CANGAROO-III OBSERVATION OF TeV GAMMA RAYS FROM THE UNIDENTIFIED GAMMA-RAY SOURCE HESS J1614-518
- Department of Physics, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502 (Japan)
- Faculty of Science, Ibaraki University, Mito, Ibaraki 310-8512 (Japan)
- Graduate School of Advanced Science and Engineering, Faculty of Science and Engineering, Waseda University, 3-4-1 Ohkubo, Shinjuku, Tokyo 169-0072 (Japan)
- Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582 (Japan)
- Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292 (Japan)
- Research School of Astronomy and Astrophysics, Australian National University, ACT 2611 (Australia)
- School of Chemistry and Physics, University of Adelaide, SA 5005 (Australia)
- CSIRO Astronomy and Space Science, Australia Telescope National Facility, Epping, NSW 2121 (Australia)
- Department of Physics, Yamagata University, Yamagata, Yamagata 990-8560 (Japan)
- Faculty of Management Information, Yamanashi Gakuin University, Kofu, Yamanashi 400-8575 (Japan)
- Department of Physics, Konan University, Kobe, Hyogo 658-8501 (Japan)
- Department of Physical Science, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526 (Japan)
We report the detection, with the CANGAROO-III imaging atmospheric Cherenkov telescope array, of a very high energy gamma-ray signal from the unidentified gamma-ray source HESS J1614-518, which was discovered in the H.E.S.S. Galactic plane survey. Diffuse gamma-ray emission was detected above 760 GeV at the 8.9{sigma} level during an effective exposure of 54 hr from 2008 May to August. The spectrum can be represented by a power law: (8.2 {+-} 2.2{sub stat} {+-} 2.5{sub sys}) x 10{sup -12} x (E/1 TeV){sup -}{gamma} cm{sup -2} s{sup -1} TeV{sup -1} with a photon index {gamma} of 2.4 {+-} 0.3{sub stat} {+-} 0.2{sub sys}, which is compatible with that of the H.E.S.S. observations. By combining our result with multiwavelength data, we discuss the possible counterparts for HESS J1614-518 and consider radiation mechanisms based on hadronic and leptonic processes for a supernova remnant (SNR), stellar winds from massive stars, and a pulsar wind nebula (PWN). Although a leptonic origin from a PWN driven by an unknown pulsar remains possible, hadronic-origin emission from an unknown SNR is preferred.
- OSTI ID:
- 21587358
- Journal Information:
- Astrophysical Journal, Vol. 740, Issue 2; Other Information: DOI: 10.1088/0004-637X/740/2/78; Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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