INTEGRAL and XMM-Newton Observations of the Weak Gamma-Ray Burst GRB 030227 (Articolo in rivista)

Type
Label
  • INTEGRAL and XMM-Newton Observations of the Weak Gamma-Ray Burst GRB 030227 (Articolo in rivista) (literal)
Anno
  • 2003-01-01T00:00:00+01:00 (literal)
Alternative label
  • Mereghetti, S.; Götz, D.; Tiengo, A.; Beckmann, V.; Borkowski, J.; Courvoisier, T. J.-L.; von Kienlin, A.; Schoenfelder, V.; Roques, J. P.; Bouchet, L.; Ubertini, et al. (2003)
    INTEGRAL and XMM-Newton Observations of the Weak Gamma-Ray Burst GRB 030227
    (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#autori
  • Mereghetti, S.; Götz, D.; Tiengo, A.; Beckmann, V.; Borkowski, J.; Courvoisier, T. J.-L.; von Kienlin, A.; Schoenfelder, V.; Roques, J. P.; Bouchet, L.; Ubertini, et al. (literal)
Pagina inizio
  • L73 (literal)
Pagina fine
  • L77 (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#numeroVolume
  • 590 (literal)
Note
  • ISI Web of Science (WOS) (literal)
Titolo
  • INTEGRAL and XMM-Newton Observations of the Weak Gamma-Ray Burst GRB 030227 (literal)
Abstract
  • We present International Gamma-Ray Astrophysical Laboratory (INTEGRAL) and XMM-Newton observations of the prompt γ-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 ~1.1 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 ~2, 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 1.3×10-12 to 5×10-13 ergs cm-2 s-1. The afterglow spectrum is well described by a power law with photon index 1.94+/-0.05 modified by a redshifted neutral absorber with column density of several 1022 cm-2. A possible emission line at 1.67 keV could be due to Fe for a redshift z~3, consistent with the value inferred from the absorption. (literal)
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