Discovery of an X-ray afterglow associated with the γ-ray burst of 28 February 1997

Costa, E.; Frontera, F.; Heise, J.; Feroci, M.; Zand, J. in ’t; Fiore, F.; Cinti, M.N.; Fiume, D. Dal; Nicastro, L.; Orlandini, M.; Palazzi, E.; Rapisarda, M.; Zavattini, G.; Jäger, R.; Parmar, A. N.; Owens, A.; Molendi, S.; Cusumano, G.; Maccarone, M. C.; Giarrusso, S.; Coletta, Alessandro; Antonelli, L. A.; Giommi, P.; Müller, J.; Piro, L.; Butler, R. C.

doi:10.1038/42885

Cited by 973 publications

(642 citation statements)

References 14 publications

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“…In many such cases afterglow emission was detected, the host galaxies were discovered, and the associated measurement of spectral line redshifts confirmed the cosmological distances to the burst sources (e.g., Costa et al 1997;Piro et al 1998;van Paradijs et al 1997;Bremer et al 1998;Frail et al 1997). Observational evidence also indicates that the bursts originate from star formation regions, suggesting a possible link to massive star explosions.…”

Section: Introductionmentioning

confidence: 71%

Relativistic outflows from remnants of compact object mergers and their viability for short gamma-ray bursts

Aloy¹,

Janka²,

Müeller³

2005

A&A

254

295

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Abstract. We present the first general relativistic hydrodynamic models of the launch and evolution of relativistic jets and winds, driven by thermal energy deposition, possibly due to neutrino-antineutrino annihilation, in the close vicinity of black hole-accretion torus systems. The latter are considered to be the remnants of compact object mergers. Our two-dimensional simulations establish the link between models of such mergers and future observations of short gamma-ray bursts by the SWIFT satellite. They show that ultrarelativistic outflow with maximum terminal Lorentz factors around 1000 develops for polar energy deposition rates above some 10 48 erg s −1 per steradian, provided the merger environment has a sufficiently low baryon density. By the interaction with the dense accretion torus the ultrarelativistic outflow with Lorentz factors Γ above 100 is collimated into a sharp-edged cone that is embedded laterally by a wind with steeply declining Lorentz factor. The typical semi-opening angles of the Γ > 100 cone are 5 • −10 • , corresponding to about 0.4−1.5% of the hemisphere and apparent isotropized energies (kinetic plus internal) up to ≈10 51 erg although at most 10−30% of the deposited energy is transferred to the outflow with Γ > 100. The viability of post-merger black hole-torus systems as engines of short, hard gamma-ray bursts is therefore confirmed. The annihilation of neutrino-antineutrino pairs radiated from the hot accretion torus appears as a suitable energy source for powerful axial outflow even if only ≈10 49 erg are deposited within a cone of 45 • half-opening angle around the system axis. Although the torus lifetimes are expected to be only between some 0.01 s and several 0.1 s, our models can explain the durations of all observed short gamma-ray bursts, because different propagation velocities of the front and rear ends will lead to a radial stretching of the ultrarelativistic fireball before transparency is reached. The ultrarelativistic flow reveals a highly non-uniform structure caused by the action of Kelvin-Helmholtz instabilities that originate at the fireball-torus interface. Large radial variations of the baryon density (up to several orders of magnitude) are uncorrelated with moderate variations of the Lorentz factor (factors of a few) and fluctuations of the gently declining radiation-dominated pressure. In the angular direction the Lorentz factor reveals a nearly flat plateau-like maximum with values of several hundreds, that can be located up to 7 • off the symmetry axis, and a steep decrease to less than 10 for polar angles larger than 15 • −20 • . Lateral expansion of the ultrarelativistic core of the flow is prevented by a subsonic velocity component of about 0.05c towards the symmetry axis, whereas the moderately relativistic wings show a subsonic sideways inflation with less than 0.07c (measured in the frame comoving with the radial flow).

