Photometry and spectroscopy of GRB 060526: a detailed study of the afterglow and host galaxy of a<i>z</i> = 3.2 gamma-ray burst

Thöne, C. C.; Канн, Д. А.; Jóhannesson, G.; Selj, Josefine; Jaunsen, A. O.; Fynbo, J. P. U.; Akerlof, C.; Baliyan, K. S.; Bartolini, C.; Bikmaev, I.; Bloom, J.; Burenin, R.; Cobb, B. E.; Covino, S.; Curran, P. A.; Dahle, H.; Ferrero, Alejandro; Foley, S.; French, J.; Fruchter, A. S.; Ganesh, S.; Graham, John F.; Greco, G.; Гуарниери, А.; Hanlon, L.; Hjorth, J.; Ibrahimov, M.; Israel, G. L.; Jakobsson, P.; Jelínek, M.; Jensen, B. L.; Jørgensen, U. G.; Khamitov, I.; Koch, T. S.; Levan, A. J.; Malesani, D.; Masetti, N.; Meehan, S.; Melady, G.; Nanni, D.; Näränen, Jyri; Pakštienė, E.; Pavlinsky, M.; Perley, D.; Piccioni, A.; Pizzichini, G.; Pozanenko, A.; Roming, P. W. A.; Rujopakarn, W.; Rumyantsev, V.; Rykoff, E. S.; Sharapov, D.; Starr, D.; Sunyaev, R.; Swan, H.; Tanvir, N. R.; Terra, F.; Postigo, A. de Ugarte; Vreeswijk, P. M.; Wilson, Andrew; Yost, S. A.; Yuan, F.

doi:10.1051/0004-6361/200810340

Cited by 37 publications

(12 citation statements)

References 139 publications

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“…Early time optical emission could be associated with the late internal shock scenario. The optical LC at later times shows some deviations from the smooth power-law behaviour, which can be explained by energy injections from the central engine (Dai et al 2007;Thöne et al 2010).…”

Section: Sub-samplementioning

confidence: 94%

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GRB 090727 and Gamma-Ray Bursts With Early-Time Optical Emission

Kopač

Kobayashi

Gomboc

et al. 2013

ApJ

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We present a multi-wavelength analysis of gamma-ray burst GRB 090727, for which optical emission was detected during the prompt gamma-ray emission by the 2-m autonomous robotic Liverpool Telescope and subsequently monitored for a further two days with the Liverpool and Faulkes telescopes. Within the context of the standard fireball model, we rule out a reverse shock origin for the early time optical emission in GRB 090727 and instead conclude that the early time optical flash likely corresponds to emission from an internal dissipation processes. Putting GRB 090727 into a broader observational and theoretical context, we build a sample of 36 gamma-ray bursts (GRBs) with contemporaneous early time optical and gamma-ray detections. From these GRBs, we extract a sub-sample of 18 GRBs, which show optical peaks during prompt gamma-ray emission, and perform detailed temporal and spectral analysis in gamma-ray, X-ray, and optical bands. We find that in most cases early time optical emission shows sharp and steep behaviour, and notice a rich diversity of spectral properties. Using a simple internal shock dissipation model, we show that the emission during prompt GRB phase can occur at very different frequencies via synchrotron radiation. Based on the results obtained from observations and simulation, we conclude that the standard external shock interpretation for early time optical emission is disfavoured in most cases due to sharp peaks (∆t/t < 1) and steep rise/decay indices, and that internal dissipation can explain the properties of GRBs with optical peaks during gamma-ray emission.

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Section: Sub-samplementioning

confidence: 94%

“…Energetics: At redshift z = 3.221 this GRB had an isotropic gamma-ray energy release of E γ,iso ≈ 2.4 × 10 52 ergs in 15 − 150 keV band (Thöne et al 2010).…”

Section: Sub-samplementioning

confidence: 99%

GRB 090727 and Gamma-Ray Bursts With Early-Time Optical Emission

Kopač

Kobayashi

Gomboc

et al. 2013

ApJ

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“…13 For discussion on X-ray flares see e.g., O'Brien et al 2006;Chincarini et al 2007;Margutti et al 2010. 14 For optical flares/rebrightenings see e.g., Akerlof et al 1999;Blake et al 2005;Vestrand et al 2005;Page et al 2007;Mundell et al 2007a;Racusin et al 2008;Thöne et al 2010;Guidorzi et al 2011;Gendre et al 2012Gendre et al , 2013Kopač et al 2013;Virgili et al 2013;Elliott et al 2014;Greiner et al 2014;Vestrand et al 2014;Nappo et al 2014. 15 For X-ray flashes see e.g., Boër et al 2006;Krühler et al 2009;Guidorzi et al 2009. On 2014 April 30, at t 0 = 20 : 33 : 36 UT, the Burst Alert Telescope (BAT; Barthelmy et al 2005) onboard the Swift satellite triggered on the long GRB 140430A and immediately slewed to the burst (Siegel et al 2014).…”

