A Comprehensive Study of GRB 070125, A Most Energetic Gamma‐Ray Burst

Chandra, Poonam; Cenko, S. B.; Frail, D. A.; Chevalier, Roger A.; Macquart, Jean–Pierre; Kulkarni, S. R.; Bock, Douglas C.-J.; Bertoldi, F.; Kasliwal, Mansi M.; Fox, D. B.; Price, P. A.; Berger, E.; Söderberg, A. M.; Harrison, Fiona A.; Gal‐Yam, A.; Ofek, E. O.; Rau, A.; Schmidt, B.; Cameron, P. B.; Cowie, L. L.; Cowie, Antionette; Roth, Katherine C.; Dopita, Michael A.; Peterson, Bruce A.; Penprase, Bryan E.

doi:10.1086/589807

Cited by 80 publications

(98 citation statements)

References 61 publications

(57 reference statements)

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“…These values are similar to those obtained for GRBs at z∼1 (Panaitescu & Kumar 2002;Yost et al 2003;Chandra et al 2008;Cenko et al 2010Cenko et al , 2011Laskar et al 2014), indicating no evolution in these properties with a redshift to z∼5.…”

Section: Summary and Discussionsupporting

confidence: 85%

“…Similar late-time X-ray excess emission has been observed in other GRBs, with suggested explanations, including dust echoes and inverse-Compton scattering (Shao & Dai 2007;Chandra et al 2008;Liang et al 2008;Margutti et al 2010;Fong et al 2014). Alternatively, the discrepancy may arise from the simplistic treatment of the hydrodynamics at the jet break, such as exponential sideways expansion (Rhoads 1999), which is likely an incomplete description of the blast wave evolution (Zhang & MacFadyen 2009;Granot & Piran 2012;Duffell & Laskar 2017).…”

Section: F T 1 3 a Mmentioning

confidence: 56%

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A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

Laskar

Berger

Chornock

et al. 2018

ApJ

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We present the first results from a recently concluded study of GRBs at z  5 with the Karl G. Jansky Very Large Array (VLA). Spanning 1 to 85.5 GHz and 7 epochs from 1.5 to 82.3 days, our observations of GRB140311A are the most detailed joint radio and millimeter observations of a GRB afterglow at z  5 to date. In conjunction with optical/near-IR and X-ray data, the observations can be understood in the framework of radiation from a single blast wave shock with energy »É 8.5 10 K,iso 53 erg expanding into a constant density environment with density, » n 8 0 -cm 3 . The X-ray and radio observations require a jet break at » t 0.6 jet days, yielding an opening angle of q »  4 jet and a beaming-corrected blast wave kinetic energy of »É 2.2 10 K 50 erg. The results from our radio follow-up and multiwavelength modeling lend credence to the hypothesis that detected high-redshift GRBs may be more tightly beamed than events at lower redshift. We do not find compelling evidence for reverse shock emission, which may be related to fast cooling driven by the moderately high circumburst density.

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Section: Summary and Discussionsupporting

confidence: 85%

Section: F T 1 3 a Mmentioning

confidence: 56%

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

Laskar

Berger

Chornock

et al. 2018

ApJ

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“…The configuration and data reduction are identical to those described by Chandra et al (2008). We report a nondetection at the optical afterglow position with a 2σ limit of 0.50 mJy (Bock et al 2008).…”

Section: Grb 080319bmentioning

confidence: 70%

THE COLLIMATION AND ENERGETICS OF THE BRIGHTESTSWIFTGAMMA-RAY BURSTS

Cenko

Frail

Harrison

et al. 2010

ApJ

128

127

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Long-duration gamma-ray bursts (GRBs) are widely believed to be highly collimated explosions (bipolar conical outflows with half-opening angle θ ≈ 1 • -10 • ). As a result of this beaming factor, the true energy release from a GRB is usually several orders of magnitude smaller than the observed isotropic value. Measuring this opening angle, typically inferred from an achromatic steepening in the afterglow light curve (a "jet" break), has proven exceedingly difficult in the Swift era. Here, we undertake a study of five of the brightest (in terms of the isotropic prompt γ -ray energy release, E γ,iso ) GRBs in the Swift era to search for jet breaks and hence constrain the collimation-corrected energy release. We present multi-wavelength (radio through X-ray) observations of GRBs 050820A, 060418, and 080319B, and construct afterglow models to extract the opening angle and beaming-corrected energy release for all three events. Together with results from previous analyses of GRBs 050904 and 070125, we find evidence for an achromatic jet break in all five events, strongly supporting the canonical picture of GRBs as collimated explosions. The most natural explanation for the lack of observed jet breaks from most Swift GRBs is therefore selection effects. However, the opening angles for the events in our sample are larger than would be expected if all GRBs had a canonical energy release of ∼10 51 erg. The total energy release we measure for the "hyper-energetic" (E tot 10 52 erg) events in our sample is large enough to start challenging models with a magnetar as the compact central remnant.

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“…However, an energetic explosion does not appear to be an exclusive property of high-z GRBs. There is a small but growing population of bursts with energy > 10 52 erg, termed 'hyper-energetic GRBs' [6], which includes moderate-z events like GRB 070125 [8] and GRB 050820A [7]. Another potentially useful diagnostic is the density structure in the immediate environs of the progenitor star.…”

Section: Figurementioning

confidence: 99%

The most distant cosmological explosion

Chandra

Frail

Fox³

et al. 2011

AIP Conference Proceedings

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Abstract. At a redshift of 8.3 GRB 090423 marks the highest known redshift object in the Universe. By combining our radio measurements with existing X-ray and infrared observations, we estimated the kinetic energy of the afterglow, the geometry of the outflow and the density of the circumburst medium. Our best fit model is a quasi-spherical, high-energy explosion in a low, constant-density medium. We compare the properties of GRB 090423 with a sample of GRBs at moderate redshifts. We find that the high energy and afterglow properties of GRB 090423 are not sufficiently different from other GRBs to suggest a different kind of progenitor, such as a Population III star. However, we argue that it is not clear that the afterglow properties alone can provide convincing identification of Population III progenitors. We suggest that the millimeter and centimeter radio detections of GRB 090423 at early times contained emission from a reverse shock component. This has important implications for the detection of high redshift GRBs by the next generation of radio facilities.

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A Comprehensive Study of GRB 070125, A Most Energetic Gamma‐Ray Burst

Cited by 80 publications

References 61 publications

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

THE COLLIMATION AND ENERGETICS OF THE BRIGHTESTSWIFTGAMMA-RAY BURSTS

The most distant cosmological explosion

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