Volume 409, Number 3, October III 2003
|Page(s)||983 - 987|
|Section||Stellar structure and evolution|
|Published online||17 November 2003|
The X-ray afterglow of GRB 030329
Istituto di Astrofisica Spaziale e Fisica Cosmica – CNR, Sezione di Milano “G.Occhialini”, Via Bassini 15, 20133 Milano, Italy
2 Università degli Studi di Milano, Dipartimento di Fisica, v. Celoria 16, 20133 Milano, Italy
3 INAF-Osservatorio Astronomico di Brera, v. Bianchi 46, 23907 Merate (LC), Italy
4 Institute of Astronomy, Madingley Road, Cambridge CB3 OHA, UK
5 XMM-Newton Science Operation Center, ESA, Vilspa, Apartado 50727, 28080 Madrid, Spain
Corresponding author: A. Tiengo, email@example.com
Accepted: 23 July 2003
We report on XMM-Newton and Rossi-XTE observations of the bright (fluence ~10-4 erg cm-2) and nearby () Gamma-Ray Burst GRB 030329 associated to SN2003dh. The first Rossi-XTE observation, 5 hours after the burst, shows a flux decreasing with time as a power law with index . Such a decay law is only marginally consistent with a further Rossi-XTE measurement (at hr). Late time observations of this bright afterglow at X-ray wavelengths have the advantage, compared to optical observations, of not being affected by contributions from the supernova and host galaxy. A first XMM-Newton observation, at days, shows a flux of erg cm-2 s-1 (0.2–10 keV). The spectrum is a power law with photon index and absorption < cm-2, consistent with the Galactic value. A further XMM-Newton pointing at days shows a flux fainter by a factor ~2. The combined Rossi-XTE and XMM-Newton measurements require a break at days in the afterglow decay, with a power law index increasing from 0.9 to 1.9, similar to what is observed in the early part of the optical afterglow. The extrapolation of the XMM-Newton spectra to optical frequencies lies a factor of ~10 below simultaneous measurements. This is likely due to the presence of SN2003dh.
Key words: gamma rays: bursts
© ESO, 2003
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