Revisiting the Southern Vela "Jet"

Details Revisiting the Southern Vela "Jet" Revisiting the Southern Vela "Jet"

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.0303l&link_type=abstract

American Astronomical Society Meeting 208, #3.03; Bulletin of the American Astronomical Society, Vol. 38, p.81

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The Vela supernova remanant (SNR) has been extensively studied in X-rays. ROSAT observations revealed a filamentary X-ray structure about 45' in length, south-southwest of the Vela pulsar. Markwardt and Ogelman (1997) interpreted this feature as a jet along which the Vela pulsar loses mechanical energy. Gvaramadze (1999) later interpreted this feature as a dense filament in the SNR shell, connected to the projection effects of the Rayleigh-Taylor unstable shell, and unrelated to the pulsar itself. Subsequent Chandra observations show that the pulsar does indeed have a jet, but that it is actually oriented along a northwest-southeast axis, roughly along the proper motion vector of the pulsar, and not in the direction of the extended ROSAT structure. However, recent H.E.S.S. observations have revealed TeV gamma-ray emission emanating from this region, indicating the presence of some mechanism by which particles are accelerated to extremely high energies.Using archival XMM observations, we have investigated the X-ray spectrum of the extreme southern edge of this feature. Consistent with previous ASCA results, we find that a two-component spectrum is required. The hard component is best described by a power law, and the accompanying thermal emission from this region appears to have abundances of several species that are enhanced above the values found for the bulk of the Vela SNR. Here we summarize the spectral results and investigate the energetics of the nonthermal component in the context of the TeV emission from this region of Vela.

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