Discovery of a Redshifted Iron K Line in the X-Ray Afterglow of GRB 000214

By L. Antonelli, L. Piro, M. Vietri, E. Costa, P. Soffitta, M. Feroci, L. Amati, F. Frontera, E. Pian, J. I. Zand and 6 more. 2000

132 citations recorded by the source corpus.

We report the detection (3 σ significance level) of a strong iron emission line in the X-ray spectrum of the afterglow of GRB 000214 ("Valentine's Day Burst") observed by BeppoSAX. An emission-line feature was observed with a centroid energy of 4.7 ± 0.2 keV, which, if interpreted as Kα emission from hydrogen-like iron, corresponds to a redshift of z = 0.47. The intensity (EW ~ 2 keV) and duration (tens of hours) of the line give information on the distance, from the burst region, of the emitting material (R ≥ 3 × 1015 cm) and its mass (M ≥ 1.4 M☉). These results are not easily reconciled with the binary merger and hypernova models for gamma-ray bursts because they require large amounts of mass (about 1 M☉) at large distances (≈1016 cm) and at Newtonian speeds.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/bc1cbc5719d20f076a9b942673b918177bf57c7a

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In Astronomy and Astrophysics

1. Bing Zhang
2. P. Mészáros
3. Pawan Kumar
4. E. Liang
5. E. Ramirez-Ruiz
6. P. O’Brien
7. B. Metzger
8. L. Amati

Citations in the corpus

• Gamma-Ray Bursts from Delayed Collapse of Neutron Stars to Quark Matter Stars (2002, background): “…I-10129 Torino, Italy the evidence of emission features in the afterglow of several GRBs (Piro et al. 1999; Yoshida et al. 1999; Piro et al. 2000; Antonelli et al. 2000; Reeves et al. 2002) have stimulated the interpretation of these characteristics in the context of the fireball model of…”
• Quark Deconfinement and Implications for the Radius and the Limiting Mass of Compact Stars (2004, background): “…are giving mounting evidence that ‘‘long-duration’’ gamma-ray bursts (GRBs) are associated with supernova explosions (Bloom et al. 1999; Amati et al. 2000; Antonelli et al. 2000; Piro et al. 2000; Reeves et al. 2002; Hjorth et al. 2003; Price et al. 2003; Stanek et al. 2003; Lipkin et al. 2004).”
• The afterglow of GRB 021004: surfing on density waves (2002, background): “This possibility was also suggested to account for the possible detections of X-ray lines (Piro et al. 1999, 2000; Antonelli et al. 2000; Reeves et al. 2002) in the early XA of several GRBs.”
• A RADIO-SELECTED SAMPLE OF GAMMA-RAY BURST AFTERGLOWS (2011, unknown): “Abbreviations for the references are as follows: (1) Aleksić et al. 2010; (2) Chandra et al. 2010; (3) Amati 2006; (4) Antonelli et al. 2000; (5) Berger et al. 2005b; (6) Berger et al. 2007; (7) Bloom et al. 2001; (8) Butler et al. 2007; (9) Cardone et al. 2009; (10) Cenko et al. 2006; (11)…”
• Cosmological Aspects of Gamma-Ray Bursts: Luminosity Evolution and an Estimate of the Star Formation Rate at High Redshifts (2001, background): “…of some afterglows (Bloom et al. 1999; Reichart 1999), and direct iron line observations in the X-ray afterglows of a few GRBs (Piro et al. 2000; Antonelli et al. 2000).10 Theoretically, massive star progenitors have proved to be viable models, particularly for the longer duration bursts…”
• Gamma-Ray Bursts in the Swift Era (2009, unknown): “These included BeppoSAX observations of GRB 970508 (Piro et al. 1999) and GRB 000214 (Antonelli et al. 2000), ASCA observations of GRB 970828 (Yoshida et al. 1999), Chandra observations of GRB 991216 (Piro et al. 2000) and XMM observations of GRB 011211 (Reeves et al. 2002).”
• A Systematic Analysis of Supernova Light in Gamma-Ray Burst Afterglows (2003, background): “Furthermore, for several GRB afterglows X-ray data suggest a period of nucleosynthesis preceding or accompanying the burst (e.g., Antonelli et al. 2000; Lazzati et al. 1999; Mészáros & Rees 2001).”
• The signature of supernova ejecta in the X-ray afterglow of the γ-ray burst 011211 (2002, result): “Our result contrasts with the large masses of iron implied by the iron lines reported in the X-ray spectra of several other afterglow”
• Gamma-Ray Burst Afterglow with Continuous Energy Injection: Signature of a Highly Magnetized Millisecond Pulsar (2000, background): “…the recent detection of Fe features in the X-ray afterglow of GRB 991216 after about 1.5 days (Piro et al. 2000) and GRB 000214 after about 1 day (Antonelli et al, 2000), which may require a continuing post-burst outflow in order to achieve less restrictive Fe abundance constraints (Rees &…”