DETAILED INVESTIGATION OF THE GAMMA-RAY EMISSION IN THE VICINITY OF SNR W28 WITH FERMI-LAT

被引:43
作者
Hanabata, Y. [1 ]
Katagiri, H. [2 ]
Hewitt, J. W. [3 ,4 ]
Ballet, J. [5 ]
Fukazawa, Y. [6 ]
Fukui, Y. [7 ]
Hayakawa, T. [7 ]
Lemoine-Goumard, M. [8 ]
Pedaletti, G. [9 ]
Strong, A. W. [10 ]
Torres, D. F. [9 ,11 ]
Yamazaki, R. [12 ]
机构
[1] Univ Tokyo, Inst Cosmic Ray Res, Kashiwa, Chiba 2778582, Japan
[2] Ibaraki Univ, Coll Sci, Bunkyo Ku, Mito, Ibaraki 3108512, Japan
[3] Univ Maryland, CRESST, Baltimore, MD 21250 USA
[4] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
[5] Univ Paris Diderot, Serv Astrophys, CEA Saclay, CNRS,CEA IRFU,Lab AIM, F-91191 Gif Sur Yvette, France
[6] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan
[7] Nagoya Univ, Dept Phys & Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan
[8] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France
[9] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain
[10] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany
[11] ICREA, Barcelona, Spain
[12] Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2525258, Japan
关键词
acceleration of particles; cosmic rays; diffusion; gamma rays: ISM; ISM: supernova remnants; LARGE-AREA TELESCOPE; SUPERNOVA REMNANT W28; DIFFUSIVE SHOCK ACCELERATION; GALACTIC COSMIC-RAYS; MHZ OH MASERS; H-II REGIONS; MOLECULAR CLOUDS; HIGH-ENERGY; IC; 443; STREAMING INSTABILITY;
D O I
10.1088/0004-637X/786/2/145
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present a detailed investigation of the gamma-ray emission in the vicinity of the supernova remnant (SNR) W28 (G6.4-0.1) observed by the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. We detected significant gamma-ray emission spatially coincident with TeV sources HESS J1800-240A, B, and C, located outside the radio boundary of the SNR. Their spectra in the 2-100 GeV band are consistent with the extrapolation of the power-law spectra of the TeV sources. We also identified a new source of GeV emission, dubbed Source W, which lies outside the boundary of TeV sources and coincides with radio emission from the western part of W28. All of the GeV gamma-ray sources overlap with molecular clouds in the velocity range from 0 to 20 km s(-1). Under the assumption that the gamma-ray emission toward HESS J1800-240A, B, and C comes from pi(0) decay due to the interaction between the molecular clouds and cosmic rays (CRs) escaping from W28, they can be naturally explained by a single model in which the CR diffusion coefficient is smaller than the theoretical expectation in the interstellar space. The total energy of the CRs escaping from W28 is constrained through the same modeling to be larger than similar to 2 x 10(49) erg. The emission from Source W can also be explained with the same CR escape scenario.
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