Please use this identifier to cite or link to this item:
https://hdl.handle.net/2440/12405
Type: | Journal article |
Title: | Observations of the supernova remnant W28 at TeV energies |
Author: | Rowell, G. Naito, T. Dazeley, S. Edwards, P. Gunji, S. Hara, T. Holder, J. Kawachi, A. Kifune, T. Matsubara, Y. Mizumoto, Y. Mori, M. Muraishi, H. Muraki, Y. Nishijima, K. Ogio, S. Patterson, J. Roberts, M. Sako, T. Sakurazawa, K. et al. |
Citation: | Astronomy and Astrophysics: a European journal, 2000; 359(1):337-346 |
Publisher: | E D P Sciences |
Issue Date: | 2000 |
ISSN: | 0004-6361 |
Statement of Responsibility: | G.P. Rowell, T. Naito, S.A. Dazeley, P.G. Edwards, S. Gunji, T. Hara, J. Holder, A. Kawachi, T. Kifune, Y. Matsubara, Y. Mizumoto, M. Mori, H. Muraishi, Y. Muraki, K. Nishijima, S. Ogio, J.R. Patterson, M.D. Roberts, T. Sako, K. Sakurazawa, R. Susukita, T. Tamura, T. Tanimori, G.J. Thornton, S. Yanagita, T. Yoshida and T. Yoshikoshi. For the CANGAROO collaboration |
Abstract: | The atmospheric Cerenkov imaging technique has been used to search for point-like and diffuse TeV gamma-ray emission from the southern supernova remnant, W28, and surrounding region. The search, made with the CANGAROO 3.8m telescope, encompasses a number of interesting features, the supernova remnant itself, the EGRET source 3EG J1800-2338, the pulsar PSR J1801-23, strong 1720 MHz OH masers and molecular clouds on the north and east boundaries of the remnant. An analysis tailored to extended and off-axis point sources was used, and no evidence for TeV gamma-ray emission from any of the features described above was found in data taken over the 1994 and 1995 seasons. Our upper limit (E>1.5 TeV) for a diffuse source of radius 0.25deg encompassing both molecular clouds was calculated at 6.64e-12 photons cm^-2 s^-1 (from 1994 data), and interpreted within the framework of a model predicting TeV gamma-rays from shocked-accelerated hadrons. Our upper limit suggests the need for some cutoff in the parent spectrum of accelerated hadrons and/or slightly steeper parent spectra than that used here (-2.1). As to the nature of 3EG J1800-2338, it possibly does not result entirely from pi-zero decay, a conclusion also consistent with its location in relation to W28. |
Rights: | © European Southern Observatory (ESO) 2000 Submitted to Cornell University’s online archive www.arXiv.org in 2000 by Gavin Rowell. Post-print sourced from www.arxiv.org. |
Published version: | http://arxiv.org/abs/astro-ph/0004280 |
Appears in Collections: | Aurora harvest 7 Physics publications |
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