Early re-brightening of the afterglow of GRB 050525a

Klotz, A.; Boër, M.; Atteia, J. L.; Stratta, G.; Behrend, R.; Malacrino, F.; Damerdji, Y.

doi:10.1051/0004-6361:200500153

Cited by 42 publications

(36 citation statements)

References 17 publications

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“…ac Followed by a plateau phase . ad Later followed by a plateau phase (Klotz et al 2005b). ae Long, slow rollover preceded by early complex variability.…”

Section: Results From Sed Fitting: Low Host Extinctions At High Redshmentioning

confidence: 99%

“…An early reverse-shock component has been proposed for GRB 050525A (Klotz et al 2005b;Shao & Dai 2005); this is also an interpretation for the early steep decay of GRB 061126 (Perley et al 2008c) and GRB 060908 (Covino et al 2010). In the case of GRB 051111, an early steep decay is associated with the tail of the prompt emission (Yost et al 2007a;Butler et al 2006).…”

Section: The Luminosity Distribution At Early Times: Diversity and CLmentioning

confidence: 92%

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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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“…ac Followed by a plateau phase . ad Later followed by a plateau phase (Klotz et al 2005b). ae Long, slow rollover preceded by early complex variability.…”

Section: Results From Sed Fitting: Low Host Extinctions At High Redshmentioning

confidence: 99%

Section: The Luminosity Distribution At Early Times: Diversity and CLmentioning

confidence: 92%

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

View full text Add to dashboard Cite

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“…Nysewander et al (2005) subsequently provided revised coordinates for the object of Haislip et al (2005a), showing it was coincident with our candidate. The afterglow was also detected by the TAROT robotic telescope up to eight minutes after the GRB (Klotz et al 2005). Data reduction was carried out following standard procedures.…”

Section: Observations and Data Analysismentioning

confidence: 99%

GRB 050904 at redshift 6.3: observations of the oldest cosmic explosion after the Big Bang

Tagliaferri¹,

Antonelli²,

Chincarini³

et al. 2005

A&A

103

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We present optical and near-infrared observations of the afterglow of the gamma-ray burst GRB 050904. We derive a photometric redshift z = 6.3, estimated from the presence of the Lyman break falling between the I and J filters. This is by far the most distant GRB known to date. Its isotropic-equivalent energy is 3.4 × 10 53 erg in the rest-frame 110−1100 keV energy band. Despite the high redshift, both the prompt and the afterglow emission are not peculiar with respect to other GRBs. We find a break in the J-band light curve at t b = 2.6 ± 1.0 d (observer frame). If we assume this is the jet break, we derive a beaming-corrected energy E γ ∼ (4 ÷ 12) × 10 51 erg. This limit shows that GRB 050904 is consistent with the Amati and Ghirlanda relations. This detection is consistent with the expected number of GRBs at z > 6 and shows that GRBs are a powerful tool to study the star formation history up to very high redshift.

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“…We finally note that there are several sources that exhibit optical light curves analogous to GRB 061121, that is, GRB 021004 (Uemura et al 2002), GRB 050525A (Klotz et al 2005;Blustin et al 2006), GRB 060117 (Jelínek et al 2006), GRB 060526 (Dai et al 2007), and GRB 061007 (Mundell et al 2007). For all of them, an early decay phase was terminated by a flattening or a hump at 10 2−4 s, which was followed by a steeper decay phase.…”

Section: Implication To the Synchrotron-shock Modelmentioning

confidence: 83%

“…Krühler et al (2009) report on optical-IR and X-ray light curves of GRB 080710, in which an achromatic break was observed. Blustin et al (2006) report another example of a possible achromatic break in GRB 050525A, while X-ray flares make it difficult to accurately determine a break time (also see, Klotz et al 2005). In some of past cases, optical observations were too sparse to determine break times and to capturethe detailed behavior on either side of the breaks.…”

Section: Introductionmentioning

confidence: 99%

Optical behavior of GRB 061121 around its X-Ray shallow decay phase

Uehara

Uemura

Arai

et al. 2011

A&A

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Aims. We report on a detailed study of the optical afterglow of GRB 061121 with our original time-series photometric data. Along with our optical observations and public X-ray data, we discuss the origin of its optical and X-ray afterglows. Methods. We observed the optical afterglow of Swift burst GRB 061121 with the Kanata 1.5-m telescope at Higashi-Hiroshima Observatory. Our observation covers a period just after an X-ray plateau phase. We also performed deep imaging with the Subaru telescope in 2010 in order to estimate the contamination by the host galaxy. Results. In the light curve, we find that the optical afterglow also exhibited a break as in the X-ray afterglow. However, our observation suggests a possible hump structure or a flattening period before the optical break in the light curve. There is no sign of such a hump in the X-ray light curve. Conclusions. This implies that the optical emitting region was distinct from the X-ray one. The hump in the optical light curve was possibly caused by a passage with the typical frequency of synchrotron emission from another forward shock distinct from the early afterglow. The observed decay and spectral indices are inconsistent with the standard synchrotron-shock model. As a results, the observation requires a change in microphysical parameters in the shock region or prior activity by the central engine. Alternatively, the emission during the shallow decay phase may be a composition of two forward shock emissions, as indicated by the hump structure in the light curve.

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Early re-brightening of the afterglow of GRB 050525a

Cited by 42 publications

References 17 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

GRB 050904 at redshift 6.3: observations of the oldest cosmic explosion after the Big Bang

Optical behavior of GRB 061121 around its X-Ray shallow decay phase

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