The Collimation‐corrected Gamma‐Ray Burst Energies Correlate with the Peak Energy of Their ν<i>F</i><sub>ν</sub>Spectrum

Ghirlanda, G.; Ghisellini, G.; Lazzati, Davide

doi:10.1086/424913

Cited by 674 publications

(978 citation statements)

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“…We checked whether GRB 061201 satisfies the E p,i −E iso and E p,i − E γ correlations found for long GRBs (Amati et al 2002;Ghirlanda et al 2004), where E p,i is the intrinsic peak energy of the νF ν spectrum of the prompt emission. We find that, by rescaling the measured E p = 873 +458 −284 keV from Konus-Wind observations (Golenetskii et al 2006) at each proposed redshift for this burst, the isotropic and beaming corrected energy are several orders of magnitudes lower than the values predicted by the correlations.…”

Section: Discussionmentioning

confidence: 99%

A study of the prompt and afterglow emission of the short GRB 061201

Stratta¹,

D’Avanzo

Piranomonte

et al. 2007

A&A

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Context. Our knowledge of the intrinsic properties of short duration Gamma-Ray Bursts has relied, so far, only upon a few cases for which the estimate of the distance and an extended, multiwavelength monitoring of the afterglow have been obtained. Aims. We carried out multiwavelength observations of the short GRB 061201 aimed at estimating its distance and studying its properties. Methods. We performed a spectral and timing analysis of the prompt and afterglow emission and discuss the results in the context of the standard fireball model. Results. A clear temporal break was observed in the X-ray light curve about 40 min after the burst trigger. We find that the spectral and timing behaviour of the X-ray afterglow is consistent with a jet origin of the observed break, although the optical data can not definitively confirm this and other scenarios are possible. No underlying host galaxy down to R ∼ 26 mag was found after fading of the optical afterglow. Thus, no secure redshift could be measured for this burst. The nearest galaxy is at z = 0.111 and shows evidence of star formation activity. We discuss the association of GRB 061201 with this galaxy and with the ACO S 995 galaxy cluster, from which the source is at an angular distance of 17 and 8.5 , respectively. We also test the association with a possible undetected, positionally consistent galaxy at z ∼ 1. In all these cases, in the jet interpretation, we find a jet opening angle of 1-2 degrees.Key words. gamma rays: bursts IntroductionShort duration Gamma-ray Bursts (GRBs) are historically defined as those GRBs with burst duration less than two seconds and hard spectra (Kouveliotou et al. 1993). As the sample of short GRBs increases, in order to take into account all the spectral and temporal properties of the prompt emission, alternative empirical definitions of short GRBs have been introduced (e.g. Norris & Bonnell 2006;Zhang et al. 2007).The expected progenitor for short GRBs is a merging binary system of compact objects. However, our present knowledge of the intrinsic properties of short bursts mainly relies upon a few cases for which the distance could be derived and an extendedThe results reported in this paper are partially based on observations carried out at ESO telescopes under program 078.D-0809.INAF personnel resident at ASDC. multiwavelength monitoring of the afterglow was carried out.From these it appears that short bursts are less energetic and less collimated than long GRBs (e.g. Fox et al. 2005;Burrows et al. 2006;Soderberg et al. 2006). Intrinsic spectral parameters such as the peak energy E p of the EF(E) spectrum of the burst and the equivalent isotropic energy E iso , do not match the E p − E iso correlation for long GRBs (e.g. Amati 2007).The short bursts for which unambiguous hosts have been found are at redshifts between z = 0.10 and z = 0.55. The optical afterglows of seven short bursts and their likely host galaxies have been recently observed with telescopes such as ESO/VLT, Gemini, Magellan and HST, but no firm estimation of...

