TeV gamma rays from PSR 1706-44

Abstract

Observations made with the University of Durham Mark 6 atmospheric Cerenkov telescope confirm that PSR B1706-44 is a very high energy gamma-ray emitter. There is no indication from our dataset that the very high energy gamma-rays are pulsed, in contrast to the findings at < 20 GeV, which indicate that more than 80% of the flux is pulsed. The flux at E > 300 GeV is estimated to be (3.9 +/- 0.7 (statistical)) x 10^-11 cm^-2 s^-1.

9 pages, 3 figures, accepted for publication in Astroparticle Physics

References in corpus (1)

• Detection of Gamma Rays of Up to 50 TeV From the Crab Nebula

Cited by in corpus (16)

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• XMM-Newton Observations of PSR B1706-44
• Neutrinos from the pulsar wind nebulae
• Gamma-rays and cosmic-rays from a pulsar in Cygnus OB2
• Detection of very-high-energy gamma-ray emission from the vicinity of PSR B1706-44 and G343.1-2.3 with H.E.S.S
• TeV Gamma-rays from the Northern Sky Pulsar Wind Nebulae
• On the association of G343.1-2.3 and PSR 1706-44
• High Energy Processes in Pulsar Wind Nebulae
• Geomagnetic effects on atmospheric Cerenkov images
• The Uuniversity of Durham Mark 6 Gamma Ray Telescope
• Possible TeV Source Candidates In The Unidentified EGRET Sources
• Reanalysis of Data Taken by the CANGAROO 3.8 Meter Imaging Atmospheric Cherenkov Telescope: PSR B1706-44, SN 1006, and Vela
• CANGAROO-III Observation of TeV Gamma Rays from the vicinity of PSR B1 706-44
• Observations of TeV gamma rays from Markarian 501 at large zenith angles