Prompt and Delayed Emission Properties of Gamma‐Ray Bursts Observed with
                    <i>BeppoSAX</i>

Frontera, F.; Amati, L.; Costa, E.; Müller, J.; Pian, E.; Piro, L.; Soffitta, P.; Tavani, M.; Castro-Tirado, A. J.; Fiume, D. Dal; Feroci, M.; Heise, J.; Masetti, N.; Nicastro, L.; Orlandini, M.; Palazzi, E.; Sari, Re’em

doi:10.1086/313316

Cited by 190 publications

(196 citation statements)

References 53 publications

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“…Frontera et al (2000) report that the X-ray afterglow starts at about 50% of the GRB duration and its fluence, as computed from the WFC light curve, is consistent with the decay law found from the afterglow NFI observations. In our case the extrapolation of the X-ray afterglow is well below the γ-ray flux and extrapolates to a time earlier than the GRB.…”

Section: The Prompt Eventsupporting

confidence: 86%

The weakINTEGRALbursts GRB 040223 and GRB 040624: an emerging population of dark afterglows

Filliatre¹,

Covino

D’Avanzo

et al. 2006

A&A

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We report here γ-ray, X-ray and near-infrared observations of GRB 040223 along with γ-ray and optical observations of GRB 040624. GRB 040223 was detected by INTEGRAL close to the Galactic plane and GRB 040624 at high Galactic latitude. Analyses of the prompt emission detected by the IBIS instrument on INTEGRAL are presented for both bursts. The two GRBs have long durations, slow pulses and are weak. The γ-ray spectra of both bursts are best fit with steep power-laws, implying they are X-ray rich. GRB 040223 is among the weakest and longest of INTEGRAL GRBs. The X-ray afterglow of this burst was detected 10 h after the prompt event by XMM-Newton. The measured spectral properties are consistent with a column density much higher than that expected from the Galaxy, indicating strong intrinsic absorption. We carried out near-infrared observations 17 h after the burst with the NTT of ESO, which yielded upper limits. Given the intrinsic absorption, we find that these limits are compatible with a simple extrapolation of the X-ray afterglow properties. For GRB 040624, we carried out optical observations 13 h after the burst with FORS 1 and 2 at the VLT, and DOLoRes at the TNG, again obtaining upper limits. We compare these limits with the magnitudes of a compilation of promptly observed counterparts of previous GRBs and show that they lie at the very faint end of the distribution. These two bursts are good examples of a population of bursts with dark or faint afterglows that are being unveiled through the increasing usage of large diameter telescopes engaged in comprehensive observational programmes.

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Section: The Prompt Eventsupporting

confidence: 86%

The weakINTEGRALbursts GRB 040223 and GRB 040624: an emerging population of dark afterglows

Filliatre¹,

Covino

D’Avanzo

et al. 2006

A&A

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“…Much attention has been given to the synchrotron emission from relativistic electrons, possibly accompanied by SSC emission to explain the observed GRB spectrum. These processes were found to be consistent with the observational data of many GRBs (Tavani 1996;Frontera et al 2000). However, several limitations have been reported in relation with the low-energy spectral slopes of time-integrated spectra (Crider et al 1997;Preece et al 2002;Ghirlanda et al 2002Ghirlanda et al , 2003Daigne et al 2009) and timeresolved spectra (Ghirlanda et al 2003).…”

Section: A Brief Review Of the Fireshell And Alternative Modelssupporting

confidence: 79%

A double component in GRB 090618: a proto-black hole and a genuinely long gamma-ray burst

