3-11 July 2007
Merida, Mexico
Mexico/General timezone
- icrc2007@icrc2007.unam.mx
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Contribution Poster
Merida, Mexico
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Regency (Hyatt)
OG.2.2
A Search for energy dependent morphology from the cocoon of Vela X with H.E.S.S.
Speakers
- Dr. Bruno KHELIFI
Primary authors
- Dr. Bruno KHELIFI (LLR, Ecole Polytechnique)
- Dr. Conor MASTERSON (Dublin Institute for Advanced Studies)
Co-authors
- Dr. Okkie DE JAGER (North West University, RSA)
- Dr. Bruno KHELIFI (LLR, Ecole Polytechnique)
Abstract content
The Vela Supernova remnant is a large, nearby remnant with a complex morphology, containing a bright pulsar at its centre. This pulsar has an associated pulsar wind nebula (PWN), gamma-ray emission from which was detected by the H.E.S.S. collaboration at very high energies. As the Vela remnant is the closest known PWN to us, detailed study of the spectral and morphological characteristics of the emission associated with the PWN can shed considerable light on the acceleration of particles to very high energies in this category of object. This question will be addressed here in the context of H.E.S.S. observations of the Vela region.
If this papers is presented for a collaboration, please specify the collaboration
H.E.S.S. collaboration