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Section: Introductionmentioning

confidence: 71%

Relativistic outflows from remnants of compact object mergers and their viability for short gamma-ray bursts

Aloy¹,

Janka²,

Müeller³

2005

A&A

254

295

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“…Among the most important results obtained with the WFCs is the discovery of the X-ray afterglow phenomenon of Gamma Ray Bursts in 1997 (Costa et al 1997). Moreover, the 12 monitoring campaigns of the Galactic Bulge allowed the spectral and timing monitoring of known persistent and transient X-ray sources and the discovery of many new galactic X-ray transients and phenomena (see for example Ubertini et al 1999;Cornelisse et al 2000;in 't Zand 2001in 't Zand , 2004aCornelisse et al 2003).…”

Section: Introductionmentioning

confidence: 99%

TheBeppoSAX WFC X-ray source catalogue

Verrecchia

Zand

Giommi

et al. 2007

A&A

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Aims. We present the catalogue of X-ray sources detected by the two Wide Field Cameras (WFCs) in complete observations on board BeppoSAX during its 6 years of operational lifetime, between April 1996 and April 2002. Methods. The BeppoSAX WFCs were coded mask instruments sensitive in the 2-28 keV energy band with a 40 × 40 square degree fields of view, pointing in opposite directions and perpendicularly to the BeppoSAX Narrow Field Instruments (NFI). The WFCs were usually operated simultaneously to NFI observations, each lasting up to several days. WFCs observed thus the entire sky several times with a typical sensitivity of 2 to 10 mCrab. A systematic analysis of all WFC observations in the BeppoSAX archive has been carried out using the latest post-mission release of the WFC analysis software and calibrations. Results. The catalogue includes 253 distinct sources, obtained from a total sample of 8283 WFC detections. We describe the basic statistical properties of the sample and present a six-year history of two celestial calibration X-ray sources.

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“…They were discovered in 1967 (see Bonnell & Klebesadel 1996 for a discussion of the first GRB detections), but due to the lack of rapid and precise localisations, their emission at other wavelengths was not detected until 1997 (van Paradijs et al 1997;Frail et al 1997;Costa et al 1997). Thus, for 30 years they were not localised at longer wavelengths (X-ray, UV, optical, IR, radio) and their distances could not be measured.…”

Section: Introductionmentioning

confidence: 99%

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Gorosabel¹,

Fynbo²,

Hjorth

et al. 2002

A&A

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Abstract.We report the discovery of the optical and near-infrared counterparts to GRB 001011. The GRB 001011 error box determined by Beppo-SAX was simultaneously imaged in the near-infrared by the 3.58-m New Technology Telescope and in the optical by the 1.54-m Danish Telescope ∼8 hr after the gamma-ray event. Here we implement the colour-colour discrimination technique proposed by Rhoads (2001) and extend it using near-IR data as well. We present the results provided by an automatic colour-colour discrimination pipe-line developed to discern the different populations of objects present in the GRB 001011 error box. Our software revealed three candidates based on single-epoch images. Second-epoch observations carried out ∼3.2 days after the burst revealed that the most likely candidate had faded, thus identifying it with the counterpart to the GRB. In deep R-band images obtained 7 months after the burst a faint (R = 25.38 ± 0.25) elongated object, presumably the host galaxy of GRB 001011, was detected at the position of the afterglow. The GRB 001011 afterglow is the first discovered with the assistance of colour-colour diagram techniques. We discuss the advantages of using this method and its application to error boxes determined by future missions.

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Discovery of an X-ray afterglow associated with the γ-ray burst of 28 February 1997

Cited by 973 publications

References 14 publications

Relativistic outflows from remnants of compact object mergers and their viability for short gamma-ray bursts

Relativistic outflows from remnants of compact object mergers and their viability for short gamma-ray bursts

TheBeppoSAX WFC X-ray source catalogue

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

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