Section: Swiftmentioning

confidence: 99%

Limits on Optical Polarization During the Prompt Phase of GRB 140430a

Kopač

Mundell

Japelj

et al. 2015

ApJ

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Gamma-ray burst GRB 140430A was detected by the Swift satellite and observed promptly with the imaging polarimeter RINGO3 mounted on the Liverpool Telescope, with observations beginning while the prompt γ-ray emission was still ongoing. In this paper, we present densely sampled (10second temporal resolution) early optical light curves in 3 optical bands and limits to the degree of optical polarization. We compare optical, X-ray and gamma-ray properties and present an analysis of the optical emission during a period of high-energy flaring. The complex optical light curve cannot be explained merely with a combination of forward and reverse shock emission from a standard external shock, implying additional contribution of emission from internal shock dissipation. We estimate an upper limit for time averaged optical polarization during the prompt phase to be as low as P < 12% (1σ). This suggests that the optical flares and early afterglow emission in this GRB are not highly polarized. Alternatively, time averaging could mask the presence of otherwise polarized components of distinct origin at different polarization position angles.

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“…The detection of GRBs is at once both independent of the luminosity of their host galaxy and, at high energies, unaffected by dust obscuration. They are also extremely luminous at all wavelengths, so that they can be used to perform transmission spectroscopy of their host galaxies, even where such hosts are too faint to be detected photometrically (e.g., Thöne et al 2010). This also permits them to be found across the universe from very low to very high redshift: Indeed, GRB 090423 holds the record at z = 8.2 for the most distant spectroscopically confirmed object known (Tanvir et al 2009;Salvaterra et al 2009).…”

Section: Introductionmentioning

confidence: 99%

The Optically Unbiased Gamma-Ray Burst Host (Tough) Survey. I. Survey Design and Catalogs

Hjorth

Malesani

Jakobsson

et al. 2012

ApJ

166

142

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Long-duration gamma-ray bursts (GRBs) are powerful tracers of star-forming galaxies. We have defined a homogeneous subsample of 69 Swift GRB-selected galaxies spanning a very wide redshift range. Special attention has been devoted to making the sample optically unbiased through simple and well-defined selection criteria based on the high-energy properties of the bursts and their positions on the sky. Thanks to our extensive follow-up observations, this sample has now achieved a comparatively high degree of redshift completeness, and thus provides a legacy sample, useful for statistical studies of GRBs and their host galaxies. In this paper, we present the survey design and summarize the results of our observing program conducted at the ESO Very Large Telescope (VLT) aimed at obtaining the most basic properties of galaxies in this sample, including a catalog of R and K s magnitudes and redshifts. We detect the host galaxies for 80% of the GRBs in the sample, although only 42% have K s -band detections, which confirms that GRB-selected host galaxies are generally blue. The sample is not uniformly blue, however, with two extremely red objects detected. Moreover, galaxies hosting GRBs with no optical/NIR afterglows, whose identification therefore relies on X-ray localizations, are significantly brighter and redder than those with an optical/NIR afterglow. This supports a scenario where GRBs occurring in more massive and dusty galaxies frequently suffer high optical obscuration. Our spectroscopic campaign has resulted in 77% now having redshift measurements, with a median redshift of 2.14 ± 0.18. TOUGH alone includes 17 detected z > 2 Swift GRB host galaxies suitable for individual and statistical studies-a substantial increase over previous samples. Seven hosts have detections of the Lyα emission line and we can exclude an early indication that Lyα emission is ubiquitous among GRB hosts, but confirm that Lyα is stronger in GRB-selected galaxies than in flux-limited samples of Lyman break galaxies.

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Photometry and spectroscopy of GRB 060526: a detailed study of the afterglow and host galaxy of az = 3.2 gamma-ray burst

Cited by 37 publications

References 139 publications

GRB 090727 and Gamma-Ray Bursts With Early-Time Optical Emission

GRB 090727 and Gamma-Ray Bursts With Early-Time Optical Emission

Limits on Optical Polarization During the Prompt Phase of GRB 140430a

The Optically Unbiased Gamma-Ray Burst Host (Tough) Survey. I. Survey Design and Catalogs

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