Early‐Time Observations of the GRB 050319 Optical Transient

Rykoff, E. S.; Aharonian, F.; Akerlof, C.; Alatalo, Katherine; Ashley, M. C. B.; Güver, T.; Horns, D.; Kehoe, R.; Kızıloğlu, Ü.; McKay, T. A.; Özel, M. E.; Phillips, A.; Quimby, R.; Schaefer, Bradley E.; Smith, D. A.; Swan, H.; Vestrand, W. T.; Wheeler, J. C.; Wren, J.; Yost, S. A.; Göǧüş, E.

doi:10.1086/499803

Cited by 46 publications

(60 citation statements)

References 14 publications

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“…In this case, the optical emission showed a temporal variability correlated with the gamma-ray emission, suggesting a common origin for the two components. The prompt afterglows of GRB 050319 (Quimby et al 2006;Woźniak et al 2005) and GRB 050401 (Rykoff et al 2005) showed a decay matching the late-time one, without the need for extra components. Last, GRB 050801 ) showed a period of plateaux up to a few minutes after the burst, excluding contribution from the internal shocks, but possibly arguing for energisation from the central engine correlated with the X-ray emission.…”

Section: Introductionmentioning

confidence: 78%

Panchromatic study of GRB 060124: from precursor to afterglow

Romano¹,

Campana²,

Chincarini

et al. 2006

A&A

216

173

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We present observations of GRB 060124, the first event for which both the prompt and the afterglow emission could be observed simultaneously and in their entirety by the three Swift instruments. Indeed, Swift-BAT triggered on a precursor ∼570 s before the main burst peak, and this allowed Swift to repoint the narrow field instruments to the burst position ∼350 s before the main burst occurred. GRB 060124 also triggered Konus-Wind, which observed the prompt emission in a harder gamma-ray band (up to 2 MeV). Thanks to these exceptional circumstances, the temporal and spectral properties of the prompt emission can be studied in the optical, X-ray and gamma-ray ranges. While the X-ray emission (0.2-10 keV) clearly tracks the gamma-ray burst, the optical component follows a different pattern, likely indicating a different origin, possibly the onset of external shocks. The prompt GRB spectrum shows significant spectral evolution, with both the peak energy and the spectral index varying. As observed in several long GRBs, significant lags are measured between the hard-and low-energy components, showing that this behaviour extends over 3 decades in energy. The GRB peaks are also much broader at soft energies. This is related to the temporal evolution of the spectrum, and can be accounted for by assuming that the electron spectral index softened with time. The burst energy (E iso ∼ 5 × 10 53 erg) and average peak energy (E p ∼ 300 keV) make GRB 060124 consistent with the Amati relation. The X-ray afterglow is characterized by a decay which presents a break at t b ∼ 10 5 s.

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Section: Introductionmentioning

confidence: 78%

Panchromatic study of GRB 060124: from precursor to afterglow

Romano¹,

Campana²,

Chincarini

et al. 2006

A&A

216

173

View full text Add to dashboard Cite

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“…When observed, the ratio of the correlated γ-ray to optical flux densities has been found to be roughly 10 5 to one. In contrast to bursts with γ-ray correlated emission, the common burst is now revealed to either exhibit a single power-law decay from early times (Rykoff et al 2005b, Quimby et al 2006a), or to exhibit a flat or rising (Rykoff et al 2004a or rebrightening (Stanek et al 2007) optical light curve before it enters the standard power-law afterglow decay. The initial brightness of the typical counterpart is V ∼ 14 to 17 mag 3 (Roming et al 2009), which has made observations challenging for smaller (<1 m) robotic facilities, and has limited the extent of the lightcurves collected by the UVOT.…”

Section: Optical Observationsmentioning

confidence: 93%

Gamma-Ray Bursts in theSwiftEra

Gehrels

Ramírez-Ruiz

Fox

2009

Annu. Rev. Astron. Astrophys.

588

474

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With its rapid-response capability and multiwavelength complement of instruments, the Swift satellite has transformed our physical understanding of γ-ray bursts (GRBs). Providing highquality observations of hundreds of bursts, and facilitating a wide range of follow-up observations within seconds of each event, Swift has revealed an unforeseen richness in observed burst properties, shed light on the nature of short-duration bursts, and helped realize the promise of GRBs as probes of the processes and environments of star formation out to the earliest cosmic epochs. These advances have opened new perspectives on the nature and properties of burst central engines, interactions with the burst environment from microparsec to gigaparsec scales, and the possibilities for nonphotonic signatures. Our understanding of these extreme cosmic sources has thus advanced substantially; yet, more than 40 years after their discovery, GRBs continue to present major challenges on both observational and theoretical fronts.

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“…Such an event had already been observed in at least two other cases: GRB 060218A (z = 0.03) 1000 s after the GRB [66], and GRB 060729 (z = 0.54) 450 s after the GRB [67,68]. Note that the Figure 3: Observations of GRB 050824 from the MASTER telescope and the MDM Observatory (R) [56].…”

Section: The Short Burst Grb 051103 -A Soft Gamma-ray Repeater In Thementioning

confidence: 89%

“…5). Comparison of the light curve of GRB 060926 obtained using the MASTER telescope [63] (points) with the (a) OPTIMA Burst [64] (circles) and (b) SWIFT XRT (0.3.10 keV; diamonds) [65] light curves.…”

Section: Optical Emission Of Grbs In the First Hour After The Burstmentioning

confidence: 99%

Optical observations of gamma-ray bursts, the discovery of supernovae 2005bv, 2005ee, and 2006ak, and searches for transients using the “MASTER” robotic telescope

et al. 2007

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We present the results of observations obtained using the MASTER robotic telescope in 2005 -2006, including the earliest observations of the optical emission of the gamma-ray bursts GRB 050824 and GRB 060926. Together with later observations, these data yield the brightness-variation law t −0.55±0.05 for GRB 050824. An optical flare was detected in GRB 060926 -a brightness enhancement that repeated the behavior observed in the X-ray variations. The spectrum of GRB 060926 is found to be F E ≈ E −β , where β = 1.0 ± 0.2. Limits on the optical brightnesses of 26 gamma-ray bursts have been derived, 9 of these for the first time. Data for more than 90% of the accessible sky down to 19 m were taken and reduced in real time during the survey. A database has been composed based on these data. Limits have been placed on the rate of optical flares that are not associated with detected gamma-ray bursts, and on the opening angle for the beams of gamma-ray bursts. Three new supernovae have been discovered: SN 2005bv (type Ia) -the first to be discovered on Russian territory, SN 2005ee -one of the most powerful type II supernovae known, and SN 2006ak (type Ia). We have obtained an image of SN 2006X during the growth stage and a light curve that fully describes the brightness maximum and exponential decay. A new method for searching for optical transients of gamma-ray bursts detected using triangulation from various spacecraft is proposed and tested.

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Early‐Time Observations of the GRB 050319 Optical Transient

Cited by 46 publications

References 14 publications

Panchromatic study of GRB 060124: from precursor to afterglow

Panchromatic study of GRB 060124: from precursor to afterglow

Gamma-Ray Bursts in theSwiftEra

Optical observations of gamma-ray bursts, the discovery of supernovae 2005bv, 2005ee, and 2006ak, and searches for transients using the “MASTER” robotic telescope

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