A photometric redshift of z = 6.39 ± 0.12 for GRB 050904

Haislip, J.; Nysewander, M.; Reichart, D.; Levan, A. J.; Tanvir, N. R.; Cenko, S. B.; Fox, D. B.; Price, P. A.; Castro-Tirado, A. J.; Gorosabel, J.; Evans, Charles R.; Figuerêdo, E.; MacLeod, Chelsea L.; Kirschbrown, J.; Jelínek, M.; Guziy, S.; Postigo, A. de Ugarte; Cypriano, E. S.; Lacluyzé, A.; Graham, James R.; Priddey, R.; Chapman, R. W.; Rhoads, James E.; Fruchter, A. S.; Lamb, D. Q.; Kouveliotou, C.; Wijers, R. A. M. J.; Bayliss, M.; Schmidt, B.; Söderberg, A. M.; Kulkarni, S. R.; Harrison, Fiona A.; Moon, Dae‐Sik; Gal‐Yam, A.; Kasliwal, M. M.; Hudec, R.; Vítek, Stanislav; Kubánek, P.; Crain, J. A.; Foster, Antonina; Clemens, J. C.; Bartelme, J. W.; Canterna, R.; Hartmann, D. H.; Henden, A. A.; Klose, S.; Park, H. S.; Williams, G. G.; Rol, E.; O’Brien, P. T.; Bersier, D.; Prada, Francisco; Pizarro, S.; Maturana, D.; Ugarte, P.; Alvarez, Agustín O.; Fernandez, A. J. Melgarejo; Jarvis, Matt J.; Moles, M.; Alfaro, E. J.; Ivarsen, K.; Kumar, Naveen; Mack, Claude E.; Zdarowicz, C. M.; Gehrels, N.; Barthelmy, S. D.; Burrows, D. N.

doi:10.1038/nature04552

Cited by 112 publications

(127 citation statements)

References 15 publications

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“…On the upper part of the diagram, we identify a family of very luminous events, peaking at ∼10 33 erg s −1 Hz −1 , composed by GRB 980329 (Smith et al 1999;Jaunsen et al 2003), GRB 050904 (Tagliaferri et al 2005;Haislip et al 2006), GRB 080129 (Greiner et al 2009) and GRB 090313 (Melandri et al 2010), all beyond redshift 3. If those bursts were to be found at redshift of ∼1 they would reach peak fluxes of 40 mJy and easily over 100 mJy at redshifts of ∼0.5.…”

Section: Redshift Distribution and Luminositiesmentioning

confidence: 99%

“…13 we have drawn the SED of GRB 050904 at z = 6.3, including radio limits (Frail et al 2006), a detection in band 3 (and a limit in band 6) from Plateau de Bure Interferometer (CastroTirado et al, in prep. ), near-infrared and optical data (Tagliaferri et al 2005;Haislip et al 2006) and X-ray data from Swift. In spite of its high redshift, this burst was detected with a peak flux density of 1.47 mJy in band 3, 80 times above ALMA's detection threshold for 1 h of observations in band 3.…”

Section: Grb Afterglowsmentioning

confidence: 99%

“…SED of GRB 050904 at redshift z = 6.29 (Kawai et al 2006) using the detection from PdBI 5.896 days after the burst (Castro-Tirado et al, in prep.). The X-ray flux is estimated from the XRT light curve, the radio data are from Frail et al (2006), while optical/NIR are extrapolations from Tagliaferri et al (2005); Haislip et al (2006). For the rough synchrotron spectrum drawn in blue, we have assumed an electron energy distribution index of p = 2.30, while an SMC extinction with A V = 0.12 (consistent with the value derived by Stratta et al 2011; but see also Zafar et al 2010) and Lyman blanketing (Madau 1995) have been considered in the red dotted line to match the optical/NIR observations.…”

Section: Grb Host Galaxies With Almamentioning

confidence: 99%

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Pre-ALMA observations of GRBs in the mm/submm range

