| Issue |
A&A
Volume 436, Number 3, June IV 2005
|
|
|---|---|---|
| Page(s) | 917 - 923 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361:20042367 | |
| Published online | 03 June 2005 | |
The extended hard X-ray emission from the Vela Plerion
1
Istituto di Astrofisica Spaziale e Fisica Cosmica - Sezione di Palermo, IASF-CNR, via Ugo La Malfa 153, 90146 Palermo, Italy e-mail: vanessa@pa.iasf.cnr.it
2
Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, 00185 Roma, Italy
3
INAF-Osservatorio Astronomico di Palermo, Piazza dei Normanni 1, 90100 Palermo, Italy
Received:
15
November
2004
Accepted:
6
February
2005
We present the results of a broad band (3-200 keV)
spectral analysis of BeppoSAX and XMM-Newton observations of
the Vela plerion.
The hard X-ray (>15 keV) emission is found to be extended over a
region of 
radius, corresponding to a size of about
1.0-1.3 pc for a source distance of 290 pc.
A single power law does not give an acceptable fit while
a broken power law or a log-parabolic law nicely fit the data.
The former spectral model has the photon index
for energies lower than the break value equal to
12.5 keV and the index 
up to
about 200 keV. The total X-ray luminosity of the Vela plerion
is 
erg s-1, which implies
a conversion factor of the spin-down power of ~10-3.
Key words: stars: pulsars: general / shock waves / ISM: supernova remnants / ISM: individual object: Vela PWN / X-rays: general
© ESO, 2005
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