FERMI-LAT DISCOVERY OF GeV GAMMA-RAY EMISSION FROM THE YOUNG SUPERNOVA REMNANT CASSIOPEIA A

被引：148

作者：

Abdo, A. A. ^{[1
,2
]}

Ackermann, M. ^{[3
,4
]}

Ajello, M. ^{[3
,4
]}

Allafort, A. ^{[3
,4
]}

Baldini, L. ^{[5
]}

Ballet, J. ^{[6
]}

Barbiellini, G. ^{[7
,8
]}

Baring, M. G. ^{[9
]}

Bastieri, D. ^{[10
,11
]}

Baughman, B. M. ^{[12
]}

Bechtol, K. ^{[3
,4
]}

Bellazzini, R. ^{[5
]}

Berenji, B. ^{[3
,4
]}

Blandford, R. D. ^{[3
,4
]}

Bloom, E. D. ^{[3
,4
]}

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

Borgland, A. W. ^{[3
,4
]}

Bregeon, J. ^{[5
]}

Brez, A. ^{[5
]}

Brigida, M. ^{[15
,16
]}

Bruel, P. ^{[17
]}

Buehler, R. ^{[3
,4
]}

Burnett, T. H. ^{[18
]}

Busetto, G. ^{[10
,11
]}

Caliandro, G. A. ^{[19
]}

Cameron, R. A. ^{[3
,4
]}

Caraveo, P. A. ^{[20
]}

Casandjian, J. M. ^{[6
]}

Cecchi, C. ^{[13
,14
]}

Celik, Oe. ^{[21
,22
,23
,24
]}

Charles, E. ^{[3
,4
]}

Chaty, S. ^{[6
]}

Chekhtman, A. ^{[1
,25
]}

Cheung, C. C. ^{[1
,2
]}

Chiang, J. ^{[3
,4
]}

Cillis, A. N. ^{[21
]}

Ciprini, S. ^{[14
]}

Claus, R. ^{[3
,4
]}

Cohen-Tanugi, J. ^{[26
]}

Conrad, J. ^{[27
,28
]}

Corbel, S. ^{[6
]}

de Palma, F. ^{[15
,16
]}

Digel, S. W. ^{[3
,4
]}

Dormody, M. ^{[29
,30
]}

do Couto e Silva, E. ^{[3
,4
]}

Drell, P. S. ^{[3
,4
]}

Dubois, R. ^{[3
,4
]}

Dumora, D. ^{[31
,32
]}

Edmonds, Y. ^{[3
,4
]}

Farnier, C. ^{[26
]}

机构：

[1] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA

[2] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA

[3] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA

[4] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA

[5] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[6] Univ Paris Diderot, CNRS, CEA Saclay, Lab AIM,CEA IRFU,Serv Astrophys, F-91191 Gif Sur Yvette, France

[7] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy

[8] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy

[9] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA

[10] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[11] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy

[12] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[13] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[14] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy

[15] Univ & Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy

[16] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy

[17] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France

[18] Univ Washington, Dept Phys, Seattle, WA 98195 USA

[19] CSIC, IEEC, Inst Ciencies Espai, Barcelona 08193, Spain

[20] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy

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

[22] CRESST, Greenbelt, MD 20771 USA

[23] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA

[24] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA

[25] George Mason Univ, Fairfax, VA 22030 USA

[26] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France

[27] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden

[28] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden

[29] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA

[30] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA

[31] Univ Bordeaux, CEN Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France

[32] CEN Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France

[33] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy

[34] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy

[35] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan

[36] ASI, Sci Data Ctr, I-00044 Frascati, Roma, Italy

[37] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

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

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

[40] Max Planck Inst Radioastron, D-53121 Bonn, Germany

[41] Univ Alabama, CSPAR, Huntsville, AL 35899 USA

[42] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden

[43] Waseda Univ, Shinjuku Ku, Tokyo 1698050, Japan

[44] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan

[45] RIKEN, Cosm Radiat Lab, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan

[46] CNRS, UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France

[47] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy

[48] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA

[49] Univ Tokyo, Dept Phys, Grad Sch Sci, Bunkyo Ku, Tokyo 1130033, Japan

[50] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2010年 / 710卷 / 01期

基金：

瑞典研究理事会;

关键词：

acceleration of particles; ISM: individual objects (Cassiopeia A); radiation mechanisms: non-thermal; MAGNETIC-FIELD; COSMIC-RAYS; PARTICLE-ACCELERATION; SYNCHROTRON EMISSION; SHOCK ACCELERATION; AMPLIFICATION; RADIO; TELESCOPE; OBJECT;

D O I：

10.1088/2041-8205/710/1/L92

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the first detection of GeV high-energy gamma-ray emission from a young supernova remnant (SNR) with the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope. These observations reveal a source with no discernible spatial extension detected at a significance level of 12.2 sigma above 500 MeV a a location that is consistent with the position of the remnant of the supernova explosion that occurred around 1680 in the Cassiopeia constellation-Cassiopeia A (Cas A). The gamma-ray flux and spectral shape of the source are consistent with a scenario in which the gamma-ray emission originates from relativistic particles accelerated in the shell of this remnant. The total content of cosmic rays (electrons and protons) accelerated in Cas A can be estimated as W-CR similar or equal to (1-4) x 10(49) erg thanks to the well-known density in the remnant assuming that the observed gamma ray originates in the SNR shell(s). The magnetic field in the radio-emitting plasma can be robustly constrained as B >= 0.1 mG, providing new evidence of the magnetic field amplification at the forward shock and the strong field in the shocked ejecta.

引用

页码：L92 / L97

页数：6

共 43 条

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