Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006rmxac..26..202d&link_type=abstract
XI IAU Regional Latin American Meeting of Astronomy (Eds. L. Infante & M. Rubio) Revista Mexicana de Astronomía y Astrofísica (S
Astronomy and Astrophysics
Astronomy
Scientific paper
Radio composite supernova remnants (SNRs) consist of a shell and a spectrally distinct inner nebula, presumably a pulsar wind nebula (PWN), powered by the wind of relativistic electron/positron pairs from a central pulsar. The SNR G0.9+0.1 is a composite SNR characterized by a bright, centrally condensed synchrotron nebula and a weak surrounding radio shell. The central core was detected in X-rays using BeppoSAX (Mereghetti et al. 1998, AA, 331, L77) and later studied with the Chandra (Gaensler et al. 2001, ApJ, 556, L107) and XMM-Newton telescopes (Porquet et al. 2003, AA, 401, 197).
The Chandra observations revealed the presence of the point-like source CXOU J174722.8-280915, candidate to be the central powering pulsar. This SNR has also been detected with the HESS instrument at energies greater than 100 GeV (Aharonian et al. 2005, AA, 432, L25). The very high energy gamma-rays appear to originate in the PWN.
In this work we present new high-resolution radio data of the SNR G0.9+0.1 showing for the first time a detailed multiwavelength comparison of the central nebula and a spectral study of the complete SNR.
Decourchelle Anne
Dubner Gloria M.
Giacani Elsa
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