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Astron. Astrophys. 361, 719-724 (2000)

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X-ray emission from the galactic center region supernova remnant G0.9+0.1

L. Sidoli 1, S. Mereghetti 2, G.L. Israel *  3 and F. Bocchino 1

1 Astrophysics Division, Space Science Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands
2 Istituto di Fisica Cosmica G.Occhialini, C.N.R., Via Bassini 15, 20133 Milano, Italy
3 Osservatorio Astronomico di Roma, Via Frascati 23, 00040 Monteporzio Catone (Roma), Italy

Received 14 June 2000 / Accepted 13 July 2000

Abstract

We report the results of a BeppoSAX observation of the composite supernova remnant G0.9+0.1, located in the Galactic Center region. This new observation, in which the core of G0.9+0.1 is observed on-axis, confirms our previous results obtained from a pointing in which the supernova remnant was serendipitously observed at a large off-axis angle. The better quality of the new data allows us to confirm the non-thermal nature of the X-ray source coincident with the central plerion, to significantly improve the estimate of its spectral parameters, to put more stringent upper limits on the presence of coherent pulsations (in the range of periods from 4 ms to [FORMULA]4[FORMULA]104 s), to obtain marginal evidence of the possible extended nature of the X-ray plerion and to put a better upper limit on the 2-10 keV X-ray emission from the 8´ diameter radio shell ([FORMULA] erg s-1). The X-ray spectrum is best fit with a power-law model with a photon index [FORMULA] 2, [FORMULA]  cm-2 and a 2-10 keV luminosity of [FORMULA] erg s-1. The broad band (radio-X-ray) properties of the composite supernova remnant G0.9+0.1 are indicative of the likely presence of a young ([FORMULA]2,700 yr) neutron star in its central radio core.

Key words: ISM: supernova remnants – ISM: individual objects: G0.9+0.1 – X-rays: ISM

* Affiliated to I.C.R.A.

Send offprint requests to: L. Sidoli (lsidoli@astro.estec.esa.nl)

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© European Southern Observatory (ESO) 2000

Online publication: October 2, 2000
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