<i>FERMI</i>AND<i>SWIFT</i>GAMMA-RAY BURST AFTERGLOW POPULATION STUDIES

Racusin, J. L.; Oates, S. R.; Schady, P.; Burrows, D. N.; Pasquale, M. de; Donato, D.; Gehrels, N.; Koch, S.; McEnery, J. E.; Piran, Tsvi; Roming, P. W. A.; Sakamoto, T.; Swenson, C. A.; Troja, E.; Vasileiou, V.; Virgili, F. J.; Wanderman, David; Zhang, Bing

doi:10.1088/0004-637x/738/2/138

Cited by 109 publications

(156 citation statements)

References 74 publications

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“…The Amati correlation was investigated (Basak & Rao 2013;Gruber 2012) and a link between short and long GRBs was discovered (Muccino et al 2013). It gave insight into the GRB afterglow population (Racusin et al 2011), allowed to observe a number of high-energy GRBs (with photon energies exceeding 100 MeV, or even 10 GeV) (Atwood et al 2013), and provided a verification of the short-long classification (Zhang et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Distinguishing short and longFermigamma-ray bursts

Tarnopolski

2015

Mon. Not. R. Astron. Soc.

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Two classes of gamma-ray bursts (GRBs), short and long, have been determined without any doubts, and are usually ascribed to different progenitors, yet these classes overlap for a variety of descriptive parameters. A subsample of 46 long and 22 short Fermi GRBs with estimated Hurst Exponents (HEs), complemented by minimum variability time-scales (MVTS) and durations (T 90 ) is used to perform a supervised Machine Learning (ML) and Monte Carlo (MC) simulation using a Support Vector Machine (SVM) algorithm. It is found that while T 90 itself performs very well in distinguishing short and long GRBs, the overall success ratio is higher when the training set is complemented by MVTS and HE. These results may allow to introduce a new (non-linear) parameter that might provide less ambiguous classification of GRBs.

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Section: Introductionmentioning

confidence: 99%

Distinguishing short and longFermigamma-ray bursts

Tarnopolski

2015

Mon. Not. R. Astron. Soc.

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“…Ghirlanda et al 2012). It should be noted that some of the most powerful GRBs including GRB 120711A are also detected by Fermi/LAT (McBreen et al 2010;Racusin et al 2011;Ackermann et al 2013). The emission from GRB 120711A is well modelled using a density profile of k ∼ 1.2, which corresponds to an intermediate case between the ISM and wind environments.…”

Section: Grb 120711a As a Member Of The Long Grb Populationmentioning

confidence: 95%

GRB 120711A: an intense INTEGRAL burst with long-lasting softγ-ray emission and a powerful optical flash

Martín-Carrillo

Hanlon

Topinka

et al. 2014

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A long and intense γ-ray burst (GRB) was detected by INTEGRAL on 11 July 2012 with a duration of ∼115 s and fluence of 2.8 × 10 −4 erg cm −2 in the 20 keV−8 MeV energy range. GRB 120711A was at z ∼ 1.405 and produced soft γ-ray emission (>20 keV) for at least ∼10 ks after the trigger. The GRB was observed by several ground-based telescopes that detected a powerful optical flash peaking at an R-band brightness of ∼11.5 mag at ∼126 s after the trigger, or ∼9th magnitude when corrected for the host galaxy extinction (A V ∼ 0.85). The X-ray afterglow was monitored by the Swift, XMM-Newton, and Chandra observatories from 8 ks to 7 Ms and provides evidence for a jet break at ∼0.9 Ms. We present a comprehensive temporal and spectral analysis of the long-lasting soft γ-ray emission detected in the 20−200 keV band with INTEGRAL/IBIS, the Fermi/LAT post-GRB detection above 100 MeV, the soft X-ray afterglow and the optical/near-infrared detections from Watcher, Skynet/PROMPT, GROND, and REM. The prompt emission had a very hard spectrum (E peak ∼ 1 MeV) and yields an E γ,iso ∼ 10 54 erg (1 keV−10 MeV rest frame), making GRB 120711A one of the most energetic GRBs detected so far. We modelled the long-lasting soft γ-ray emission using the standard afterglow scenario, which indicates a forward shock origin. The combination of data extending from the near-infrared to GeV energies suggest that the emission is produced by a broken power-law spectrum consistent with synchrotron radiation. The afterglow is well modelled using a stratified wind-like environment with a density profile k ∼ 1.2, suggesting a massive star progenitor (i.e. Wolf-Rayet) with a mass-loss rate between ∼10 −5 −10 −6 M yr −1 depending on the value of the radiative efficiency (η γ = 0.2 or 0.5). The analysis of the reverse and forward shock emission reveals an initial Lorentz factor of ∼120−340, a jet half-opening angle of ∼2 • −5 • , and a baryon load of ∼10 −5 −10 −6 M consistent with the expectations of the fireball model when the emission is highly relativistic. Long-lasting soft γ-ray emission from other INTEGRAL GRBs with high peak fluxes, such as GRB 041219A, was not detected, suggesting that a combination of high Lorentz factor, emission above 100 MeV, and possibly a powerful reverse shock are required. Similar long-lasting soft γ-ray emission has recently been observed from the nearby and extremely bright Fermi/LAT burst GRB 130427A.

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“…In addition, Ghisellini et al (2009) also investigated the relation between E γ,prompt and the kinetic isotropic energy in the afterglow, E k,af t , with the same sample, finding a relation with b = 0.42. Similarly, Racusin et al (2011) studied the same relation, using 69 GRBs and assuming different efficiencies to find some limits between E k,af t and E γ,prompt , see the right panel of Fig. 14. This relation was most likely used to study the differences in detection of several instruments and to analyze the transferring process of kinetic energy into the prompt emission in GRBs, making the relation by Racusin et al (2011) the most reliable one.…”

Section: The Prompt-afterglow Relationsmentioning

confidence: 96%

Gamma Ray Burst afterglow and prompt-afterglow relations: An overview

Dainotti

Vecchio

2017

New Astronomy Reviews

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The mechanism responsible for the afterglow emission of Gamma Ray Bursts (GRBs) and its connection to the prompt γ-ray emission is still a debated issue. Relations between intrinsic properties of the prompt or afterglow emission can help to discriminate between plausible theoretical models of GRB production. Here we present an overview of the afterglow and prompt-afterglow two parameter relations, their physical interpretations, their use as redshift estimators and as possible cosmological tools. A similar task has already been correctly achieved for Supernovae (SNe) Ia by using the peak magnitude-stretch relation, known in the literature as the Phillips relation (Phillips 1993). The challenge today is to make GRBs, which are amongst the farthest objects ever observed, standardizable candles as the SNe Ia through well established and robust relations. Thus, the study of relations amongst the observable and physical properties of GRBs is highly relevant together with selection biases in their physical quantities. Therefore, we describe the state of the art of the existing GRB relations, their possible and debated interpretations in view of the current theoretical models and how relations are corrected for selection biases. We conclude that only after an appropriate evaluation and correction for selection effects can GRB relations be used to discriminate among the theoretical models responsible for the prompt and afterglow emission and to estimate cosmological parameters.

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FERMIANDSWIFTGAMMA-RAY BURST AFTERGLOW POPULATION STUDIES

Cited by 109 publications

References 74 publications

Distinguishing short and longFermigamma-ray bursts

Distinguishing short and longFermigamma-ray bursts

GRB 120711A: an intense INTEGRAL burst with long-lasting softγ-ray emission and a powerful optical flash

Gamma Ray Burst afterglow and prompt-afterglow relations: An overview

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