Izzo

Ruffini

Penacchioni

et al. 2012

A&A

114

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Context. The joint X-ray and gamma-ray observations of GRB 090618 by very many satellites offer an unprecedented possibility of testing crucial aspects of theoretical models. In particular, they allow us to test (a) in the process of gravitational collapse, the formation of an optically thick e + e − -baryon plasma self-accelerating to Lorentz factors in the range 200 < Γ < 3000; (b) its transparency condition with the emission of a component of 10 53−54 baryons in the TeV region and (c) the collision of these baryons with the circumburst medium (CBM) clouds, characterized by dimensions of 10 15−16 cm. In addition, these observations offer the possibility of testing a new understanding of the thermal and power-law components in the early phase of this GRB. Aims. We test the fireshell model of GRBs in one of the closest (z = 0.54) and most energetic (E iso = 2.90 × 10 53 erg) GRBs, namely GRB 090618. It was observed at ideal conditions by several satellites, namely Fermi, Swift, Konus-WIND, AGILE, RT-2, and Suzaku, as well as from on-ground optical observatories. Methods. We analyzed the emission from GRB 090618 using several spectral models, with special attention to the thermal and powerlaw components. We determined the fundamental parameters of a canonical GRB within the context of the fireshell model, including the identification of the total energy of the e + e − plasma, E e + e − tot , the proper GRB (P-GRB), the baryon load, the density and structure of the CBM. Results. We find evidence of the existence of two different episodes in GRB 090618. The first episode lasts 50 s and is characterized by a spectrum consisting of a thermal component, which evolves between kT = 54 keV and kT = 12 keV, and a power law with an average index γ = 1.75 ± 0.04. The second episode, which lasts for ∼100 s, behaves as a canonical long GRB with a Lorentz gamma factor at transparency of Γ = 495, a temperature at transparency of 29.22 keV and with a characteristic size of the surrounding clouds of R cl ∼ 10 15−16 cm and masses of ∼10 22−24 g. Conclusions. We support the recently proposed two-component nature of GRB 090618, namely, episode 1 and episode 2, with a specific theoretical analysis. We furthermore illustrate that episode 1 cannot be considered to be either a GRB or a part of a GRB event, but it appears to be related to the progenitor of the collapsing bare core, leading to the formation of the black hole, which we call a "proto-black hole". Thus, for the first time, we are witnessing the process of formation of a black hole from the phases just preceding the gravitational collapse all the way up to the GRB emission.

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“…In addition, the index of the electron energy distribution derived in the sideways expanding jet scenario, p = 1.3, is very flat (in general, p values larger than 2 are found; see Frontera et al 2000) and may pose Fig. 6.…”

Section: Discussionmentioning

confidence: 88%

GRB010222: Afterglow emission from a rapidly decelerating shock

Masetti¹,

Palazzi²,

Pian³

et al. 2001

A&A

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Abstract. The GRB010222 optical and near-infrared (NIR) afterglow was monitored at the TNG and other Italian telescopes starting ∼1 day after the high-energy prompt event. The BV R light curves, which are the best sampled, are continuously steepening and can be described by two power laws, f (t) ∝ t −α , of indices α1 ∼ 0.7 and α2 ∼ 1.3 before and after a break occurring at about 0.5 days after the GRB start time, respectively. This model accounts well also for the flux in the U , I and J bands, which are less well monitored. The temporal break appears to be achromatic. The two K-band points are not consistent with the above behaviour, and rather suggest a constant trend. A low-resolution optical spectrum has also been taken with TNG. In the optical spectrum we found three absorption systems at different redshifts (0.927, 1.155 and 1.475), the highest of which represents a lower limit to, and probably coincides with, the redshift of the GRB. The broad-band optical spectral energy distributions do not appear to vary with time, consistently with the achromatic behaviour of the light curves. We compare our measurements with different afterglow evolution scenarios and we find that they favor a transition from relativistic to non-relativistic conditions in the shock propagation.

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Prompt and Delayed Emission Properties of Gamma‐Ray Bursts Observed with BeppoSAX

Cited by 190 publications

References 53 publications

The weakINTEGRALbursts GRB 040223 and GRB 040624: an emerging population of dark afterglows

The weakINTEGRALbursts GRB 040223 and GRB 040624: an emerging population of dark afterglows

A double component in GRB 090618: a proto-black hole and a genuinely long gamma-ray burst

GRB010222: Afterglow emission from a rapidly decelerating shock

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