FERMI-LAT STUDY OF GAMMA-RAY EMISSION IN THE DIRECTION OF SUPERNOVA REMNANT W49B

被引：92

作者：

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

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

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

Baldini, L. ^{[5
]}

Ballet, J. ^{[6
]}

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

Bastieri, D. ^{[9
,10
]}

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

Bellazzini, R. ^{[5
]}

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

Bonamente, E. ^{[11
,12
]}

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

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

Bregeon, J. ^{[5
]}

Brez, A. ^{[5
]}

Brigida, M. ^{[13
,14
]}

Bruel, P. ^{[15
]}

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

Buson, S. ^{[9
,10
]}

Caliandro, G. A. ^{[16
]}

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

Caraveo, P. A. ^{[17
]}

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

Cecchi, C. ^{[11
,12
]}

Celik, Oe ^{[18
,19
,20
,21
]}

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

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

Ciprini, S. ^{[12
]}

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

Cohen-Tanugi, J. ^{[22
]}

Conrad, J. ^{[23
,24
]}

Dermer, C. D. ^{[1
]}

de Palma, F. ^{[13
,14
]}

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

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

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

Dumora, D. ^{[25
,26
]}

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

Funk, S. ^{[3
,4
]}

Fusco, P. ^{[13
,14
]}

Gargano, F. ^{[14
]}

Gehrels, N. ^{[18
]}

Giglietto, N. ^{[13
,14
]}

Giordano, F. ^{[13
,14
]}

Giroletti, M. ^{[27
]}

Glanzman, T. ^{[3
,4
]}

Godfrey, G. ^{[3
,4
]}

Grenier, I. A. ^{[6
]}

Grondin, M-H. ^{[25
,26
]}

Grove, J. E. ^{[1
]}

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, Lab AIM, CEA IRFU, CNRS,CEA Saclay, 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] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

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

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

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

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

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

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

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

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

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

[19] CRESST, Greenbelt, MD 20771 USA

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

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

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

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

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

[25] Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France

[26] Univ Bordeaux, UMR 5797, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France

[27] INAF Ist Radioastron, I-40129 Bologna, Italy

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

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

[30] ICREA, Barcelona, Spain

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

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

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

[34] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan

[35] JAXA, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan

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

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

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

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

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

[41] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan

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

[43] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[44] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria

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

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

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

[48] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA

[49] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA

[50] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 722卷 / 02期

关键词：

acceleration of particles; ISM: individual objects (W49B); radiation mechanisms: non-thermal; LARGE-AREA TELESCOPE; X-RAY; PARTICLE-ACCELERATION; RX J1713.7-3946; COSMIC-RAYS; CATALOG; RADIO; DISCOVERY; PULSARS; ORIGIN;

D O I：

10.1088/0004-637X/722/2/1303

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present an analysis of the gamma-ray data obtained with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope in the direction of SNR W49B (G43.3-0.2). A bright unresolved gamma-ray source detected at a significance of 38 sigma is found to coincide with SNR W49B. The energy spectrum in the 0.2-200 GeV range gradually steepens toward high energies. The luminosity is estimated to be 1.5 x 10(36) (D/8 kpc)(2) erg s(-1) in this energy range. There is no indication that the gamma-ray emission comes from a pulsar. Assuming that the supernova remnant (SNR) shell is the site of gamma-ray production, the observed spectrum can be explained either by the decay of neutral pi mesons produced through the proton-proton collisions or by electron bremsstrahlung. The calculated energy density of relativistic particles responsible for the LAT flux is estimated to be remarkably large, U-e,U-p > 10(4) eV cm(-3), for either gamma-ray production mechanism.

引用

页码：1303 / 1311

页数：9

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