Observation of an extended VHE gamma-ray emission from MSH 15-52 with CANGAROO-III

Abstract

We have observed the supernova remnant MSH 15-52 (G320.4-1.2), which contains the gamma-ray pulsar PSR B1509-58, using the CANGAROO-III imaging atmospheric Cherenkov telescope array from April to June in 2006. We detected gamma rays above 810 GeV at the 7 sigma level during a total effective exposure of 48.4 hours. We obtained a differential gamma-ray flux at 2.35 TeV of (7.9+/-1.5_{stat}+/-1.7_{sys}) \times 10^{-13} cm^{-2}s^{-1}TeV^{-1} with a photon index of 2.21+/-0.39_{stat}+/-0.40_{sys}, which is compatible with that of the H.E.S.S. observation in 2004. The morphology shows extended emission compared to our Point Spread Function. We consider the plausible origin of the high energy emission based on a multi-wavelength spectral analysis and energetics arguments.

arXiv comment9 pages, 9 figures, Accepted in ApJ

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Cited by in corpus (8)

• Modeling the spectral evolution of PWNe inside SNRs
• Detection of the energetic pulsar PSR B1509-58 and its pulsar wind nebula in MSH 15-52 using the Fermi-Large Area Telescope
• The soft gamma-ray pulsar population: an high-energy overview
• Multiband Emission from Pulsar Wind Nebulae: A Possible Injection Spectrum
• Revised predictions of neutrino fluxes from Pulsar Wind Nebulae
• High-Energy X-ray Imaging of the Pulsar Wind Nebula MSH~15-52: Constraints on Particle Acceleration and Transport
• CANGAROO-III observation of TeV gamma rays from the unidentified gamma-ray source HESS J1614-518
• CANGAROO-III Observation of TeV Gamma Rays from the vicinity of PSR B1 706-44