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Title:
The extended hard X-ray emission from the Vela Plerion
Authors:
Mangano, V.; Massaro, E.; Bocchino, F.; Mineo, T.; Cusumano, G.
Affiliation:
AA(Istituto di Astrofisica Spaziale e Fisica Cosmica - Sezione di Palermo, IASF-CNR, via Ugo La Malfa 153, 90146 Palermo, Italy ), AB(Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, 00185 Roma, Italy), AC(INAF-Osservatorio Astronomico di Palermo, Piazza dei Normanni 1, 90100 Palermo, Italy), AD(Istituto di Astrofisica Spaziale e Fisica Cosmica - Sezione di Palermo, IASF-CNR, via Ugo La Malfa 153, 90146 Palermo, Italy), AE(Istituto di Astrofisica Spaziale e Fisica Cosmica - Sezione di Palermo, IASF-CNR, via Ugo La Malfa 153, 90146 Palermo, Italy)
Publication:
Astronomy and Astrophysics, Volume 436, Issue 3, June IV 2005, pp.917-923 (A&A Homepage)
Publication Date:
06/2005
Origin:
EDP Sciences
Keywords:
stars: pulsars: general, shock waves, ISM: supernova remnants, ISM: individual object: Vela PWN, X-rays: general
DOI:
10.1051/0004-6361:20042367
Bibliographic Code:
2005A&A...436..917M

Abstract

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 12'-15' 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 Γ1 = 1.66±0.01 for energies lower than the break value equal to 12.5 keV and the index Γ2 = 2.01±0.05 up to about 200 keV. The total X-ray luminosity of the Vela plerion is L_X=5.5×1033 erg s-1, which implies a conversion factor of the spin-down power of ~10-3.
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