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Title: INTEGRAL and XMM-Newton observations of the weak gamma-ray burst GRB 030227
Type: Journal articleJournal article
Participant(s):
Forfatter:  Mereghetti, S.
Technical University of Denmark

Forfatter:  Gotz, D.
Technical University of Denmark

Forfatter:  Tiengo, A.
Technical University of Denmark

Forfatter:  Beckmann, V.
Technical University of Denmark

Forfatter:  Borkowski, J.
Technical University of Denmark

Forfatter:  Courvoisier, T.J.L.
Technical University of Denmark

Forfatter:  von Kienlin, A.
Technical University of Denmark

Forfatter:  Schoenfelder, V.
Technical University of Denmark

Forfatter:  Roques, J.P.
Technical University of Denmark

Forfatter:  Bouchet, L.
Technical University of Denmark

Forfatter:  Ubertini, P.
Technical University of Denmark

Forfatter:  Castro-Tirado, A.
Technical University of Denmark

Forfatter:  Lebrun, F.
Technical University of Denmark

Author:  Paul, Joachim (Cwisno: 9319)
Technical University of Denmark

Author:  Lund, Niels (Cwisno: 38305)
Technical University of Denmark
Email:

Forfatter:  Mas-Hesse, J.M.
Technical University of Denmark

Forfatter:  Hermsen, W.
Technical University of Denmark

Forfatter:  den Hartog, P.R.
Technical University of Denmark

Forfatter:  Winkler, C.
Technical University of Denmark
Abstract: We present International Gamma-Ray Astrophysical Laboratory ( INTEGRAL) and XMM-Newton observations of the prompt gamma-ray emission and the X-ray afterglow of GRB 030227, the first gamma-ray burst for which the quick localization obtained with the INTEGRAL Burst Alert System has led to the discovery of X-ray and optical afterglows. GRB 030227 had a duration of about 20 s and a peak flux of similar to1.1 photons cm(-2) s(-1) in the 20-200 keV energy range. The time-averaged spectrum can be fitted by a single power law with photon index similar to2, and we find some evidence for a hard-to-soft spectral evolution. The X-ray afterglow has been detected starting only 8 hr after the prompt emission, with a 0.2-10 keV flux decreasing as t(-1) from 1.3 x 10(-12) to 5 x 10(-13) ergs cm(-2) s(-1). The afterglow spectrum is well described by a power law with photon index modified by a 1.94 +/- 0.05 redshifted neutral absorber with column density of several 10(22) cm(-2). A possible emission line at 1.67 keV could be due to Fe for a redshift z similar to 3, consistent with the value inferred from the absorption.
Published: in journal: Astrophysical Journal (ISSN: 0004-637X), vol: 590, issue: 2, pages: L73-L77, 2003
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