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This work reports on the discovery of HESS J1514-591, a VHE gamma-ray sourcefound at the pulsar wind nebula (PWN) MSH 15-52 and its associated pulsar PSRB1509-58. The discovery was made with the High Energy Stereoscopic System(H.E.S.S.), which currently provides the most sensitive measurement in theenergy range of about 0.2-100 TeV. This analysis is the first to include allH.E.S.S. data from observations dedicated to MSH 15-52. The corresponding fluxabove 1 TeV is (4.4+/-0.2stat+/-1.0syst) x 10^{-12}cm^{-2}s^{-1}. The energyspectrum obeys a power-law with a differential flux at 1 TeV of(5.8+/-0.2stat+/-1.3syst) x 10^{-12}cm^{-2}s^{-1}TeV^{-1} and a photon index of2.32+/-0.04stat+/-0.10syst. The gamma-ray emission extends along the pulsarjet, previously resolved in X-rays. This becomes more apparent after imagedeconvolution. The emission region along the jet axis decreases with increasingenergy. An upper limit for the pulsed gamma-ray flux from PSR B1509-58 wascalculated. Additional discussions include: the system of MSH 15-52 and PSRB1509-58, theory and methods of VHE gamma-ray astronomy and H.E.S.S., the first(Richardson-Lucy) deconvolution of VHE gamma-ray maps, search for pulsedemission from pulsars. The results are discussed within the framework of PWNsand are explained by inverse Compton scattering of leptons. A hadroniccomponent is not excluded, but its gamma-ray emission would not be significant.Moreover, it is concluded that advection is the dominant transport mechanismover diffusion in the magnetized flow of the pulsar wind from PSR B1509-58. Acorrelation analysis with the Chandra X-ray data suggests that gamma radiationis emitted from the region of PSR B1509-58, but not from the neighboringoptical nebula RCW 89.

Detection of VHE Gamma Radiation from the Pulsar Wind Nebula MSH 15-52 with H.E.S.S