Evidence for supernova-synthesized dust from the rising afterglow of GRB 071025 at z∼ 5

Perley, D.; Bloom, J.; Klein, C. R.; Covino, S.; Minezaki, Takeo; Woźniak, P. R.; Vestrand, W. T.; Williams, G. G.; Milne, Peter; Butler, Nathaniel R.; Updike, A. C.; Krühler, T.; Afonso, P.; Antonelli, L. A.; Cowie, L. L.; Ferrero, P.; Greiner, J.; Hartmann, D. H.; Kakazu, Y.; Yoldaş, A.; Morgan, A. N.; Price, P. A.; Prochaska, J. Xavier; Yoshii, Yuzuru

doi:10.1111/j.1365-2966.2010.16772.x

Cited by 79 publications

(83 citation statements)

References 110 publications

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“…Properties of all z>4 GRBs. Those with only a photometric redshift, GRB 050814, (Jakobsson et al, 2006), GRB 071025 (Perley et al, 2010), GRB 080916C (Greiner et al, 2009c), GRB 080825B (Krühler et al, 2011a) and GRB 090429A (Cucchiara et al, 2011) …”

Section: Discussionmentioning

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: Discussionmentioning

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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“…Signatures of SN-origin dust have been claimed in the extinction curves of a z ∼ 6.2 QSO (Maiolino et al 2004; see also Gallerani et al 2010) and of two gamma-ray burst host galaxies, one at z ∼ 6.3 (Stratta et al 2007; but this result was undermined by Zafar et al 2010) and one at z ∼ 5 (Perley et al 2010).…”

Section: Introductionmentioning

confidence: 96%

Dust grain growth in the interstellar medium of 5 < z < 6.5 quasars

Michałowski

Murphy

Hjorth

et al. 2010

A&A

107

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Aims. We investigate whether stellar dust sources i.e. asymptotic giant branch (AGB) stars and supernovae (SNe) can account for dust detected in 5 < z < 6.5 quasars (QSOs). Methods. We calculate the required dust yields per AGB star and per SN using the dust masses of QSOs inferred from their millimeter emission and stellar masses approximated as the difference between the dynamical and the H 2 gas masses of these objects. Results. We find that AGB stars are not efficient enough to form dust in the majority of the z > 5 QSOs, whereas SNe may be able to account for dust in some QSOs. However, they require very high dust yields even for a top-heavy initial mass function.Conclusions. This suggests additional non-stellar dust formation mechanism e.g. significant dust grain growth in the interstellar medium of at least three out of nine z > 5 QSOs. SNe (but not AGB stars) may deliver enough heavy elements to fuel this growth.

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“…The dust around the GRB might possibly be subject to destruction by the intense UV radiation of the afterglow or the GRB progenitor (Waxman & Draine 2000;Draine & Hao 2002;D'Elia et al 2007), albeit a clear and highly significant observational signature of this process is still lacking (e.g. Perley et al 2010). Although nearly all afterglow SEDs are well described with continuous extinction laws (e.g.…”

Section: Caveats In the Photo-z Measurementmentioning

confidence: 99%

Photometric redshifts for gamma-ray burst afterglows from GROND andSwift/UVOT

Krühler

Schady

Greiner

et al. 2011

A&A

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Aims. We present a framework to obtain photometric redshifts (photo-zs) for gamma-ray burst afterglows. Using multi-band photometry from GROND and Swift/UVOT, photo-zs are derived for five GRBs for which spectroscopic redshifts are not available. Methods. We use UV/optical/NIR data and synthetic photometry based on afterglow observations and theory to derive the photometric redshifts of GRBs and their accuracy. Taking into account the afterglow synchrotron emission properties, we investigate the application of photometry to derive redshifts in a theoretical range between z ∼ 1 to z ∼ 12.Results. The measurement of photo-zs for GRB afterglows provides a quick, robust and reliable determination of the distance scale to the burst, particularly in those cases where spectroscopic observations in the optical/NIR range cannot be obtained. Given a sufficiently bright and mildly reddened afterglow, the relative photo-z accuracy η = Δz/(1 + z) is better than 10% between z = 1.5 and z ∼ 7 and better than 5% between z = 2 and z = 6. We detail the approach on 5 sources without spectroscopic redshifts observed with UVOT on-board Swift and/or GROND. The distance scale to those same afterglows is measured to be z = 4.31 +0.14 −0.15 for GRB 080825B, z = 2.13 +0.14 −0.20 for GRB 080906, z = 3.44 +0.15 −0.32 for GRB 081228, z = 2.03 +0.16 −0.14 for GRB 081230 and z = 1.28 +0.16 −0.15 for GRB 090530. Conclusions. Due to the exceptional luminosity and simple continuum spectrum of GRB afterglows, photometric redshifts can be obtained to an accuracy as good as η ∼ 0.03 over a large redshift range including robust (η ∼ 0.1) measurements in the ultra-high redshift regime (z 7). Combining the response from UVOT with ground-based observatories and in particular GROND operating in the optical/NIR wavelength regime, reliable photo-zs can be obtained from z ∼ 1.0 out to z ∼ 10, and possibly even at higher redshifts in some favorable cases, provided that these GRBs exist, are localized quickly, have sufficiently bright afterglows and are not heavily obscured.

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Evidence for supernova-synthesized dust from the rising afterglow of GRB 071025 at z∼ 5

Cited by 79 publications

References 110 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

Dust grain growth in the interstellar medium of 5 < z < 6.5 quasars

Photometric redshifts for gamma-ray burst afterglows from GROND andSwift/UVOT

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