The Prompt X‐Ray Emission of GRB 011211: Possible Evidence of a Transient Absorption Feature | Zendy

F. Frontera | Zendy; L. Amati | Zendy; J. J. M. in ’t Zand | Zendy; Davide Lazzati | Zendy; Arieh Königl | Zendy; M. Vietri | Zendy; E. Costa | Zendy; M. Feroci | Zendy; C. Guidorzi | Zendy; E. Montanari | Zendy; M. Orlandini | Zendy; E. Pian | Zendy; L. Piro | Zendy

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The Prompt X‐Ray Emission of GRB 011211: Possible Evidence of a Transient Absorption Feature

Author(s) -

F. Frontera,

L. Amati,

J. J. M. in ’t Zand,

Davide Lazzati,

Arieh Königl,

M. Vietri,

E. Costa,

M. Feroci,

C. Guidorzi,

E. Montanari,

M. Orlandini,

E. Pian,

L. Piro

Publication year - 2004

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/425066

Subject(s) - afterglow , gamma ray burst , astrophysics , physics , redshift , event (particle physics) , transient (computer programming) , absorption (acoustics) , feature (linguistics) , emission spectrum , gaussian , astronomy , spectral line , optics , quantum mechanics , linguistics , philosophy , galaxy , computer science , operating system

We report on observation results of the prompt X- and gamma-ray emission fromGRB011211. This event was detected with the Gamma-Ray Burst Monitor and one ofthe Wide Field Cameras aboard the BeppoSAX satellite. The optical counterpartto the GRB was soon identified and its redshift determined (z = 2.140), whilewith the XMM-Newton satellite, the X-ray afterglow emission was detected.Evidence of soft X-ray emission lines was reported by Reeves et al. (2002), butnot confirmed by other authors. In investigating the spectral evolution of theprompt emission we find the possible evidence of a transient absorption featureat 6.9^{+0.6}_{-0.5} keV during the rise of the primary event. The significanceof the feature is derived with non parametric tests and numerical simulations,finding a chance probability which ranges from 3x10^{-3} down to 4x10^{-4}. Thefeature shows a Gaussian profile and an equivalent width of 1.2^{+0.5}_{-0.6}keV. We discuss our results and their possible interpretation.Comment: 23 pages, 3 Tables, 6 Figures. Accepted for publication in Astrophysical Journa

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