Prompt optical observations of GRB 080330 and GRB 080413A

Yuan, F.; Rykoff, E. S.; Schaefer, Bradley E.; Rujopakarn, W.; Güver, T.; Aharonian, F.; Akerlof, C.; Ashley, M. C. B.; Barthelmy, S. D.; Gehrels, N.; Gögăüş, E.; Horns, D.; Kızıloğlu, Ü.; Krimm, H. A.; McKay, T. A.; Özel, M. E.; Phillips, A.; Quimby, R.; Rowell, G.; Swan, H.; Vestrand, W. T.; Wheeler, J. C.; Wren, J.

doi:10.1063/1.3027891

Cited by 6 publications

(3 citation statements)

References 5 publications

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“…This GRB afterglow was rapidly observed by many observatories on the western Pacific rim. It shows a plateau phase early on (Yuan et al 2007b;Huang et al 2008a), after 0.003 days, we find a decay slope of α = 0.93 ± 0.02 in the R C band. The SED is broad (UVW1 to K), shows slight curvature, is well fit by a small amount of SMC dust and shows a strong dropout in UV M2 and UVW2, in agreement with the low redshift (z = 0.8227; Fynbo et al 2009).…”

Section: B2 Details On the Swift-era Golden Samplementioning

confidence: 81%

“…We constructed the light curve and the SED with data from the following sources ), Yuan et al (2007b), Wang et al (2007, Klotz et al (2007), Burenin et al (2007), Chen et al (2007aChen et al ( , 2007b, Dintinjana et al (2007), Oates & Stratta (2007), Ishimura et al (2007b), Greco et al (2007), Sposetti (2007b), Yoshida et al (2007c), Uemura et al (2007b), Minezaki et al (2007), and Huang et al (2008a). This GRB afterglow was rapidly observed by many observatories on the western Pacific rim.…”

Section: B2 Details On the Swift-era Golden Samplementioning

confidence: 99%

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THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

Канн

Klose

Zhang

et al. 2010

ApJ

287

356

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15131514 KANN ET AL.Vol. 720 ABSTRACT We have gathered optical photometry data from the literature on a large sample of Swift-era gamma-ray burst (GRB) afterglows including GRBs up to 2009 September, for a total of 76 GRBs, and present an additional three pre-Swift GRBs not included in an earlier sample. Furthermore, we publish 840 additional new photometry data points on a total of 42 GRB afterglows, including large data sets for GRBs 050319, 050408, 050802, 050820A, 050922C, 060418, 080413A, and 080810. We analyzed the light curves of all GRBs in the sample and derived spectral energy distributions for the sample with the best data quality, allowing us to estimate the host-galaxy extinction. We transformed the afterglow light curves into an extinction-corrected z = 1 system and compared their luminosities with a sample of pre-Swift afterglows. The results of a former study, which showed that GRB afterglows clustered and exhibited a bimodal distribution in luminosity space, are weakened by the larger sample. We found that the luminosity distribution of the two afterglow samples (Swift-era and pre-Swift) is very similar, and that a subsample for which we were not able to estimate the extinction, which is fainter than the main sample, can be explained by assuming a moderate amount of line-of-sight host extinction. We derived bolometric isotropic energies for all GRBs in our sample, and found only a tentative correlation between the prompt energy release and the optical afterglow luminosity at 1 day after the GRB in the z = 1 system. A comparative study of the optical luminosities of GRB afterglows with echelle spectra (which show a high number of foreground absorbing systems) and those without, reveals no indication that the former are statistically significantly more luminous. Furthermore, we propose the existence of an upper ceiling on afterglow luminosities and study the luminosity distribution at early times, which was not accessible before the advent of the Swift satellite. Most GRBs feature afterglows that are dominated by the forward shock from early times on. Finally, we present the first indications of a class of long GRBs, which form a bridge between the typical highluminosity, high-redshift events and nearby low-luminosity events (which are also associated with spectroscopic supernovae) in terms of energetics and observed redshift distribution, indicating a continuous distribution overall.

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Section: B2 Details On the Swift-era Golden Samplementioning

confidence: 81%

Section: B2 Details On the Swift-era Golden Samplementioning

confidence: 99%

THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

Канн

Klose

Zhang

et al. 2010

ApJ

287

356

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“…ROTSE‐IIIb, located at McDonald Observatory, Texas, responded to GRB 080310 and began imaging 5.7 s after the Gamma‐ray Coordinates Network (GCN) notice time (Yuan et al 2008). Observations were carried out under fluctuating weather conditions.…”

Section: Observationsmentioning

confidence: 99%

The origin of the early-time optical emission of Swift GRB 080310★

Littlejohns¹,

Willingale²,

O’Brien³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present broad‐band multiwavelength observations of GRB 080310 at redshift z= 2.43. This burst was bright and long‐lived, and unusual in having extensive optical and near‐infrared (IR) follow‐up during the prompt phase. Using these data we attempt to simultaneously model the gamma‐ray, X‐ray, optical and IR emission using a series of prompt pulses and an afterglow component. Initial attempts to extrapolate the high‐energy model directly to lower energies for each pulse reveal that a spectral break is required between the optical regime and 0.3 keV to avoid overpredicting the optical flux. We demonstrate that afterglow emission alone is insufficient to describe all morphology seen in the optical and IR data. Allowing the prompt component to dominate the early‐time optical and IR and permitting each pulse to have an independent low‐energy spectral indices we produce an alternative scenario which better describes the optical light curve. This, however, does not describe the spectral shape of GRB 080310 at early times. The fit statistics for the prompt‐ and afterglow‐dominated models are nearly identical making it difficult to favour either. However one enduring result is that both models require a low‐energy spectral index consistent with self‐absorption for at least some of the pulses identified in the high‐energy emission model.

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GRB 081008: From Burst to Afterglow and the Transition Phase in Between

Yuan¹,

Schady²,

Racusin³

et al. 2010

ApJ

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We present a multi-wavelength study of GRB 081008, at redshift 1.967, by Swift, ROTSE-III and GROND. Compared to other Swift GRBs, GRB 081008 has a typical gamma-ray isotropic equivalent energy output (∼ 10 53 erg) during the prompt phase, and displayed two temporally separated clusters of pulses. The early X-ray emission seen by the Swift/XRT was dominated by the softening tail of the prompt emission, producing multiple flares during and after the Swift/BAT detections. Optical observations that started shortly after the first active phase of gamma-ray emission showed two consecutive peaks. We interpret the first optical peak as the onset of the afterglow associated with the early burst activities. A second optical peak, coincident with the later gamma-ray pulses, imposes a small modification to the otherwise smooth lightcurve and thus suggests a minimal contribution from a probable internal component. We suggest the early optical variability may be from continuous energy injection into the forward shock front by later shells producing the second epoch of burst activities. These early observations thus provide a potential probe for the transition from prompt to the afterglow phase. The later lightcurve of GRB 081008 displays a smooth steepening in all optical bands and X-ray. The temporal break is consistent with being achromatic at the observed wavelengths. Our broad energy coverage shortly after the break constrains a spectral break within optical. However, the evolution of the break frequency is not observed. We discuss the plausible interpretations of this behavior.

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Prompt optical observations of GRB 080330 and GRB 080413A

Cited by 6 publications

References 5 publications

THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

The origin of the early-time optical emission of Swift GRB 080310★

GRB 081008: From Burst to Afterglow and the Transition Phase in Between

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