Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:astro-ph/0002252)
· References in the article
· Citations to the Article (28) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (6)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Very High Energy Gamma-Ray Observations of PSR B1509-58 with the CANGAROO 3.8 Meter Telescope
Authors:
Sako, T.; Matsubara, Y.; Muraki, Y.; Ramanamurthy, P. V.; Dazeley, S. A.; Edwards, P. G.; Gunji, S.; Hara, T.; Hara, S.; Holder, J.; Kamei, S.; Kawachi, A.; Kifune, T.; Kita, R.; Masaike, A.; Mizumoto, Y.; Mori, M.; Moriya, M.; Muraishi, H.; Naito, T.; Nishijima, K.; Ogio, S.; Patterson, J. R.; Rowell, G. P.; Sakurazawa, K.; Sato, Y.; Susukita, R.; Suzuki, R.; Tamura, T.; Tanimori, T.; Thornton, G. J.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T.
Affiliation:
AA(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan.; Present address: Laboratoire de Physique Nucléaire des Hautes Energies, Ecole Polytechnique, Palaiseau CEDEX 91128, France; ), AB(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AC(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AD(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AE(Department of Physics and Mathematical Physics, University of Adelaide, South Australia 5005, Australia), AF(Institute of Space and Astronautical Science, Sagamihara 229-8510, Japan), AG(Department of Physics, Yamagata University, Yamagata, Yamagata 990-8560, Japan), AH(Faculty of Management Information, Yamanashi Gakuin University, Kofu 400-8575, Japan), AI(Department of Physics, Tokyo Institute of Technology, Tokyo 152-8551, Japan), AJ(Institute for Cosmic Ray Research, University of Tokyo, Tokyo 188-8502, Japan.; Present address: Laboratoire de l'Accélérateur Linéaire, Université de Paris-Sud, BP 34, Orsay CEDEX 91898, France), AK(Department of Physics, Tokyo Institute of Technology, Tokyo 152-8551, Japan), AL(Institute for Cosmic Ray Research, University of Tokyo, Tokyo 188-8502, Japan), AM(Institute for Cosmic Ray Research, University of Tokyo, Tokyo 188-8502, Japan), AN(Faculty of Science, Ibaraki University, Mito 310-8521, Japan), AO(Department of Physics, Kyoto University, Kyoto 606-8502, Japan), AP(National Astronomical Observatory of Japan, Tokyo 181-8588, Japan), AQ(Institute for Cosmic Ray Research, University of Tokyo, Tokyo 188-8502, Japan), AR(Department of Physics, Tokyo Institute of Technology, Tokyo 152-8551, Japan), AS(Faculty of Science, Ibaraki University, Mito 310-8521, Japan), AT(National Astronomical Observatory of Japan, Tokyo 181-8588, Japan), AU(Department of Physics, Tokai University, Hiratsuka 259-1292, Japan), AV(Department of Physics, Tokyo Institute of Technology, Tokyo 152-8551, Japan), AW(Department of Physics and Mathematical Physics, University of Adelaide, South Australia 5005, Australia), AX(Institute for Cosmic Ray Research, University of Tokyo, Tokyo 188-8502, Japan), AY(Department of Physics, Tokyo Institute of Technology, Tokyo 152-8551, Japan), AZ(Institute for Cosmic Ray Research, University of Tokyo, Tokyo 188-8502, Japan), BA(Institute of Physical and Chemical Research, Wako 351-0198, Japan), BB(Department of Physics, Tokyo Institute of Technology, Tokyo 152-8551, Japan), BC(Faculty of Engineering, Kanagawa University, Yokohama 221-8686, Japan), BD(Department of Physics, Tokyo Institute of Technology, Tokyo 152-8551, Japan), BE(Department of Physics and Mathematical Physics, University of Adelaide, South Australia 5005, Australia), BF(Faculty of Science, Ibaraki University, Mito 310-8521, Japan), BG(Faculty of Science, Ibaraki University, Mito 310-8521, Japan), BH(Institute for Cosmic Ray Research, University of Tokyo, Tokyo 188-8502, Japan)
Publication:
The Astrophysical Journal, Volume 537, Issue 1, pp. 422-428. (ApJ Homepage)
Publication Date:
07/2000
Origin:
UCP
ApJ Keywords:
Gamma Rays: Observations, pulsars: individual (PSR B1509-58), ISM: Supernova Remnants
DOI:
10.1086/308998
Bibliographic Code:
2000ApJ...537..422S

Abstract

The gamma-ray pulsar PSR B1509-58 and its surrounding nebulae have been observed with the Collaboration of Australia and Nippon for a Gamma-Ray Observatory in the Outback (CANGAROO) 3.8 m imaging atmospheric Cerenkov telescope. The observations were performed from 1996 to 1998 in Woomera, South Australia, under different instrumental conditions with estimated threshold energies of 4.5 (1996), 1.9 (1997), and 2.5 TeV (1998) at zenith angles of ~30°. Although no strong evidence of gamma-ray emission was found, the lowest energy threshold data of 1997 showed a marginal excess of gamma-ray-like events at the 4.1 σ significance level. The corresponding gamma-ray flux is calculated to be (2.9+/-0.7)×10-12 cm-2 s-1 above 1.9 TeV. The observations of 1996 and 1998 yielded only upper limits (99.5% confidence level) of 1.9×10-12 cm-2 s-1 above 4.5 TeV and 2.0×10-12 cm-2 s-1 above 2.5 TeV. Assuming that the 1997 excess is due to very high energy (VHE) gamma-ray emission from the pulsar nebula, our result, when combined with the X-ray observations, leads to a value of the magnetic field strength ~=5 μG. This is consistent with the equipartition value previously estimated in the X-ray nebula surrounding the pulsar. No significant periodicity at the 150 ms pulsar period has been found in any of the three years' data. The flux upper limits set from our observations are 1 order of magnitude below previously reported detections of pulsed TeV emission.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints