite wide agreement that supernova remnants (SNRs) are the sources of galactic cosmic rays, unequivocal evidence for the acceleration of protons in these objects is still lacking. When accelerated protons encounter interstellar material, they produce neutral pions, which in turn decay into gamma rays. This offers a compelling way to detect the acceleration sites of protons. The identification of pion-decay gamma rays has been difficult because high-energy electrons also produce gamma rays via bremsstrahlung and inverse Compton scattering. We detected the characteristic pion-decay feature in the gamma-ray spectra of two SNRs, IC 443 and W44, with the Fermi Large Area Telescope. This detection provides direct evidence that cosmic-ray protons are accelerated in SNRs.
language: eng
source:
identifier: ISSN: 0036-8075 ; ISSN: 0036-8075 ; DOI: 10.1126/science.1231160
fulltext: no_fulltext
issn:
  • 0036-8075
  • 00368075
url: Link


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titleDetection of the Characteristic Pion-Decay Signature in Supernova Remnants
creatorAckermann, M. ; Jackson, Miranda S. ; Zimmer, S. ; Et Al., M. ; Ajello, A. ; Allafort, L. ; Baldini, J. ; Ballet, G. ; Barbiellini, M. G. ; Baring, D. ; Bastieri, K. ; Bechtol, R. ; Bellazzini, R. D. ; Blandford, E. D. ; Bloom, E. ; Bonamente, A. W. ; Borgland, E. ; Bottacini, T. J. ; Brandt, J. ; Bregeon
ispartofScience, 2013, Vol.339(6121), pp.807-811
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subjectNatural Sciences ; Physical Sciences ; Naturvetenskap ; Fysik ; Gamma-Ray Emission ; Large-Area Telescope ; Ic 443 ; Cosmic-Rays ; Fermi Lat ; Snr W44 ; Acceleration ; Clouds ; Discovery ; Radiation
descriptionCosmic rays are particles (mostly protons) accelerated to relativistic speeds. Despite wide agreement that supernova remnants (SNRs) are the sources of galactic cosmic rays, unequivocal evidence for the acceleration of protons in these objects is still lacking. When accelerated protons encounter interstellar material, they produce neutral pions, which in turn decay into gamma rays. This offers a compelling way to detect the acceleration sites of protons. The identification of pion-decay gamma rays has been difficult because high-energy electrons also produce gamma rays via bremsstrahlung and inverse Compton scattering. We detected the characteristic pion-decay feature in the gamma-ray spectra of two SNRs, IC 443 and W44, with the Fermi Large Area Telescope. This detection provides direct evidence that cosmic-ray protons are accelerated in SNRs.
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15Bonamente, A. W.
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17Bottacini, T. J.
18Brandt, J.
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titleDetection of the Characteristic Pion-Decay Signature in Supernova Remnants
descriptionCosmic rays are particles (mostly protons) accelerated to relativistic speeds. Despite wide agreement that supernova remnants (SNRs) are the sources of galactic cosmic rays, unequivocal evidence for the acceleration of protons in these objects is still lacking. When accelerated protons encounter interstellar material, they produce neutral pions, which in turn decay into gamma rays. This offers a compelling way to detect the acceleration sites of protons. The identification of pion-decay gamma rays has been difficult because high-energy electrons also produce gamma rays via bremsstrahlung and inverse Compton scattering. We detected the characteristic pion-decay feature in the gamma-ray spectra of two SNRs, IC 443 and W44, with the Fermi Large Area Telescope. This detection provides direct evidence that cosmic-ray protons are accelerated in SNRs.
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titleDetection of the Characteristic Pion-Decay Signature in Supernova Remnants
authorAckermann, M. ; Jackson, Miranda S. ; Zimmer, S. ; Et Al., M. ; Ajello, A. ; Allafort, L. ; Baldini, J. ; Ballet, G. ; Barbiellini, M. G. ; Baring, D. ; Bastieri, K. ; Bechtol, R. ; Bellazzini, R. D. ; Blandford, E. D. ; Bloom, E. ; Bonamente, A. W. ; Borgland, E. ; Bottacini, T. J. ; Brandt, J. ; Bregeon
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1Jackson, Miranda S.
2Zimmer, S.
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4Ajello, A.
5Allafort, L.
6Baldini, J.
7Ballet, G.
8Barbiellini, M. G.
9Baring, D.
10Bastieri, K.
11Bechtol, R.
12Bellazzini, R. D.
13Blandford, E. D.
14Bloom, E.
15Bonamente, A. W.
16Borgland, E.
17Bottacini, T. J.
18Brandt, J.
19Bregeon, M.
20Brigida, P.
21Bruel, R.
22Buehler, G.
23Busetto, S.
24Buson, G. A.
25Caliandro, R. A.
26Cameron, P. A.