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Section: Discussionmentioning

confidence: 99%

A study of the prompt and afterglow emission of the short GRB 061201

Stratta¹,

D’Avanzo

Piranomonte

et al. 2007

A&A

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“…However, statistical investigations of large samples of GRBs aim to find common characteristics and correlations that link individual events and therefore provide insight into the mechanisms common to GRBs. Statistical investigations performed so far have found a number of trends and correlations within and linking the prompt gamma-ray emission and the afterglow emission (e.g., Amati et al 2002;Ghirlanda, Ghisellini & Lazzati 2004;Dainotti, Cardone & Capozziello 2008;Panaitescu & Vestrand 2008;Bernardini et al 2012;D'Avanzo et al 2012;Li et al 2012;Liang et al 2013;Zaninoni et al 2013;Panaitescu, Vestrand & Woźniak 2013). Within the prompt gamma-ray emission, the most renowned correlation discovered is the Amati relation, a correlation between the isotropic γ-ray energy Eiso and the restframe γ-ray peak energy E peak (see Amati et al 2002, and references therein).…”

Section: Introductionmentioning

confidence: 99%

Exploring the canonical behaviour of long gamma-ray bursts using an intrinsic multiwavelength afterglow correlation

Oates

Racusin

Pasquale

et al. 2015

Mon. Not. R. Astron. Soc.

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In this paper we further investigate the relationship, reported by Oates et al. (2012), between the optical/UV afterglow luminosity (measured at restframe 200 s) and average afterglow decay rate (measured from restframe 200 s onwards) of long duration Gamma-ray Bursts (GRBs). We extend the analysis by examining the X-ray light curves, finding a consistent correlation. We therefore explore how the parameters of these correlations relate to the prompt emission phase and, using a Monte Carlo simulation, explore whether these correlations are consistent with predictions of the standard afterglow model. We find significant correlations between: log L O,200s and log L X,200s ; α O,>200s and α X,>200s , consistent with simulations. The model also predicts relationships between log E iso and log L 200,s , however, while we find such relationships in the observed sample, the slope of the linear regression is shallower than that simulated and inconsistent at 3σ. Simulations also do not agree with correlations observed between log L 200s and α >200s , or log E iso and α >200s . Overall, these observed correlations are consistent with a common underlying physical mechanism producing GRBs and their afterglows regardless of their detailed temporal behaviour. However, a basic afterglow model has difficulty explaining all the observed correlations. This leads us to briefly discuss alternative more complex models.

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“…Ghirlanda et al (2004) suggested that the maximum opening angle is about θ max = 24 o . In this paper, the opening angle for each GRB is generated randomly within θ < θ max .…”

Section: Samples and Equationsmentioning

confidence: 99%

Pulsar kicks andγ-ray burst

Cui

Wang²,

et al. 2007

A&A

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Aims. We use the supernova-GRB (γ-ray burst) association and assume that the GRB asymmetric explosions produce pulsars in order to test the consistency of distributions of modeled and observed pulsar-kick velocities. Methods. The deduced distribution of kick velocity from the model of GRB and the observed kick distribution of radio pulsars are checked by a K-S test. Results. These two distributions are found to come from the same parent population. Conclusions. This result may indicate that GRBs could really be related to supernova and that the asymmetry of GRB associated with supernova would cause the pulsar kick.

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The Collimation‐corrected Gamma‐Ray Burst Energies Correlate with the Peak Energy of Their νF_νSpectrum

Cited by 674 publications

References 64 publications

A study of the prompt and afterglow emission of the short GRB 061201

A study of the prompt and afterglow emission of the short GRB 061201

Exploring the canonical behaviour of long gamma-ray bursts using an intrinsic multiwavelength afterglow correlation

Pulsar kicks andγ-ray burst

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The Collimation‐corrected Gamma‐Ray Burst Energies Correlate with the Peak Energy of Their νFνSpectrum

Cited by 674 publications

References 64 publications

A study of the prompt and afterglow emission of the short GRB 061201

A study of the prompt and afterglow emission of the short GRB 061201

Exploring the canonical behaviour of long gamma-ray bursts using an intrinsic multiwavelength afterglow correlation

Pulsar kicks andγ-ray burst

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The Collimation‐corrected Gamma‐Ray Burst Energies Correlate with the Peak Energy of Their νF_νSpectrum