Swift observations of GRB 050712

Pasquale, M. de; Grupe, D.; Poole, T.; Breeveld, A. A.; Zane, S.; Rosen, S. R.; Page, M. J.; Mason, K. O.; Burrows, D. N.; Krimm, H. A.; Gehrels, N.; Nousek, J. A.; Roming, P. W. A.; Kobayashi, S.; Zhang, Bing

doi:10.1111/j.1365-2966.2006.10609.x

Cited by 6 publications

(5 citation statements)

References 44 publications

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“…The power-law model shows that there is a decrease in the absorption column density by a factor of 4 from the beginning of the observation at 131 s after the burst to 300 s after the burst. Such decreases in the absorption column density have been observed before in GRB afterglows (e.g., in GRB 050712;De Pasquale et al 2006;Lazzati & Perna 2002) but have been usually linked to a flattening of the X-ray spectral slope. This is typically an artifact of the spectral fitting routine, which may be due to the correlation between spectral parameters such as N H and X .…”

Section: Spectra Analysis Of the Early-time Datamentioning

confidence: 69%

“…Such decreases in the absorption column density have been observed before in GRB afterglows, like e.g. in GRB 050712 (De Pasquale et al 2006;Lazzati & Perna 2002), but have been usually linked to a flattening of the X-ray spectral slope. This is typically an artifact of the spectral fitting routine, that may be due to the correlation between spectral parameters such as N H and β X .…”

Section: Spectra Analysis Of the Early Time Datamentioning

confidence: 71%

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SwiftandXMM‐NewtonObservations of the Extraordinary Gamma‐Ray Burst 060729: More than 125 Days of X‐Ray Afterglow

Grupe

Grönwall

Wang

et al. 2007

ApJ

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106

109

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We report the results of the Swift and XMM-Newton observations of the Swift-discovered GRB 060729 (T 90 ¼ 115 s). The afterglow of this burst was exceptionally bright in X-rays as well as at UV/optical wavelengths, showing an unusually long slow decay phase (¼ 0:14 AE 0:02), suggesting a larger energy injection phase at early times than in other bursts. The X-ray light curve displays a break at about 60 ks after the burst. The X-ray decay slope after the break is ¼ 1:29 AE 0:03. Up to 125 days after the burst we do not detect a jet break, suggesting that the jet opening angle is larger than 28. We find that the X-ray spectra of the early phase change dramatically and can all be fitted by an absorbed singleYpower-law models or alternatively by a blackbody plus power-law model. The power-law fits show that the X-ray spectrum becomes steeper while the absorption column density decreases. In the blackbody model the temperature decreases from kT ¼ 0:6 to 0.1 keV between 85 and 160 s after the burst in the rest frame. The afterglow was clearly detected up to 9 days after the burst in all six UVOT filters and in UVW1 even for 31 days. A break at about 50 ks is clearly detected in all six UVOT filters from a shallow decay slope of about 0.3 and a steeper decay slope of 1.3.The XMM-Newton observations started about 12 hr after the burst and show a typical afterglow X-ray spectrum with X ¼ 1:1 and absorption column density of 1 ; 10 21 cm À2 .

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Section: Spectra Analysis Of the Early-time Datamentioning

confidence: 69%

Section: Spectra Analysis Of the Early Time Datamentioning

confidence: 71%

SwiftandXMM‐NewtonObservations of the Extraordinary Gamma‐Ray Burst 060729: More than 125 Days of X‐Ray Afterglow

Grupe

Grönwall

Wang

et al. 2007

ApJ

Self Cite

106

109

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“…-Shallow decay phase (II): Typically with a temporal decay slope ∼ −0.5 or flatter extending to ∼ (10 3 − 10 4 )s, at which a temporal break is observed before the normal decay phase (e.g. Campana et al 2005;De Pasquale et al 2006). There is no spectral evolution across the break.…”

Section: A Canonical Lightcurve Of X-ray Afterglowsmentioning

confidence: 99%

“…This is different from the requirement of the ana-lytical pulsar model (q = 0). However, numerical calculations suggest that a pulsar model can fit some of the XRT lightcurves De Pasquale et al 2006;Yu & Dai 2006). -Energy injection from the ejecta with a wide Γdistribution.…”

Section: Shallow Decay Phase: Still a Mysterymentioning

confidence: 99%

Gamma-ray burst afterglows

Zhang

2007

Advances in Space Research

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Extended, fading emissions in multi-wavelength are observed following Gamma-ray bursts (GRBs). Recent broad-band observational campaigns led by the Swift Observatory reveal rich features of these GRB afterglows. Here we review the latest observational progress and discuss the theoretical implications for understanding the central engine, composition, and geometric configuration of GRB jets, as well as their interactions with the ambient medium.Comment: References added, accepted for publication in Advances in Space Researc

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“…Flares in the early light curve of the short GRBs 050724 (Barthelmy et al 2005b;Campana et al 2006;Grupe et al 2006), 051210 (La Parola et al 2006, and 060121 (Levan et al 2006) have also been seen. Flaring in GRBs has been attributed to long-lasting activity by the central engine with internal shocks continuing for hundreds of seconds (Burrows et al 2005c;Falcone et al 2006aFalcone et al , 2006bPagani et al 2006c;Zhang et al 2006;De Pasquale et al 2006). Although the decay slope of GRB 060313 is consistent with GRBs 050509B, 050709, and 051221A, no early flaring was seen in these three bursts (Fox et al [2005] report the possibility of a flare at early times for GRB 050709; however, the fitting of the light curve at early times was difficult since only one data point was available in the first day after the burst).…”

Section: Afterglowmentioning

confidence: 99%

GRB 060313: A New Paradigm for Short‐Hard Bursts?

Roming

Berk

Pal'Shin

et al. 2006

ApJ

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We report the simultaneous observations of the prompt emission in the gamma-ray and hard X-ray bands by the Swift BAT and the Konus-Wind instruments of the short-hard burst, GRB 060313. The observations reveal multiple peaks in both the gamma-ray and hard X-ray bands suggesting a highly variable outflow from the central explosion. We also describe the early-time observations of the X-ray and UV/optical afterglows by the Swift XRT and UVOT instruments. The combination of the X-ray and UV/optical observations provides the most comprehensive light curves to date of a short-hard burst at such an early epoch. The afterglows exhibit complex structure with different decay indices and flaring. This behavior can be explained by the combination of a structured jet, radiative loss of energy, and decreasing microphysics parameters occurring in a circumburst medium with densities varying by a factor of approximately two on a length scale of 10 17 cm. These density variations are normally associated with the environment of a massive star and inhomogeneities in its windy medium. However, the mean density of the observed medium (n $ 10 À4 cm 3) is much less than that expected for a massive star. Although the collapse of a massive star as the origin of GRB 060313 is unlikely, the merger of a compact binary also poses problems for explaining the behavior of this burst. Two possible suggestions for explaining this scenario are that some short bursts may arise from a mechanism that does not invoke the conventional compact binary model, or that soft late-time central engine activity is producing UV/optical but no X-ray flaring.

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Swift observations of GRB 050712

Cited by 6 publications

References 44 publications

SwiftandXMM‐NewtonObservations of the Extraordinary Gamma‐Ray Burst 060729: More than 125 Days of X‐Ray Afterglow

SwiftandXMM‐NewtonObservations of the Extraordinary Gamma‐Ray Burst 060729: More than 125 Days of X‐Ray Afterglow

Gamma-ray burst afterglows

GRB 060313: A New Paradigm for Short‐Hard Bursts?

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