Please use this identifier to cite or link to this item: http://hdl.handle.net/2381/33530
Full metadata record
DC FieldValueLanguage
dc.contributor.authorHartoog, O. E.-
dc.contributor.authorMalesani, D.-
dc.contributor.authorFynbo, J. P. U.-
dc.contributor.authorGoto, T.-
dc.contributor.authorKruehler, T.-
dc.contributor.authorVreeswijk, P. M.-
dc.contributor.authorDe Cia, A.-
dc.contributor.authorXu, D.-
dc.contributor.authorMoller, P.-
dc.contributor.authorCovino, S.-
dc.contributor.authorD'Elia, V.-
dc.contributor.authorFlores, H.-
dc.contributor.authorGoldoni, P.-
dc.contributor.authorHjorth, J.-
dc.contributor.authorJakobsson, P.-
dc.contributor.authorKrogager, J-K.-
dc.contributor.authorKaper, L.-
dc.contributor.authorLedoux, C.-
dc.contributor.authorLevan, A. J.-
dc.contributor.authorMilvang-Jensen, B.-
dc.contributor.authorSollerman, J.-
dc.contributor.authorSparre, M.-
dc.contributor.authorTagliaferri, G.-
dc.contributor.authorTanvir, Nial-
dc.contributor.authorPostigo, A. D. U.-
dc.contributor.authorVergani, S. D.-
dc.contributor.authorWiersema, K.-
dc.contributor.authorDatson, J.-
dc.contributor.authorSalinas, R.-
dc.contributor.authorMikkelsen, K.-
dc.contributor.authorAghanim, N.-
dc.date.accessioned2015-11-10T13:45:44Z-
dc.date.available2015-11-10T13:45:44Z-
dc.date.issued2015-08-20-
dc.identifier.citationAstronomy and Astrophysics, 2015, 580, A139 (15)en
dc.identifier.issn0004-6361-
dc.identifier.urihttp://www.aanda.org/articles/aa/abs/2015/08/aa25001-14/aa25001-14.htmlen
dc.identifier.urihttp://hdl.handle.net/2381/33530-
dc.description.abstractContext. The reionisation of the Universe is a process that is thought to have ended around z ~ 6, as inferred from spectroscopy of distant bright background sources, such as quasars (QSO) and gamma-ray burst (GRB) afterglows. Furthermore, spectroscopy of a GRB afterglow provides insight in its host galaxy, which is often too dim and distant to study otherwise. Aims. For the Swift GRB 130606A at z = 5.913 we have obtained a high S/N spectrum covering the full optical and near-IR wavelength region at intermediate spectral resolution with VLT/X-Shooter. We aim to measure the degree of ionisation of the intergalactic medium (IGM) between z = 5.02−5.84 and to study the chemical abundance pattern and dust content of its host galaxy. Methods. We estimated the UV continuum of the GRB afterglow using a power-law extrapolation, then measured the flux decrement due to absorption at Lyα,β, and γ wavelength regions. Furthermore, we fitted the shape of the red damping wing of Lyα. The hydrogen and metal absorption lines formed in the host galaxy were fitted with Voigt profiles to obtain column densities. We investigated whether ionisation corrections needed to be applied. Results. Our measurements of the Lyα-forest optical depth are consistent with previous measurements of QSOs, but have a much smaller uncertainty. The analysis of the red damping wing yields a neutral fraction x [Subscript: H I] < 0.05 (3σ). We obtain column density measurements of H, Al, Si, and Fe; for C, O, S and Ni we obtain limits. The ionisation due to the GRB is estimated to be negligible (corrections <0.03 dex), but larger corrections may apply due to the pre-existing radiation field (up to 0.4 dex based on sub-DLA studies). Assuming that [ Si/Fe ] = +0.79 ± 0.13 is due to dust depletion, the dust-to-metal ratio is similar to the Galactic value. Conclusions. Our measurements confirm that the Universe is already predominantly ionised over the redshift range probed in this work, but was slightly more neutral at z> 5.6. GRBs are useful probes of the ionisation state of the IGM in the early Universe, but because of internal scatter we need a larger statistical sample to draw robust conclusions. The high [Si/Fe] in the host can be due to dust depletion, α-element enhancement, or a combination of both. The very high value of [ Al/Fe ] = 2.40 ± 0.78 might be due to a proton capture process and is probably connected to the stellar population history. We estimate the host metallicity to be −1.7 < [ M/H ] < −0.9 (2%−13% of solar).en
dc.language.isoenen
dc.publisherEDP Sciencesen
dc.rightsReproduced with permission from Astronomy & Astrophysics, © ESO. Deposited with reference to the publisher’s open access archiving policy, available at http://www.aanda.org/author-information/copyrighten
dc.subjectScience & Technologyen
dc.subjectPhysical Sciencesen
dc.subjectAstronomy & Astrophysicsen
dc.subjectgamma-ray burst: individual: GRB 130606Aen
dc.subjectcosmology: observationsen
dc.subjectdark ages, reionization, first starsen
dc.subjectISM: abundancesen
dc.subjectGAMMA-RAY BURSTen
dc.subjectDAMPED LY-ALPHAen
dc.subjectLYMAN-BREAK GALAXIESen
dc.subjectMASS-METALLICITY RELATIONen
dc.subjectHUBBLE-SPACE-TELESCOPEen
dc.subjectSTAR-FORMING REGIONSen
dc.subjectGUNN-PETERSON TROUGHen
dc.subjectHIGH-REDSHIFTen
dc.subjectHOST GALAXIESen
dc.subjectINTERGALACTIC MEDIUMen
dc.titleVLT/X-Shooter spectroscopy of the afterglow of the Swift GRB 130606A Chemical abundances and reionisation at z similar to 6en
dc.typeJournal Articleen
dc.identifier.doi10.1051/0004-6361/201425001-
dc.identifier.eissn1432-0746-
dc.description.statusPeer-revieweden
dc.description.versionPublisher Versionen
dc.type.subtypeArticle;Journal-
pubs.organisational-group/Organisationen
pubs.organisational-group/Organisation/COLLEGE OF SCIENCE AND ENGINEERINGen
pubs.organisational-group/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomyen
dc.dateaccepted2015-06-15-
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

Files in This Item:
File Description SizeFormat 
1409.4804v2.pdfPost-review (final submitted)5.64 MBAdobe PDFView/Open
aa25001-14.pdfPublished (publisher PDF)5.57 MBAdobe PDFView/Open


Items in LRA are protected by copyright, with all rights reserved, unless otherwise indicated.