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Title:
Very High Energy Gamma Rays from the VELA Pulsar Direction
Authors:
Yoshikoshi, T.; Kifune, T.; Dazeley, S. A.; Edwards, P. G.; Hara, T.; Hayami, Y.; Kakimoto, F.; Konishi, T.; Masaike, A.; Matsubara, Y.; Matsuoka, T.; Mizumoto, Y.; Mori, M.; Muraishi, H.; Muraki, Y.; Naito, T.; Nishijima, K.; Oda, S.; Ogio, S.; Ohsaki, T.; Patterson, J. R.; Roberts, M. D.; Rowell, G. P.; Sako, T.; Sakurazawa, K.; Susukita, R.; Suzuki, A.; Tamura, T.; Tanimori, T.; Thornton, G. J.; Yanagita, S.; Yoshida, T.
Publication:
Astrophysical Journal Letters v.487, p.L65 (ApJL Homepage)
Publication Date:
09/1997
Origin:
APJ
ApJ Keywords:
GAMMA RAYS: OBSERVATIONS, ISM: INDIVIDUAL NAME: VELA SUPERNOVA REMNANT, ISM: MAGNETIC FIELDS, STARS: PULSARS: INDIVIDUAL NAME: VELA PULSAR, ISM: SUPERNOVA REMNANTS
DOI:
10.1086/310874
Bibliographic Code:
1997ApJ...487L..65Y

Abstract

We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Cerenkov telescope near Woomera, South Australia between 1993 January and 1995 March. Evidence of an unpulsed gamma-ray signal has been detected at the 5.8 sigma level. The detected gamma-ray flux is (2.9 +/- 0.5 +/- 0.4) x 10-12 photons cm-2 s-1 above 2.5 +/- 1.0 TeV, and the signal is consistent with steady emission over the 2 years. The gamma-ray emission region is offset from the Vela pulsar position to the southeast by about 0.dg13. No pulsed emission modulated with the pulsar period has been detected, and the 95% confidence flux upper limit to the pulsed emission from the pulsar is (3.7 +/- 0.7) x 10-13 photons cm-2 s-1 above 2.5 +/- 1.0 TeV.
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