FERMI LARGE AREA TELESCOPE OBSERVATIONS OF THE SUPERNOVA REMNANT W28 (G6.4-0.1)

被引：182

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
]}

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

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

Bellazzini, R. ^{[5
]}

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

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

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

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

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

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

Brandt, T. J. ^{[13
,14
]}

Bregeon, J. ^{[5
]}

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

Bruel, P. ^{[17
]}

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

Buson, S. ^{[9
]}

Caliandro, G. A. ^{[18
]}

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

Caraveo, P. A. ^{[19
]}

Carrigan, S. ^{[10
]}

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

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

Celik, Oe. ^{[20
,21
,22
,23
]}

Chekhtman, A. ^{[1
,24
]}

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

Ciprini, S. ^{[12
]}

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

Cohen-Tanugi, J. ^{[25
]}

Conrad, J. ^{[26
,27
]}

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

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

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

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

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

Dumora, D. ^{[28
,29
]}

Farnier, C. ^{[25
]}

Favuzzi, C. ^{[15
,16
]}

Fegan, S. J. ^{[17
]}

Fukazawa, Y. ^{[30
]}

Fukui, Y. ^{[31
]}

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

Fusco, P. ^{[15
,16
]}

Gargano, F. ^{[16
]}

Gehrels, N. ^{[20
]}

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, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, 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, CEA Saclay, Serv Astrophys, CNRS,Lab AIM,CEA IRFU, 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] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France

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

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

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

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

[21] CRESST, Greenbelt, MD 20771 USA

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

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

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

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

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

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

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

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

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

[31] Nagoya Univ, Dept Phys & Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan

[32] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA

[33] ICREA, Barcelona, Spain

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

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

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

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

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

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

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

[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, Dept Phys, Santa Cruz Inst Particle 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 / 718卷 / 01期

基金：

瑞典研究理事会; 美国国家航空航天局;

关键词：

acceleration of particles; cosmic rays; gamma rays: ISM; ISM: individual objects (W28; G6.4-0.1); ISM: supernova remnants; GAMMA-RAY EMISSION; H-II REGIONS; SHOCKED MOLECULAR GAS; GALACTIC COSMIC-RAYS; MHZ OH MASERS; IC; 443; DISCOVERY; OUTFLOW; CLOUDS; W44;

D O I：

10.1088/0004-637X/718/1/348

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present detailed analysis of two gamma-ray sources, 1FGL J1801.3-2322c and 1FGL J1800.5-2359c, that have been found toward the supernova remnant (SNR) W28 with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. 1FGL J1801.3-2322c is found to be an extended source within the boundary of SNR W28, and to extensively overlap with the TeV gamma-ray source HESS J1801-233, which is associated with a dense molecular cloud interacting with the SNR. The gamma-ray spectrum measured with the LAT from 0.2 to 100 GeV can be described by a broken power-law function with a break at similar to 1 GeV and photon indices of 2.09 +/- 0.08 (stat) +/- 0.28 (sys) below the break and 2.74 +/- 0.06 (stat) +/- 0.09 (sys) above the break. Given the clear association between HESS J1801-233 and the shocked molecular cloud and a smoothly connected spectrum in the GeV-TeV band, we consider the origin of the gamma-ray emission in both GeV and TeV ranges to be the interaction between particles accelerated in the SNR and the molecular cloud. The decay of neutral pions produced in interactions between accelerated hadrons and dense molecular gas provides a reasonable explanation for the broadband gamma-ray spectrum. 1FGL J1800.5-2359c, located outside the southern boundary of SNR W28, cannot be resolved. An upper limit on the size of the gamma-ray emission was estimated to be similar to 16' using events above similar to 2 GeV under the assumption of a circular shape with uniform surface brightness. It appears to coincide with the TeV source HESS J1800-240B, which is considered to be associated with a dense molecular cloud that contains the ultra compact H II region W28A2 (G5.89-0.39). We found no significant gamma-ray emission in the LAT energy band at the positions of TeV sources HESS J1800-230A and HESS J1800-230C. The LAT data for HESS J1800-230A combined with the TeV data points indicate a spectral break between 10 GeV and 100 GeV.

引用

页码：348 / 356

页数：9

共 48 条

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