Observation of X-ray Lines from a Gamma-Ray Burst (GRB991216): Evidence of Moving Ejecta from the Progenitor

Piro, L.; Garmire, G. P.; Garcia, M. R.; Stratta, G.; Costa, E.; Feroci, M.; Mészáros, P.; Vietri, M.; Bradt, H.; Frail, D. A.; Frontera, F.; Halpern, J. P.; Heise, J.; Hurley, K.; Kawai, N.; Kippen, R. M.; Marshall, F. E.; Murakami, T.; Соколов, В. В.; Takeshima, T.; Yoshida, A.

doi:10.1126/science.290.5493.955

Cited by 245 publications

(326 citation statements)

References 18 publications

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“…Due to their large Doppler shift δ, the hydrogen emission lines (and the emission lines from the swept up ISM and supernova shell material) as well as the CB's thermal bremsstrahlung, are shifted to the observer's X-ray band. They contribute significantly to the X-ray afterglow and may provide a simple alternative explanation (Dar & De Rújula 2000) to the commonly assumed Fe-line origin of the X-ray lines observed in the afterglows of GRB 970508: Piro et al (1998), GRB 970828: Yoshida et al (1999;2001), GRB 991216: Piro et al (2000) and GRB 000214: Antonelli et al (2000).…”

Section: Discussionmentioning

confidence: 99%

On the radio afterglow of gamma ray bursts

Dado

Dar

Rújula

2003

A&A

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Abstract. We use the cannonball (CB) model of gamma ray bursts (GRBs) to predict the spectral and temporal behaviour of their radio afterglows (AGs). A single simple expression describes the AGs at all times and frequencies; its high-frequency limit reproduces the successful CB model predictions for optical and X-ray AGs. We analyze all of the observed radio AGs of GRBs with known redshifts, including those of the exceptionally close-by GRB 980425. We also study in detail the timeevolution of the AGs' spectral index. The agreement between theory and observations is excellent, even though the CB model is extremely frugal in the number of parameters required to explain the radio observations. We propose to use the scintillations in the radio AGs of GRBs to verify and measure the hyperluminal speed of their jetted CBs, whose apparent angular velocity is of the same order of magnitude as that of galactic pulsars, consistently measured directly, or via scintillations.

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Section: Discussionmentioning

confidence: 99%

On the radio afterglow of gamma ray bursts

Dado

Dar

Rújula

2003

A&A

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“…The presence of X-ray lines would require a significant amount of matter on stellar scales (e.g., Piro et al 2000), as may be expected in models involving the death of massive stars. However, to date, these detections (e.g., Piro et al 2000;Reeves et al 2002) have not been made with high significance.…”

Section: Introductionmentioning

confidence: 99%

“…On smaller spatial scales, there is growing evidence tying GRBs to regions of high ambient density (Galama & Wijers 2001;Harrison et al 2001), and at least some of the so-called dark GRBs arise in or behind regions of high extinction (Djorgovski et al 2001a;Piro et al 2002).…”

Section: Introductionmentioning

confidence: 99%

GRB 010921: Strong Limits on an Underlying Supernova from theHubble Space Telescope

Price

Kulkarni

Schmidt

et al. 2003

ApJ

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GRB 010921 was the first HETE-2 gamma-ray burst (GRB) to be localized via its afterglow emission. The low redshift of the host galaxy, z ¼ 0:451, prompted us to undertake intensive multicolor observations with the Hubble Space Telescope with the goal of searching for an underlying supernova (SN) component. We do not detect any coincident SN to a limit 1.33 mag fainter than SN 1998bw at 99.7% confidence, making this one of the most sensitive searches for an underlying SN. Analysis of the afterglow data allows us to infer that the GRB was situated behind a net extinction (Milky Way and the host galaxy) of A V $ 1:8 mag in the observer frame. Thus, had it not been for such heavy extinction, our data would have allowed us to probe for an underlying SN with brightness approaching those of more typical Type Ib/c SNe.

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“…INTRODUCTION The detection of spectral signatures associated with the environment of a g-ray burst (GRB) would provide important clues about the triggering mechanism and the progenitor (Mészáros & Rees 1998;Lazzati, Campana, & Ghisellini 1999;Böttcher 2000). Observations with Chandra, ASCA, and BeppoSAX have provided tentative evidence for Fe Ka line and edge features in at least five bursts; GRB 970508 (Piro et al 1999), GRB 970828 (Yoshida et al 1999), GRB 991216 (Piro et al 2000), and GRB 000214 (Antonelli et al 2000) all show an emission feature during the X-ray afterglow a few hours to a day after the burst event, while GRB 990705 (Amati et al 2000) displays a prominent X-ray absorption feature during the burst itself. Although most of the line detections are only marginally significant and fail to distinguish between the various line excitation mechanisms, 1 GRB 991216 shows a keV line at a mod-3.49 ‫ע‬ 0.06 erate confidence level (∼4 j).…”

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confidence: 99%

Iron Kα Emission from X-Ray Reflection: Predictions for Gamma-Ray Burst Models

Ballantyne¹,

Ramírez-Ruiz²

2001

The Astrophysical Journal

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Recent observations of several g-ray burst (GRB) afterglows have shown evidence for a large amount of X-ray line-emitting material, possibly arising from ionized iron. A significant detection of an X-ray spectral feature, such as that found in the Chandra observation of GRB 991216, may provide important constraints on the immediate environment of the burst and hence on progenitor models. The large Fe Ka equivalent widths inferred from the X-ray observations favor models in which the line is produced when the primary X-ray emission from the source strikes Thomson-thick material and Compton scatters into our line of sight. We present such reflection spectra here, computed in a fully self-consistent manner, and discuss the range of ionization parameters that may be relevant to different models of GRBs. We argue that the presence of a strong hydrogen-like Ka line is unlikely, because Fe xxvi photons would be trapped resonantly and removed from the line core by Compton scattering. In contrast, a strong narrow emission line from He-like Fe xxv is prominent in the model spectra. We briefly discuss how these constraints may affect the line energy determination in GRB 991216.

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Observation of X-ray Lines from a Gamma-Ray Burst (GRB991216): Evidence of Moving Ejecta from the Progenitor

Cited by 245 publications

References 18 publications

On the radio afterglow of gamma ray bursts

On the radio afterglow of gamma ray bursts

GRB 010921: Strong Limits on an Underlying Supernova from theHubble Space Telescope

Iron Kα Emission from X-Ray Reflection: Predictions for Gamma-Ray Burst Models

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