Observational constraints on the afterglow of GRB 020531

Klotz, A.; Boër, M.; Atteia, J. L.

doi:10.1051/0004-6361:20030121

Cited by 42 publications

(47 citation statements)

References 24 publications

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“…The optical counterpart declined rapidly and rose again to a second peak of about 17.3 mag at about 300 seconds after the burst. The later observation is consistent with other optical detections of the afterglow reported in GCNs [8,2,9,10]. Fig.…”

Section: Rotse-iii: Introduction and Statussupporting

confidence: 92%

Prompt optical observations of GRB 080330 and GRB 080413A

Yuan

Rykoff

Schaefer

et al. 2008

AIP Conference Proceedings

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Abstract. We report on the results of rapid responses to GRB 080330 and GRB 080413A by the ROTSE-IIIb and ROTSEIIIc telecopes. In both cases, optical follow-up started during the prompt emission phase and recorded optical flares peaking at similar times as the last hard X-ray pulses detected by the Swift BAT. For both events, the XRT observations started at the end of the prompt BAT detection and displayed an evolution in time opposite to the optical lightcurve. These very early observations provide us an opportunity to probe the onset of afterglow for these two events.

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Section: Rotse-iii: Introduction and Statussupporting

confidence: 92%

Prompt optical observations of GRB 080330 and GRB 080413A

Yuan

Rykoff

Schaefer

et al. 2008

AIP Conference Proceedings

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“…We constructed the light curve and the SED with data from the following sources ), Yuan et al (2007b), Wang et al (2007, Klotz et al (2007), Burenin et al (2007), Chen et al (2007aChen et al ( , 2007b, Dintinjana et al (2007), Oates & Stratta (2007), Ishimura et al (2007b), Greco et al (2007), Sposetti (2007b), Yoshida et al (2007c), Uemura et al (2007b), Minezaki et al (2007), and Huang et al (2008a). This GRB afterglow was rapidly observed by many observatories on the western Pacific rim.…”

Section: B2 Details On the Swift-era Golden Samplementioning

confidence: 99%

“…We constructed the light curve and the SED with data from the following sources: Fynbo et al (2009), Klotz et al (2008a), Küpcü Yoldaş et al (2008, Brennan et al (2008), Updike et al (2008a), Perley et al (2008b), Grupe et al (2008), as well as one data point from the 1.5 m Sayan telescope. Data on this GRB are rather sparse.…”

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

289

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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“…No optical transient was found down to R > 15.4 in the first 60 s of observations. An upper limit of R > 15.8 could be set for any transient up to 382 s after the trigger (Klotz et al 2006). The Faulkes Telescope South started observing about 2.8 h after the event.…”

Section: A5 Grb 060919mentioning

confidence: 99%

A deep search for the host galaxies of gamma-ray bursts with no detected optical afterglow

Rossi

Klose

Ferrero

et al. 2012

A&A

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Context. Gamma-ray bursts (GRBs) can provide information about star formation at high redshifts. Even in the absence of a bright optical/nearinfrared/radio afterglow, the high detection rate of X-ray afterglows by Swift/XRT and its localization precision of 2-3 arcsec facilitates the identification and the study of GRB host galaxies. Aims. We focus on the search for the host galaxies of 17 bursts with arcsec-sized XRT error circles but no detected long-wavelength afterglow, in spite of their deep and rapid follow-up observations. Three of these events can also be classified as truly dark bursts, i.e., the observed upper limit on the optical flux of the afterglow was less than expected based on the measured X-ray flux. Our goals are to identify the GRB host galaxy candidates and characterize their phenomenological parameters. Methods. Our study is based on deep R C and K s -band observations performed with FORS1, FORS2, VIMOS, ISAAC, and HAWK-I at the ESO/VLT, partly supported by observations with the seven-channel imager GROND at the 2.2-m telescope on La Silla, and supplemented by observations with NEWFIRM at the 4-m telescope on Kitt Peak. To be conservative, we searched for host galaxy candidates within an area of twice the radius of each associated 90% c.l. Swift/XRT error circle. Results. For 15 of the 17 bursts, we find at least one galaxy within the searching area, and in the remaining two cases only a deep upper limit to R C and K s can be provided. In seven cases, we discover extremely red objects in the error circles, at least four of which might be dust-enshrouded galaxies. The most remarkable case is the host of GRB 080207, which has a color of (R C − K s ) AB ∼ 4.7 mag, and is one of the reddest galaxies ever associated with a GRB. As a by-product of our study we identify the optical afterglow of GRB 070517. Conclusions. Only a minority of optically dim afterglows are due to Lyman dropout ( 1/3). Extinction by dust in the host galaxies might explain all other events. Thereby, a seemingly non-negligible fraction of these hosts are globally dust-enshrouded, extremely red galaxies. This suggests that at least a fraction of GRB afterglows trace a subpopulation of massive starburst galaxies, which are markedly different from the main body of the GRB host galaxy population, namely the blue, subluminous, compact galaxies.

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Observational constraints on the afterglow of GRB 020531

Cited by 42 publications

References 24 publications

Prompt optical observations of GRB 080330 and GRB 080413A

Prompt optical observations of GRB 080330 and GRB 080413A

THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

A deep search for the host galaxies of gamma-ray bursts with no detected optical afterglow

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