Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20915620l&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #156.20; Bulletin of the American Astronomical Society,
Astronomy and Astrophysics
Astronomy
Scientific paper
The Vela supernova remnant (SNR), at a distance of 290 pc is the closest SNR to contain an active pulsar, (PSR) B0833-45. The SNR spans about 8 degrees in diameter and contains regions of nonthermal emission, including Vela X to the south-southwest of the pulsar, thought to be a pulsar-powered wind nebula (PWN). The center of Vela X is offset by about 40' from the pulsar and emits in the radio, X-ray, and gamma ray bands.
ROSAT observations of the Vela SNR reveal a collimated X-ray filament seen predominantly at higher energies extending from the pulsar to the center of Vela X, about 45' in length. This cocoon-like feature was interpreted by Markwardt and Ogelman as an X-ray jet along which the pulsar loses energy. Subsequent Chandra observations show that the pulsar jet actually lies along the northwest-southeast direction, roughly aligned with the pulsar proper motion, leaving unanswered the nature of the extended ROSAT structure.
We investigate the properties of this cocoon-like filament using archival XMM-Newton data. We find that the spectrum is best-fit by a two-component model: an absorbed non-equilibrium plasma model with a power-law component to accommodate the hard emission. We model the synchrotron radiation responsible for the radio and X-ray emission and fit an inverse compton model to the gamma ray emission. We also investigate the thermal emission, which shows evidence for ejecta that may be have been mixed into the PWN during disruption from the reverse shock of the SNR.
de Jager O.
LaMassa Stephanie M.
Slane Pat
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