Detection of sub-TeV gamma rays from the Galactic center direction by CANGAROO-II

被引：173

作者：

Tsuchiya, K ^{[1
]}

Enomoto, R

Ksenofontov, LT

Mori, M

Naito, T

Asahara, A

Bicknell, GV

Clay, RW

Doi, Y

Edwards, PG

Gunji, S

Hara, S

Hara, T

Hattori, T

Hayashi, S

Itoh, C

Kabuki, S

Kajino, F

Katagiri, H

Kawachi, A

Kifune, T

Kubo, H

Kurihara, T

Kurosaka, R

Kushida, J

Matsubara, Y

Miyashita, Y

Mizumoto, Y

Moro, H

Muraishi, H

Muraki, Y

Nakase, T

Nishida, D

Nishijima, K

Ohishi, M

Okumura, K

Patterson, JR

Protheroe, RJ

Sakamoto, N

Sakurazawa, K

Swaby, DL

Tanimori, T

Tanimura, H

Thornton, G

Tokanai, F

Uchida, T

Watanabe, S

Yamaoka, T

Yanagita, S

Yoshida, T

机构：

[1] Univ Tokyo, ICRR, Chiba 2778582, Japan

[2] Yamanashi Gakuin Univ, Fac Management Informat, Yamanashi 4008575, Japan

[3] Kyoto Univ, Dept Phys, Grad Sch Sci, Kyoto 6068502, Japan

[4] Australian Natl Univ, RSAA, Weston, ACT 2611, Australia

[5] Univ Adelaide, Dept Phys, Adelaide, SA 5005, Australia

[6] Yamagata Univ, Dept Phys, Yamagata 9908560, Japan

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

[8] Tokai Univ, Dept Phys, Kanagawa 2591292, Japan

[9] Konan Univ, Dept Phys, Hyogo 6588501, Japan

[10] Ibaraki Prefectural Univ Hlth Sci, Ibaraki 3000394, Japan

[11] Shinshu Univ, Fac Engn, Nagano 4808553, Japan

[12] Nagoya Univ, STE Lab, Aichi 4648602, Japan

[13] Natl Astron Observ Japan, Tokyo 1818588, Japan

[14] Kitasato Univ, Sch Allied Hlth Sci, Kanagawa 2288555, Japan

[15] Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan

[16] Ibaraki Univ, Fac Sci, Ibaraki 3108512, Japan

[17] Osaka City Univ, Dept Phys, Osaka 5588585, Japan

来源：

ASTROPHYSICAL JOURNAL | 2004年 / 606卷 / 02期

基金：

欧盟地平线“2020”; 澳大利亚研究理事会; 日本学术振兴会;

关键词：

Galaxy : center; gamma rays : observations;

D O I：

10.1086/421292

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have detected sub-TeV gamma-ray emission from the direction of the Galactic center ( GC) using the CANGAROO-II Imaging Atmospheric Cerenkov Telescope. We detected a statistically significant excess at energies greater than 250 GeV. The flux was 1 order of magnitude lower than that of the Crab Nebula at 1 TeV with a soft spectrum proportional to E-4.6 +/- 0.5. The signal centroid is consistent with the GC direction, and the observed profile is consistent with a pointlike source. Our data suggest that the GeV source 3EG J1746 - 2851 is identical to this TeV source, and we study the combined spectra to determine the possible origin of the gamma-ray emission. We also obtain an upper limit on the cold dark matter density in the Galactic halo.

引用

页码：L115 / L118

页数：4

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