Very high energy gamma rays from the vela pulsar direction

T. Yoshikoshi, T. Kifune, S. A. Dazeley, P. G. Edwards, T. Hara, Y. Hayami, F. Kakimoto, T. Konishi, A. Masaike, Y. Matsubara, T. Matsuoka, Y. Mizumoto, M. Mori, H. Muraishi, Y. Muraki, T. Naito, K. Nishijima, S. Oda, S. Ogio, T. OhsakiJ. R. Patterson, M. D. Roberts, G. P. Rowell, T. Sako, K. Sakurazawa, R. Susukita, A. Suzuki, T. Tamura, T. Tanimori, G. J. Thornton, S. Yanagita, T. Yoshida

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61 Citations (Scopus)


We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Čerenkov 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 σ level. The detected gamma-ray flux is (2.9 ± 0.5 ± 0.4) × 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°.13. 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) × 10-13 photons cm-2 s-1 above 2.5 ± 1.0 TeV.

Original languageEnglish
Pages (from-to)L65-L68
JournalAstrophysical Journal
Issue number1 PART II
Publication statusPublished - 1997
Externally publishedYes

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science


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