An optical spectrum of the afterglow of a γ-ray burst at a redshift of z = 6.295

Kawai, N.; Kosugi, George; Aoki, Kentaro; Yamada, Tōru; Totani, Tomonori; Ohta, Kouji; Iye, Masanori; Hattori, Takashi; Aoki, Wako; Furusawa, Hisanori; Hurley, K.; Kawabata, Koji S.; Kobayashi, Naoto; Komiyama, Yutaka; Mizumoto, Y.; Nomoto, Ken’ichi; Noumaru, Junichi; Ogasawara, Ryusuke; Sato, Rie; Sekiguchi, K.; Shirasaki, Y.; Suzuki, M.; Takata, Tadafumi; Tamagawa, Toru; Terada, Hiroshi; Watanabe, Jun; Yatsu, Yoichi; Yoshida, A.

doi:10.1038/nature04498

Cited by 251 publications

(196 citation statements)

References 19 publications

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“…For the metal abundance, we only consider selected elements, such as carbon (C), oxygen (O), silicon (Si) and iron (Fe), since these are the most abundant in the Universe and easier to detect in the spectra of high-z GRB afterglows (Kawai et al 2006;Castro-Tirado et al 2013). Sulfur (S) always follows Si and shows a similar behaviour.…”

Section: Resultsmentioning

confidence: 99%

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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Section: Resultsmentioning

confidence: 99%

Constraining the PopIII IMF with high-zGRBs

Maio

Ciardi

et al. 2016

Mon. Not. R. Astron. Soc.

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“…All lines except S II listed in Kawai et al (2006) are completely saturated, also including another Si II line at λ1304 not listed in the paper. The saturation makes a curve-of-growth fit as mentioned in impossible, however, the column densities of Si II, O I and C II are definitely higher than listed in the paper.…”

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

confidence: 99%

“…The saturation makes a curve-of-growth fit as mentioned in impossible, however, the column densities of Si II, O I and C II are definitely higher than listed in the paper. Taking the EW from S II λ 1253 and assuming a (resonable) b-parameter of ∼ 35 km s −1 , we get a column density of around log N ∼ 15.3, 0.3 dex lower than listed in Kawai et al (2006). Totani et al (2006) reinvestigated the DLA column density of GRB 050904 and find a slightly higher value of log N HI =21.6.…”

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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“…Due to these limitations, the multiwavelength properties of GRBs at z  5 remain poorly characterized (Tagliaferri et al 2005;Haislip et al 2006;Kawai et al 2006;Greiner et al 2009;Salvaterra et al 2009;Tanvir et al 2009;Cucchiara et al 2011). We carried out a comprehensive analysis of three GRBs at z6 with radio detections and demonstrated that these events exhibit explosion energies typical of the lower redshift population but tend to exhibit narrower jet opening angles (Laskar et al 2014, henceforth LBT14).…”

Section: Introductionmentioning

confidence: 99%

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

Laskar

Berger

Chornock

et al. 2018

ApJ

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We present the first results from a recently concluded study of GRBs at z  5 with the Karl G. Jansky Very Large Array (VLA). Spanning 1 to 85.5 GHz and 7 epochs from 1.5 to 82.3 days, our observations of GRB140311A are the most detailed joint radio and millimeter observations of a GRB afterglow at z  5 to date. In conjunction with optical/near-IR and X-ray data, the observations can be understood in the framework of radiation from a single blast wave shock with energy »É 8.5 10 K,iso 53 erg expanding into a constant density environment with density, » n 8 0 -cm 3 . The X-ray and radio observations require a jet break at » t 0.6 jet days, yielding an opening angle of q »  4 jet and a beaming-corrected blast wave kinetic energy of »É 2.2 10 K 50 erg. The results from our radio follow-up and multiwavelength modeling lend credence to the hypothesis that detected high-redshift GRBs may be more tightly beamed than events at lower redshift. We do not find compelling evidence for reverse shock emission, which may be related to fast cooling driven by the moderately high circumburst density.

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An optical spectrum of the afterglow of a γ-ray burst at a redshift of z = 6.295

Cited by 251 publications

References 19 publications

Constraining the PopIII IMF with high-zGRBs

Constraining the PopIII IMF with high-zGRBs

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

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

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