GRB 090902b: Afterglow Observations and Implications

Swenson, C. A.; Perley, D.; Guidorzi, C.; Wiersema, K.; Malesani, D.; Akerlof, C.; Ashley, M. C. B.; Bersier, D.; Cano, Z.; Gomboc, A.; Ilyin, I.; Jakobsson, P.; Kleiser, I. K. W.; Kobayashi, S.; Kouveliotou, C.; Levan, A. J.; McKay, T. A.; Melandri, A.; Mottram, Chris; Mundell, C. G.; O’Brien, P. T.; Phillips, A.; Rex, J.; Siegel, M. H.; Smith, R. J.; Steele, I. A.; Stratta, G.; Tanvir, N. R.; Weights, D. J.; Yost, S. A.; Yuan, F.; Zheng, W.

doi:10.1088/0004-637x/714/1/799

Cited by 37 publications

(38 citation statements)

References 52 publications

(61 reference statements)

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“…It is the first Fermi GRB for which the afterglow was detected (by ROTSE) before the LAT position (or a Swift XRT position) was published, by mosaicing the GBM ground position. This detection shows the afterglow was probably dominated in the first hours by a reverse-shock flash (Pandey et al 2010). We find α RS > 1.8, α 1 = 0.96±0.02, t b < 0.46 days.…”

Section: B2 Details On the Swift-era Golden Samplesupporting

confidence: 48%

“…We constructed the light curve and the SED with data from the following sources: McBreen et al (2010), Pandey et al (2010), and Cenko et al (2010b). This extremely energetic GRB has the third-highest fluence of all GRBs in the Swift era, featured the highest observed energy ever for a GeV photon, and shows a highenergy spectrum consisting of a superposition of a Band function and a power-law rising to GeV energies which also dominates below 50 keV (Abdo et al 2009b).…”

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

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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 Samplesupporting

confidence: 48%

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

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287

356

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“…We note the publication of three relevant papers since the submission of this paper: Pandey et al (2010), Rau et al (2010) and Cenko et al (2010b).…”

Section: Acknowledgements Based On Observations Made With Eso Telescmentioning

confidence: 95%

Optical and near-infrared follow-up observations of fourFermi/LAT GRBs: redshifts, afterglows, energetics, and host galaxies

McBreen

Krühler

Rau

et al. 2010

A&A

114

100

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Aims. Fermi can measure the spectral properties of gamma-ray bursts over a very large energy range and is opening a new window on the prompt emission of these energetic events. Localizations by the instruments on Fermi in combination with follow-up by Swift provide accurate positions for observations at longer wavelengths leading to the determination of redshifts, the true energy budget, host galaxy properties and facilitate comparison with pre-Fermi bursts. Methods. Multi-wavelength follow-up observations were performed on the afterglows of four bursts with high energy emission detected by Fermi/LAT: GRB 090323, GRB 090328, GRB 090510 and GRB 090902B. They were obtained in the optical/near-infrared bands with GROND mounted at the MPG/ESO 2.2 m telescope and additionally of GRB 090323 in the optical with the 2 m telescope in Tautenburg, Germany. Three of the events are classified as long bursts while GRB 090510 is a well localized short GRB with GeV emission. In addition, host galaxies were detected for three of the four bursts. Spectroscopic follow-up was initiated with the VLT for GRB 090328 and GRB 090510. Results. The afterglow observations in 7 bands are presented for all bursts and their host galaxies are investigated. Knowledge of the distance and the local dust extinction enables comparison of the afterglows of LAT-detected GRBs with the general sample. The spectroscopic redshifts of GRB 090328 and GRB 090510 were determined to be z = 0.7354 ± 0.0003 and z = 0.903 ± 0.001 and dust corrected star-formation rates of 4.8 M yr −1 and 0.60 M yr −1 were derived for their host galaxies, respectively. Conclusions. The afterglows of long bursts exhibit power-law decay indices (α) from less than 1 to ∼2.3 and spectral indices (β opt ) values from 0.65 to ∼1.2 which are fairly standard for GRB afterglows. Constraints are placed on the jet half opening angles of < ∼ 2.1 • to > ∼ 6.4 • , which allows limits to be placed on the beaming corrected energies. These range from < ∼ 5 × 10 50 erg to the one of the highest values ever recorded, > ∼ 2.2 × 10 52 erg for GRB 090902B, and are not consistent with a standard candle. The extremely energetic long Fermi bursts have optical afterglows which lie in the top half of the brightness distribution of all optical afterglows detected in the Swift era or even in the top 5% if incompleteness is considered. The properties of the host galaxies of these LAT detected bursts in terms of extinction, star formation rates and masses do not appear to differ from previous samples.

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“…For instance, for the case of GRB 060117 (Jelinek et al 2006) and GRB 090902B (Pandey et al 2010), a bright afterglow and a decay slope are suggestive of a reverse shock origin.…”

Section: The Reverse Shock Emissionmentioning

confidence: 99%

Multiwavelength observations of GRB afterglows

Castro-Tirado

2011

Proc. IAU

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Abstract. Multiwavelength observations of gamma-ray burst afterglows are presented, in particular those in the optical and millimetre wavelengths. I will focus on the observations mostly carried out at Spanish ground-based observatories (mainly the 10.4m GTC) and at the Plateau de Bure Interferometer in the French Alps. The importance of global networks of robotic telescopes (like BOOTES, established worldwide) for early time observations in order to put constraints on the physical mechanisms of the GRB early time emission phase is also discussed. The overall observational efforts provide additional clues for a better understanding of the reverse and forward shock. Finally I will report on the Lomonosov/UFFO-p capabilities taking into account its launch in 2012.

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GRB 090902b: Afterglow Observations and Implications

Cited by 37 publications

References 52 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

Optical and near-infrared follow-up observations of fourFermi/LAT GRBs: redshifts, afterglows, energetics, and host galaxies

Multiwavelength observations of GRB afterglows

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