Postigo

Lundgren

Martín

et al. 2012

A&A

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Context. Gamma-ray bursts (GRBs) generate an afterglow emission that can be detected from radio to X-rays during days, or even weeks after the initial explosion. The peak of this emission crosses the millimeter and submillimeter range during the first hours to days, making their study in this range crucial for constraining the models. Observations have been limited until now due to the low sensitivity of the observatories in this range. This situation will be greatly improved with the start of scientific operations of the Atacama Large Millimeter/submillimeter Array (ALMA). Aims. In this work we do a statistical analysis of the complete sample of mm/submm observations of GRB afterglows obtained before the beginning of scientific operations at ALMA. Methods. We present observations of 11 GRB afterglows obtained from the Atacama Pathfinder Experiment (APEX) and the SubMillimeter Array (SMA), as well as the first detection of a GRB with ALMA, still in the commissioning phase, and put them into context with a catalogue of all the observations that have been published until now in the spectral range that is covered by ALMA.Results. The catalogue of mm/submm observations collected here is the largest to date and is composed of 102 GRBs, of which 88 have afterglow observations, whereas the rest are host galaxy searches. With our programmes, we contributed with data of 11 GRBs and the discovery of 2 submm counterparts. In total, the full sample, including data from the literature, has 22 afterglow detections with redshifts ranging from 0.168 to 8.2. GRBs have been detected in mm/submm wavelengths with peak luminosities spanning 2.5 orders of magnitude, the most luminous reaching 10 33 erg s −1 Hz −1 . We observe a correlation between the X-ray brightness at 0.5 days and the mm/submm peak brightness. Finally we give a rough estimate of the distribution of peak flux densities of GRB afterglows, based on the current mm/submm sample. Conclusions. Observations in the mm/submm bands have been shown to be crucial for our understanding of the physics of GRBs, but have until now been limited by the sensitivity of the observatories. With the start of the operations at ALMA, the sensitivity has improved by more than an order of magnitude, opening a new era in the study of GRB afterglows and their host galaxies. Our estimates predict that, once completed, ALMA will detect up to ∼98% of the afterglows if observed during the passage of the peak synchrotron emission.

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Section: Redshift Distribution and Luminositiesmentioning

confidence: 99%

Section: Grb Afterglowsmentioning

confidence: 99%

Section: Grb Host Galaxies With Almamentioning

confidence: 99%

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Pre-ALMA observations of GRBs in the mm/submm range

Postigo

Lundgren

Martín

et al. 2012

A&A

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“…Indeed, the majority of Swift GRB detections to date have been of the long-burst variety, and studies of the early afterglows, previously inaccessible, have added to evidence supporting the view that long-duration bursts are produced during the collapse of a massive star. Red shifts have now been measured for over 50 long bursts, including the first GRB at very high red shift (zO6; Cusumano et al 2006;Haislip et al 2006;Kawai et al 2006). These bursts are providing new ways to probe the high-red-shift universe (as reviewed by Ghirlanda 2007;Lamb 2007) and Tanvir & Jakobsson (2007) discuss conditions under which GRBs may be used as a tracer of the star formation rate in high-redshift galaxies.…”

Section: Observational Contributions From Swiftmentioning

confidence: 99%

Introduction: recent developments in the study of gamma-ray bursts

Wells

Wijers

Rees

2007

Phil. Trans. R. Soc. A.

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Gamma-ray bursts (GRBs) are immensely powerful explosions, originating at cosmological distances, whose outbursts persist for durations ranging from milliseconds to tens of seconds or more. In these brief moments, the explosions radiate more energy than the Sun will release in its entire 10 Gyr lifetime. Current theories attribute these phenomena to the final collapse of a massive star, or the coalescence of a binary system induced by gravity wave emission.New results from Swift and related programmes offer fresh understanding of the physics of GRBs, and of the local environments and host galaxies of burst progenitors. Bursts found at very high red shifts are new tools for exploring the intergalactic medium, the first stars and the earliest stages of galaxy formation.This Royal Society Discussion Meeting has brought together leading figures in the field, together with young researchers and students, to discuss and review the latest results from NASA's Swift Gamma-ray Burst Observatory and elsewhere, and to examine their impact on current understanding of the observed phenomena.

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“…These events are important to understand the formation of the first stars in the Universe. Proof that they can be detected in the mm/submm range is the fact that, out of the three GRB afterglows observed at z > 6, two have been detected (GRB 050904 at z = 6.3, Tagliaferri et al 2005, Haislip et al 2006, and GRB 090423 at z = 8.2, Tanvir et al 2009, Salvaterra et al 2009). …”

Section: Observations Of Individual Grbsmentioning

confidence: 99%

Observations of GRBs in the mm/submm range at the dawn of the ALMA era

et al. 2011

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Abstract. Gamma-ray bursts (GRBs) generate an afterglow with an emission peaking in the millimetre and submillimeter (mm/submm) range during the first hours to days, making the study in these wavelengths of great importance. Here we give an overview of the data that has been collected for GRB observations in this wavelengths until September 2011. The total sample includes 102 GRBs, of which 88 have afterglow observations, and the rest are only host galaxy searches. The 22 detections cover the redshift range between 0.168 and 8.2 and have peak luminosities that span 2.5 orders of magnitude. With the start of the operations at ALMA, the sensitivity with respect to previous facilities has already improved by over an order of magnitude. We estimate that, once completed, ALMA will be able to detect ∼98 % of the afterglows.This proceeding is based on the work published by de Ugarte Postigo et al. (2012).

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A photometric redshift of z = 6.39 ± 0.12 for GRB 050904

Cited by 112 publications

References 15 publications

Pre-ALMA observations of GRBs in the mm/submm range

Pre-ALMA observations of GRBs in the mm/submm range

Introduction: recent developments in the study of gamma-ray bursts

Observations of GRBs in the mm/submm range at the dawn of the ALMA era

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