Revealing the High-Redshift Star Formation Rate with Gamma-Ray Bursts

Yüksel, Hasan; Kistler, Matthew D.; Beacom, J. F.; Hopkins, A. M.

doi:10.1086/591449

Cited by 360 publications

(394 citation statements)

References 62 publications

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“…The peak of the SF is expected to be around z ∼ 2, and it is not yet known how the SF evolves at redshifts beyond z ∼ 4. Several attempts have been made to determine the cosmic SFR using GRBs (see, e.g., Yüksel et al 2008;Kistler et al 2009) indicating a shallower decay towards higher redshift than derived by galaxy SF measurements. The redshift distribution of Swift GRBs at high redshifts can be well explained by a constant cosmic star-formation density from redshift 3.5 onwards (Jakobsson et al, 2006) 6 .…”

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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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: 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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“…whereρ 0 = 0.0104 M ⊙ Mpc −3 yr −1 , α = 4.22, β = −0.20, γ = −11.30, B = 2.70 × 10 6 , C = 6.37 [4,12]. The total flux, dN tot ν /dE ν is the sum of neutrino fluxes from all types of SNe, and we estimate the detector event rate by…”

Section: Detection Rate Of Rsnmentioning

confidence: 99%

Study of Red Supergiant and Supernova Rate Problems via Relic Supernova Neutrino Spectrum

Hidaka¹,

Kajino²,

Mathews³

2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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Direct observations of core-collapse supernovae and their red supergiant progenitors suggest that the upper mass limit of red supergiants may be only about 16.5 − 18 M ⊙ , while the standard theoretical value is as much as 25 M ⊙ . We investigate the possibility that red supergiants with M > 16.5 − 18 M ⊙ end their lives as failed supernovae and analyze their contribution to the relic supernova neutrino spectrum. We show energetic neutrinos in the relic supernova neutrino spectrum are sensitive to the nuclear equation of state. This mass limit also influences the cosmic supernova rate, and its theoretical estimate has been known to be higher than the observational values. We show that adopting this mass limit eliminates the inconsistency.

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“…Recent studies show that the rate of GRBs does not strictly follow the SFH but is actually enhanced by some mechanism at high redshift (Le & Dermer 2007;Salvaterra & Chincarini 2007;Kistler et al 2008;Yüksel et al 2008;Robertson & Ellis 2012;Wang 2013). The SFR inferred from the highredshift (z > 6) GRBs seems to be too high in comparison with the SFR obtained from some high-redshift galaxy surveys (Bouwens et al 2009(Bouwens et al , 2011.…”

Section: Possible Origins Of High-redshift Grb Rate Excessmentioning

confidence: 99%

GRBs and Fundamental Physics

Petitjean

Wang

et al. 2016

Space Sci Rev

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Gamma-ray bursts (GRBs) are short and intense flashes at the cosmological distances, which are the most luminous explosions in the Universe. The high luminosities of GRBs make them detectable out to the edge of the visible universe. So, they are unique tools to probe the properties of high-redshift universe: including the cosmic expansion and dark energy, star formation rate, the reionization epoch and the metal evolution of the Universe. First, they can be used to constrain the history of cosmic acceleration and the evolution of dark energy in a redshift range hardly achievable by other cosmological probes. Second, long GRBs are believed to be formed by collapse of massive stars. So they can be used to derive the high-redshift star formation rate, which can not be probed by current observations. Moreover, the use of GRBs as cosmological tools could unveil the reionization history and metal evolution of the Universe, the intergalactic medium (IGM) properties and the nature of first stars in the early universe. But beyond that, the GRB high-energy photons can be applied to constrain Lorentz invariance violation (LIV) and to test Einstein's Equivalence Principle (EEP). In this paper, we review the progress on the GRB cosmology and fundamental physics probed by GRBs.

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Revealing the High-Redshift Star Formation Rate with Gamma-Ray Bursts

Cited by 360 publications

References 62 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

Study of Red Supergiant and Supernova Rate Problems via Relic Supernova Neutrino Spectrum

GRBs and Fundamental Physics

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