Very Early Optical Afterglows of Gamma‐Ray Bursts: Evidence for Relative Paucity of Detection

Roming, P. W. A.; Schady, P.; Fox, D. B.; Zhang, Bing; Liang, En‐Wei; Mason, K. O.; Rol, E.; Burrows, D. N.; Blustin, A. J.; Boyd, Patricia T.; Brown, P. J.; Holland, S. T.; McGowan, K.; Landsman, W. B.; Page, K. L.; Rhoads, James E.; Rosen, S. R.; Berk, Daniel Vanden; Barthelmy, S. D.; Breeveld, A. A.; Cucchiara, Antonino; Pasquale, M. de; Fenimore, E. E.; Gehrels, N.; Grönwall, C.; Grupe, D.; Goad, M. R.; Ivanushkina, M.; James, Cynthia H.; Kennea, J. A.; Kobayashi, S.; Mangano, V.; Mészáros, P.; Morgan, A. N.; Nousek, J. A.; Osborne, J. P.; Palmer, D. M.; Poole, T.; Still, M.; Tagliaferri, G.; Zane, S.

doi:10.1086/508481

Cited by 79 publications

(59 citation statements)

References 68 publications

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“…The lack of reverse shock (see e.g. Mundell et al 2007;Jin & Fan 2007) confirms the general results for Swift GRBs obtained by the UVOT (Roming et al 2006). These (lack of) findings impose severe constraints on the micro-physics parameters of the relativistic shocks or suggest alternatively that additional ingredients, such as magnetically dominated outflows, are required (Lyutikov et al 2003;Fan et al 2004;Zhang & Kobayashi 2005).…”

Section: Introductionsupporting

confidence: 79%

“…At variance with the expectations from the pre-Swift era, most Swift GRB afterglows indeed do not show reverse-shock emission (Roming et al 2006). Based on the already decaying phase of the afterglow at about 1 min after the GRB, we can derive a rough estimate of the initial Lorentz factor as Γ 0 ∼ 500 under the same conditions discussed earlier.…”

Section: The Early Afterglowmentioning

confidence: 46%

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Challenging gamma-ray burst models through the broadband dataset of GRB 060908

Covino¹,

Campana²,

Conciatore

et al. 2010

A&A

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Context. Multiwavelength observations of gamma-ray burst prompt and afterglow emission are a key tool to separate the various possible emission processes and scenarios proposed to interpret the complex gamma-ray burst phenomenology. Aims. We collected a large dataset on GRB 060908 in order to carry out a comprehensive analysis of the prompt emission as well as the early and late afterglow. Methods. Data from Swift-BAT, -XRT and -UVOT together with data from a number of different ground-based optical/near-infrared and millimeter telescopes allowed us to follow the afterglow evolution after about a minute from the high-energy event down to the host galaxy limit. We discuss the physical parameters required to model these emissions. Results. The prompt emission of GRB 060908 was characterised by two main periods of activity, spaced by a few seconds of low intensity, with a tight correlation between activity and spectral hardness. Observations of the afterglow began less than one minute after the high-energy event, when it was already in a decaying phase, and it was characterised by a rather flat optical/near-infrared spectrum which can be interpreted as due to a hard energy-distribution of the emitting electrons. On the other hand, the X-ray spectrum of the afterglow could be fit by a rather soft electron distribution. Conclusions. GRB 060908 is a good example of a gamma-ray burst with a rich multi-wavelength set of observations. The availability of this dataset, built thanks to the joint efforts of many different teams, allowed us to carry out stringent tests for various interpretative scenarios, showing that a satisfactorily modelling of this event is challenging. In the future, similar efforts will enable us to obtain optical/near-infrared coverage comparable in quality and quantity to the X-ray data for more events, therefore opening new avenues to progress gamma-ray burst research.

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Section: Introductionsupporting

confidence: 79%

Section: The Early Afterglowmentioning

confidence: 46%

Challenging gamma-ray burst models through the broadband dataset of GRB 060908

Covino¹,

Campana²,

Conciatore

et al. 2010

A&A

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show abstract

“…emission component (Roming et al 2006, Kann et al 2010. This fact provides observational support that the strength of the optical emission from the RS may be weaker than previously calculated, or that the RS is not radiated in the optical wavelength regime.…”

Section: Optical and Near-infrared Flares In Grb Afterglowssupporting

confidence: 74%

Optical and near-infrared flares in GRB afterglows

Krühler

2011

Proc. IAU

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Abstract. Among the diversities in the very early evolution of GRB afterglows are bright optical/near-infrared flares before or superimposed onto an otherwise smoothly decaying afterglow light curve. A lot has been learned about GRBs by using an optical flare or lack thereof as a diagnostic of the emission mechanisms and outflow conditions. In this contribution I will review the observational properties of rising and decaying light-curves in GRB afterglows, discuss their possible physical origins, and highlight in which way they help in understanding GRB and afterglows physics.

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“…Furthermore, in the Swift era, many optical afterglows are discovered first by the Swift UV/optical telescope which has only filters up to the v band precluding the rapid localisation of z > ∼ 5 or of highly extinguished afterglows (cf. Roming et al 2006). Needing only Swift XRT localisations, IFS is basically not affected by this colour-selection bias.…”

Section: Introductionmentioning

confidence: 98%

GRB 060605: multi-wavelength analysis of the first GRB observed using integral field spectroscopy

Ferrero¹,

Klose²,

Канн³

et al. 2009

A&A

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The long and relatively faint gamma-ray burst GRB 060605 detected by Swift/BAT lasted about 20 s. Its afterglow could be observed with Swift/XRT for nearly 1 day, while Swift/UVOT could detect the afterglow during the first 6 h after the event. Here, we report on integral field spectroscopy of its afterglow performed with PMAS/PPak mounted at the Calar Alto 3.5 m telescope. In addition, we report on a detailed analysis of XRT and UVOT data and on the results of deep late-time VLT observations that reveal the GRB host galaxy. We find that the burst occurred at a redshift of z = 3.773, possibly associated with a faint, R C = 26.4 ± 0.3 host. Based on the optical and X-ray data, we deduce information on the SED of the afterglow, the position of the cooling frequency in the SED, the nature of the circumburst environment, its collimation factor, and its energetics. We find that the GRB fireball was expanding into a constant-density medium and that the explosion was collimated with a narrow half-opening angle of about 2.4 degrees. The initial Lorentz factor of the fireball was about 250; however, its beaming-corrected energy release in the gamma-ray band was comparably low. The optical, X-ray afterglow, on the other hand, was rather luminous. Finally, we find that the data are consistent within the error bars with an achromatic evolution of the afterglow during the suspected jet break time at about 0.27 days after the burst.

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Very Early Optical Afterglows of Gamma‐Ray Bursts: Evidence for Relative Paucity of Detection

Cited by 79 publications

References 68 publications

Challenging gamma-ray burst models through the broadband dataset of GRB 060908

Challenging gamma-ray burst models through the broadband dataset of GRB 060908

Optical and near-infrared flares in GRB afterglows

GRB 060605: multi-wavelength analysis of the first GRB observed using integral field spectroscopy

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