A Comparison of the Afterglows of Short- And Long-Duration Gamma-Ray Bursts

Nysewander, M.; Fruchter, A. S.; Pe’er, Asaf

doi:10.1088/0004-637x/701/1/824

Cited by 158 publications

(230 citation statements)

References 106 publications

(95 reference statements)

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“…This is consistent with previous studies (e.g. Kouveliotou et al 2004;De Pasquale et al 2006;Nysewander, Fruchter & Pe'er 2009;Kann et al 2010), particularly with D'Avanzo et al (2012) and Margutti et al (2013), who performed a similar study using early X-ray luminosity, approximately 5 − 10 minutes after trigger. We have shown for the first time a correlation which relates the average temporal behaviour with log Eiso and E peak .…”

Section: Discussionsupporting

confidence: 93%

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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Section: Discussionsupporting

confidence: 93%

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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“…Figure 3 shows the light curves of the different GRB populations. In agreement with previous studies (Gehrels et al 2008;Nysewander et al 2009) and although the amount of short burst light curves is limited, the short population bursts are clearly fainter on average than the other two groups. Comparing intermediate and long bursts, we see that there is also a bimodality in the luminosity distribution with intermediate bursts being on average one order of magnitude fainter.…”

Section: X-ray Afterglowssupporting

confidence: 93%

“…Four years after the detection of its first GRB, the Swift database had 394 bursts, of which 40% have measured redshifts. This rapidly growing sample has allowed statistical studies to be performed of the short and long population of bursts (Kann et al 2010(Kann et al , 2008Gehrels et al 2008;Nysewander et al 2009). In this paper, we use the sample of the first four years of Swift GRBs with known redshifts to search for the specific properties of the intermediate population, trying to evaluate whether any significant difference with respect to the other groups exists.…”

Section: Introductionmentioning

confidence: 99%

Searching for differences inSwift’s intermediate GRBs

Postigo

Horváth²,

Vereš

et al. 2010

A&A

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Context. Gamma-ray bursts are usually classified in terms their high-energy emission into either short-duration or long-duration bursts, which presumably reflect two different types of progenitors. However, it has been shown on statistical grounds that a third, intermediate population is needed in this classification scheme, although an extensive study of the properties of this class has so far not been performed. The large amount of follow-up studies generated during the Swift era allows us to have a sufficient sample to attempt a study of this third population through the properties of their prompt emission and their afterglows. Aims. To understand the differences of the intermediate population, we study a sample of GRBs observed by Swift during its first four years of operation. The sample contains only bursts with measured redshifts since these data help us to derive intrinsic properties. Methods. We search for differences in the properties of the three groups of bursts, which we quantify using a Kolmogorov-Smirnov test whenever possible. Results. Intermediate bursts are found to be less energetic and have dimmer afterglows than long GRBs, especially when considering the X-ray light curves, which are on average one order of magnitude fainter than long bursts. There is a less significant trend in the redshift distribution that places intermediate bursts closer than long bursts. Except for this, intermediate bursts show similar properties to long bursts. In particular, they follow the E peak versus E iso correlation and have, on average, positive spectral lags with a distribution similar to that of long bursts. As for long GRBs, they normally have an associated supernova, although some intermediate bursts have been found to contain no supernova component. Conclusions. This study shows that intermediate bursts differ from short bursts, but exhibit no significant differences from long bursts apart from their lower brightness. We suggest that the physical difference between intermediate and long bursts could be explained by being produced by similar progenitors, of the former being the ejecta thin shells and the latter thick shells.

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“…For a recent review of short bursts and their progenitors see Nakar (2007) and Lee & Ramirez-Ruiz (2007). In contrast to long GRBs, the afterglows of the short bursts are generally fainter (Kann et al 2008;Nysewander et al 2009), making it difficult to obtain an absorption line spectrum of the afterglow itself. Almost exclusively, the distances to short bursts are obtained by associations with and observations of the (putative) host galaxies (e.g., Berger 2009;Graham et al 2009).…”

Section: Discussionmentioning

confidence: 99%

Optical and near-infrared follow-up observations of fourFermi/LAT GRBs: redshifts, afterglows, energetics, and host galaxies

McBreen

Krühler

Rau

et al. 2010

A&A

114

100

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Aims. Fermi can measure the spectral properties of gamma-ray bursts over a very large energy range and is opening a new window on the prompt emission of these energetic events. Localizations by the instruments on Fermi in combination with follow-up by Swift provide accurate positions for observations at longer wavelengths leading to the determination of redshifts, the true energy budget, host galaxy properties and facilitate comparison with pre-Fermi bursts. Methods. Multi-wavelength follow-up observations were performed on the afterglows of four bursts with high energy emission detected by Fermi/LAT: GRB 090323, GRB 090328, GRB 090510 and GRB 090902B. They were obtained in the optical/near-infrared bands with GROND mounted at the MPG/ESO 2.2 m telescope and additionally of GRB 090323 in the optical with the 2 m telescope in Tautenburg, Germany. Three of the events are classified as long bursts while GRB 090510 is a well localized short GRB with GeV emission. In addition, host galaxies were detected for three of the four bursts. Spectroscopic follow-up was initiated with the VLT for GRB 090328 and GRB 090510. Results. The afterglow observations in 7 bands are presented for all bursts and their host galaxies are investigated. Knowledge of the distance and the local dust extinction enables comparison of the afterglows of LAT-detected GRBs with the general sample. The spectroscopic redshifts of GRB 090328 and GRB 090510 were determined to be z = 0.7354 ± 0.0003 and z = 0.903 ± 0.001 and dust corrected star-formation rates of 4.8 M yr −1 and 0.60 M yr −1 were derived for their host galaxies, respectively. Conclusions. The afterglows of long bursts exhibit power-law decay indices (α) from less than 1 to ∼2.3 and spectral indices (β opt ) values from 0.65 to ∼1.2 which are fairly standard for GRB afterglows. Constraints are placed on the jet half opening angles of < ∼ 2.1 • to > ∼ 6.4 • , which allows limits to be placed on the beaming corrected energies. These range from < ∼ 5 × 10 50 erg to the one of the highest values ever recorded, > ∼ 2.2 × 10 52 erg for GRB 090902B, and are not consistent with a standard candle. The extremely energetic long Fermi bursts have optical afterglows which lie in the top half of the brightness distribution of all optical afterglows detected in the Swift era or even in the top 5% if incompleteness is considered. The properties of the host galaxies of these LAT detected bursts in terms of extinction, star formation rates and masses do not appear to differ from previous samples.

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A Comparison of the Afterglows of Short- And Long-Duration Gamma-Ray Bursts

Cited by 158 publications

References 106 publications

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

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

Searching for differences inSwift’s intermediate GRBs

Optical and near-infrared follow-up observations of fourFermi/LAT GRBs: redshifts, afterglows, energetics, and host galaxies

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