27Caraveo, J. M.
28Casandjian, C.
29Cecchi, O.
30Celik, E.
31Charles, S.
32Chaty, R. C. G.
33Chaves, A.
34Chekhtman, C. C.
35Cheung, J.
36Chiang, G.
37Chiaro, A. N.
38Cillis, S.
39Ciprini, R.
40Claus, J.
41Cohen-Tanugi, L. R.
42Cominsky, Jan
43Conrad, S.
44Corbel, S.
45Cutini, F.
46D'Ammando, A.
47de Angelis, F.
48de Palma, C. D.
49Dermer, E.
50do Couto e Silva, P. S.
51Drell, A.
52Drlica-Wagner, L.
53Falletti, C.
54Favuzzi, E. C.
55Ferrara, A.
56Franckowiak, Y.
57Fukazawa, S.
58Funk, P.
59Fusco, F.
60Gargano, S.
61Germani, N.
62Giglietto, P.
63Giommi, F.
64Giordano, M.
65Giroletti, T.
66Glanzman, G.
67Godfrey, I. A.
68Grenier, M. -H
69Grondin, J. E.
70Grove, S.
71Guiriec, D.
72Hadasch, Y.
73Hanabata, A. K.
74Harding, M.
75Hayashida, K.
76Hayashi, E.
77Hays, J. W.
78Hewitt, A. B.
79Hill, R. E.
80Hughes, T.
81Jogler, G.
82Johannesson, A. S.
83Johnson, T.
84Kamae, J.
85Kataoka, J.
86Katsuta, J.
87Knoedlseder, M.
88Kuss, J.
89Lande, Stefan
90Larsson, L.
91Latronico, M.
92Lemoine-Goumard, F.
93Longo, F.
94Loparco, M. N.
95Lovellette, P.
96Lubrano, G. M.
97Madejski, F.
98Massaro, M.
99Mayer, M. N.
100Mazziotta, J. E.
101McEnery, J.
102Mehault, P. F.
103Michelson, R. P.
104Mignani, W.
105Mitthumsiri, T.
106Mizuno, A. A.
107Moiseev, M. E.
108Monzani, A.
109Morselli, I. V.
110Moskalenko, S.
111Murgia, T.
112Nakamori, R.
113Nemmen, E.
114Nuss, M.
115Ohno, T.
116Ohsugi, N.
117Omodei, M.
118Orienti, E.
119Orlando, J. F.
120Ormes, D.
121Paneque, J. S.
122Perkins, M.
123Pesce-Rollins, F.
124Piron, G.
125Pivato, S.
126Raino, R.
127Rando, M.
128Razzano, S.
129Razzaque, A.
130Reimer, O.
131Reimer, S.
132Ritz, C.
133Romoli, M.
134Sanchez-Conde, A.
135Schulz, C.
136Sgro, P. E.
137Simeon, E. J.
138Siskind, D. A.
139Smith, G.
140Spandre, P.
141Spinelli, F. W.
142Stecker, A. W.
143Strong, D. J.
144Suson, H.
145Tajima, H.
146Takahashi, T.
147Tanaka, J. G.
148Thayer, J. B.
149Thayer, D. J.
150Thompson, S. E.
151Thorsett, L.
152Tibaldo, O.
153Tibolla, M.
154Tinivella, E.
155Troja, Y.
156Uchiyama, T. L.
157Usher, J.
158Vandenbroucke, V.
159Vasileiou, G.
160Vianello, V.
161Vitale, A. P.
162Waite, M.
163Werner, B. L.
164Winer, K. S.
165Wood, M.
166Wood, R.
167Yamazaki, Zhaoyu
168Yang, Zhaoyu
atitleDetection of the Characteristic Pion-Decay Signature in Supernova Remnants
jtitleScience
date2013
risdate2013
volume339
issue6121
spage807
epage811
issn0036-8075
genrearticle
ristypeJOUR
abstractCosmic rays are particles (mostly protons) accelerated to relativistic speeds. Despite wide agreement that supernova remnants (SNRs) are the sources of galactic cosmic rays, unequivocal evidence for the acceleration of protons in these objects is still lacking. When accelerated protons encounter interstellar material, they produce neutral pions, which in turn decay into gamma rays. This offers a compelling way to detect the acceleration sites of protons. The identification of pion-decay gamma rays has been difficult because high-energy electrons also produce gamma rays via bremsstrahlung and inverse Compton scattering. We detected the characteristic pion-decay feature in the gamma-ray spectra of two SNRs, IC 443 and W44, with the Fermi Large Area Telescope. This detection provides direct evidence that cosmic-ray protons are accelerated in SNRs.
doi10.1126/science.1231160
pages807-811
orcidid0000-0002-0014-7809: 0000-0001-6885-7156
eissn10959203