Gamma-Ray Burst 980329 and Its X-Ray Afterglow

Zand, J. J. M. in ’t; Amati, L.; Antonelli, L. A.; Butler, R. C.; Castro‐Tirado, Alberto J.; Coletta, Alessandro; Costa, E.; Feroci, M.; Frontera, F.; Heise, J.; Molendi, S.; Nicastro, L.; Owens, A.; Palazzi, E.; Pian, E.; Piro, L.; Pizzichini, G.; Smith, Mike; Tavani, M.

doi:10.1086/311620

Cited by 39 publications

(4 citation statements)

References 30 publications

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“…It has also been shown for several BeppoSAX bursts that the 2-10 keV flux at the end of the GRB phase, on time scale of tens of seconds, is close to that obtained by extrapolating backward in time the X-ray afterglow flux (e.g. Costa et al 1997, In 't Zand 1998. This suggests that the late GRB flux is in fact dominated by afterglow emission, i.e.…”

Section: Electron Energy Fractionsupporting

confidence: 71%

On the Energy of Gamma‐Ray Bursts

Freedman

Waxman

2001

ApJ

193

234

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We show that γ-ray burst (GRB) afterglow observations strongly suggest, within the fireball model framework, that radiating electrons are shock accelerated to a power-law energy distribution, dn e /dγ e ∝ γ −p e , with universal index p ≈ 2.2, and that the fraction of shock energy carried by electrons, ξ e , is universal and close to equipartition, ξ e ∼ 1/3. For universal p and ξ e , a single measurement of the X-ray afterglow flux on the time scale of a day provides a robust estimate of the fireball energy per unit solid angle, ε, averaged over a conical section of the fireball of opening angle θ ∼ 0.1.Applying our analysis to BeppoSAX afterglow data we find that: (i) Fireball energies are in the range of 4πε = 10 51.5 to 10 53.5 erg; (ii) The ratio of observed γ-ray to total fireball energy per unit solid angle, ε γ /ε, is of order unity, satisfying | log 10 (ε γ /ε)| ∼ < 0.5; (iii) If fireballs are jet like, their opening angle should satisfy θ ∼ > 0.1. Our results imply that if typical opening angles are θ ∼ 0.1, a value consistent with our analysis, the total energy associated with a GRB event is in the range of 10 50 erg to 10 51.5 erg.

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Section: Electron Energy Fractionsupporting

confidence: 71%

On the Energy of Gamma‐Ray Bursts

Freedman

Waxman

2001

ApJ

193

234

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“…We performed a spectral analysis of the prompt emission of GRB 990510 in the 70È650 keV band by following approximately the same procedure used for, e.g., GRB 970228 and GRB 980329 (see Frontera et al 1998 ;in Ït Zand et al 1998). The average spectrum of the prompt emission of GRB 990510 can be satisfactorily described (s2 \ 6.84 for 9 degrees of freedom [dof]) by a broken power law, with a break energy keV and E break \ 200^27 power-law indices before and after the break of [1.36^0.16 and [2.34^0.24, respectively.…”

Section: Prompt C-ray Emissionmentioning

confidence: 99%

“…We performed a spectral analysis of the prompt emission of GRB990510 in the 70-650 keV band, by following approximately the same procedure used for, e.g., GRB970228 and GRB980329 (see Frontera et al 1998;In 't Zand et al 1998). The average spectrum of the prompt emission of GRB990510 can be satisfactorily described (χ 2 = 6.84 for 9 d.o.f.)…”

Section: Prompt γ-Ray Emissionmentioning

confidence: 99%

GRB 990510: On the Possibility of a Beamed X‐Ray Afterglow

Kuulkers

Antonelli²,

Kuiper

et al. 2000

ApJ

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We discuss the prompt emission of the c-ray burst GRB 990510 and its subsequent X-ray afterglow from 8.0 to 44.3 hr after the prompt emission, using observations with the Gamma-Ray Burst Monitor and Narrow Field Instruments on BeppoSAX. In the 40È700 keV band, GRB 990510 had a Ñuence of D1.9 ] 10~5 ergs cm~2, whereas it reached a peak Ñux of D2.4 ] 10~6 ergs cm~2 s~1. The X-ray afterglow decay light curve can be satisfactorily described by a single power law with an index of [1.42^0.07. Both the X-ray and optical behavior of the afterglow can be explained by c-ray burst debris expanding as a jet ; we Ðnd that the cooling frequency is (Ðxed) between the optical and X-ray wavelength bands.

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“…Likely the GRB released energy has almost completely ionized the initially absorbing cloud (Lazzati & Perna 2002). In this scheme however we would expect to see the optical counterpart, as in the case of GRB980329 (Palazzi et al 1998), which also showed an initial high absorption (Frontera et al 2000), and even a column density a factor 10 higher than the Galactic one during the afterglow phase (In 't Zand et al 1998). Thus a likely explanation of the GRB010214 darkness could reside in an intrinsic faintness of the related OT and/or the high GRB redshift (centroid value of 4.5) estimated by us.…”

Section: Discussionmentioning

confidence: 91%

The dark burst 010214 withBeppoSAX: Possible variable absorption and jet X–ray emission

Guidorzi

Frontera

Montanari

et al. 2003

A&A

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Abstract. We report on the prompt and afterglow emission observations of the dark burst GRB010214 with BeppoSAX. The prompt emission shows possible evidence of variable absorption from N H = 3.0 +5.1 −2.0 × 10 23 cm −2 in the first 6 s of the event to a value consistent with the Galactic column density (N G H = 2.66 × 10 20 cm −2 ) in the GRB direction. An X-ray afterglow emission in the 2-10 keV energy band was detected with BeppoSAX, but an analogue search at lower wavelengths (optical, IR and radio) was unsuccessful. The X-ray afterglow spectrum is consistent with a power-law with Galactic absorption. The light curve shows a complex decay, if the tail of the prompt emission is assumed as the onset of the afterglow: if the origin of the afterglow is coincident with the GRB onset, a bump before ∼3 × 10 4 s is inferred, while if the afterglow is assumed to start later, a steepening of the power-law light curve at t ∼ 3 × 10 4 s is deduced. We discuss these results in the light of the current models of afterglows and the possible origin of the GRB darkness. Finally, we tentatively derive an estimate of the burst redshift.

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Gamma-Ray Burst 980329 and Its X-Ray Afterglow

Abstract: GRB 980329 is the brightest gamma-ray burst detected so far with the Wide Field Cameras aboard BeppoSAX, both in gamma-rays and X-rays. With

Cited by 39 publications

References 30 publications

On the Energy of Gamma‐Ray Bursts

On the Energy of Gamma‐Ray Bursts

GRB 990510: On the Possibility of a Beamed X‐Ray Afterglow

The dark burst 010214 withBeppoSAX: Possible variable absorption and jet X–ray emission

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