GRB 090423 at a redshift of z ≈ 8.1

Salvaterra, R.; Valle, M. Della; Campana, S.; Chincarini, G.; Covino, S.; D’Avanzo, P.; Fernández-Soto, A.; Guidorzi, C.; Mannucci, F.; Margutti, R.; Thöne, C. C.; Antonelli, L. A.; Barthelmy, S. D.; Pasquale, M. De; D’Elia, V.; Fiore, F.; Fugazza, D.; Hunt, L. K.; Maiorano, E.; Marinoni, S.; Marshall, F. E.; Molinari, E.; Nousek, J. A.; Pian, E.; Racusin, J. L.; Stella, L.; Amati, L.; Andreuzzi, G.; Cusumano, G.; Fenimore, E. E.; Ferrero, P.; Giommi, P.; Guetta, Dafne; Holland, S. T.; Hurley, K.; Israel, G. L.; Mao, J.; Markwardt, C. B.; Masetti, N.; Pagani, C.; Palazzi, E.; Palmer, D. M.; Piranomonte, S.; Tagliaferri, G.; Testa, V.

doi:10.1038/nature08445

Cited by 451 publications

(444 citation statements)

References 26 publications

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“…The column density derived from X-rays is about one order of magnitude higher than the column density of HI as derived from the optical of log N=21.14 (see Table 2). In fact, the X-ray column density is above the average for Swift GRBs but comparable to the mean for z > 4 GRBs of log N HX ∼ 22.5 following the trend of increasing column density with redshift (Campana et al, 2009). This is partly an observational effect (at higher redshifts, a larger column density is needed for it to even be detected) but probably also due to an increased in intervening absorbers contributing to the total absorbing column.…”

Section: Sed From X-ray To Irmentioning

confidence: 77%

“…8 (3.1% or 4.0% for Swift only) are at z > 5 of which 2 are photometric redshifts. The current records are z = 8.2 for GRB 090423A (spectroscopic, Salvaterra et al 2009;Tanvir et al 2009) and z = 9.4 for GRB 090429A (photometric, Cucchiara et al 2011), which makes them one of the farthest objects detected in the Universe. In the past, it had been estimated that a much larger fraction of GRBs might be observed at redshifts beyond 4 − 5 (Bromm & Loeb, 2002 and, taking into account the sensitivity of Swift, at least 10% should be at z>5.…”

Section: Grb 100219a In the Context Of High Redshift Galaxy Abundancesmentioning

confidence: 99%

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GRB 100219A with X-shooter – abundances in a galaxy at z =4.7

Thöne¹,

Fynbo²,

Goldoni³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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Context. Abundances of galaxies at redshifts z > 4 are difficult to obtain from damped Ly α (DLA) systems in the sightlines of quasars (QSOs) due to the Ly α forest blanketing and the low number of high-redshift quasars detected. Gamma-ray bursts (GRBs) with their higher luminosity are well suited to study galaxies out to the formation of the first stars at z > 10. Its large wavelength coverage makes the X-shooter spectrograph an excellent tool to study the interstellar medium (ISM) of high redshift galaxies, in particular if the redshift is not known beforehand. Aims. We want to determine the properties of a GRB host at z = 4.66723 from absorption lines. This is one of the highest redshifts where a detailed analysis with medium-resolution data is possible. Furthermore, we determine the dust extinction using the spectral energy distribution from X-rays to near infrared. Finally, we put the results in context to other GRBs at z > 4 and properties of (high redshift) QSO absorbers. Methods. The velocity components of the resonant and fine-structure absorption lines are fitted with Voigt-profiles and the metallicity determined from S, Si, Fe and O. Si II* together with the energy released in the UV restframe as determined from GROND photometric data gives us the distance of the absorbing material from the GRB. The extinction is determined from the spectral slope using X-ray spectral information and the flux calibrated X-shooter spectrum, cross calibrated with photometric data from GROND. We also collect information on all GRB hosts with z > 4. Results. We measure a relatively high metallicity of [M/H] = −1.0 ± 0.1 from S, the distance of the material showing fine-structure lines is 0.3 to 1.0 kpc. The extinction is moderate with A V = 0.24 ± 0.06 mag. Low-and high ionization as well as fine-structure lines show a complicated kinematic structure probably pointing to a merger in progress. We detect one intervening system at z = 2.18. Conclusions. GRB-DLAs have a shallower evolution of metallicity with redshift than QSO absorbers and no evolution in their HI column density or ionization fraction. GRB hosts at high redshift seem to continue the trend of the metallicity-luminosity relation towards lower metallicities but the sample is still too small to draw a definite conclusion. While the detection of GRBs at z > 4 with current satellites is still difficult, they are very important for our understanding of the early epochs of star-and galaxy-formation in the Universe.

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Section: Sed From X-ray To Irmentioning

confidence: 77%

Section: Grb 100219a In the Context Of High Redshift Galaxy Abundancesmentioning

confidence: 99%

GRB 100219A with X-shooter – abundances in a galaxy at z =4.7

Thöne¹,

Fynbo²,

Goldoni³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…Some of them are so bright that they have been observed up to extremely high redshift (Salvaterra et al 2009;Tanvir et al 2009;Cucchiara et al 2011). In fact, different models (Bromm & Loeb 2002;Salvaterra & Chincarini 2007;de Souza et al 2011;Salvaterra et al 2012;Ghirlanda et al 2015;Elliott et al 2015) consistently predict that ∼ 3% of the GRBs detected by the Swift satellite should lie at z > 6.…”

Section: Introductionmentioning

confidence: 97%

Constraining the PopIII IMF with high-zGRBs

Maio

Ciardi

et al. 2016

Mon. Not. R. Astron. Soc.

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We study the possibility to detect and distinguish signatures of enrichment from PopIII stars in observations of PopII GRBs (GRBIIs) at high redshift by using numerical Nbody/hydrodynamical simulations including atomic and molecular cooling, star formation and metal spreading from stellar populations with different initial mass functions (IMFs), yields and lifetimes. PopIII and PopII star formation regimes are followed simultaneously and both a top-heavy and a Salpeter-like IMF for pristine PopIII star formation are adopted. We find that the fraction of GRBIIs hosted in a medium previously enriched by PopIII stars

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“…Gamma-ray bursts (GRBs) are highly luminous, so they can be detected to much higher redshifts than optical supernovae; the current record holder is at z ≈ 8.2 (Tanvir et al, 2009;Salvaterra et al, 2009). GRBs are extremely diverse and highly beamed, but they exhibit correlations (Amati, 2006;Ghirlanda et al, 2006) between equivalent isotropic energy and spectral properties (such as the energy of peak intensity) or variability.…”

Section: Alternative Distance Indicatorsmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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GRB 090423 at a redshift of z ≈ 8.1

Cited by 451 publications

References 26 publications

GRB 100219A with X-shooter – abundances in a galaxy at z =4.7

GRB 100219A with X-shooter – abundances in a galaxy at z =4.7

Constraining the PopIII IMF with high-zGRBs

Observational probes of cosmic acceleration

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