Please use this identifier to cite or link to this item: http://hdl.handle.net/2381/33527
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dc.contributor.authorKruehler, T.-
dc.contributor.authorMalesani, D.-
dc.contributor.authorFynbo, J. P. U.-
dc.contributor.authorHartoog, O. E.-
dc.contributor.authorHjorth, J.-
dc.contributor.authorJakobsson, P.-
dc.contributor.authorPerley, D. A.-
dc.contributor.authorRossi, A.-
dc.contributor.authorSchady, P.-
dc.contributor.authorSchulze, S.-
dc.contributor.authorTanvir, Nial-
dc.contributor.authorVergani, S. D.-
dc.contributor.authorWiersema, K.-
dc.contributor.authorAfonso, P. M. J.-
dc.contributor.authorBolmer, J.-
dc.contributor.authorCano, Z.-
dc.contributor.authorCovino, S.-
dc.contributor.authorD'Elia, V.-
dc.contributor.authorde Ugarte Postigo, A.-
dc.contributor.authorFilgas, R.-
dc.contributor.authorFriis, M.-
dc.contributor.authorGraham, J. F.-
dc.contributor.authorGreiner, J.-
dc.contributor.authorGoldoni, P.-
dc.contributor.authorGomboc, A.-
dc.contributor.authorHammer, F.-
dc.contributor.authorJapelj, J.-
dc.contributor.authorKann, D. A.-
dc.contributor.authorKaper, L.-
dc.contributor.authorKlose, S.-
dc.contributor.authorLevan, A. J.-
dc.contributor.authorLeloudas, G.-
dc.contributor.authorMilvang-Jensen, B.-
dc.contributor.authorGuelbenzu, A. N.-
dc.contributor.authorPalazzi, E.-
dc.contributor.authorPian, E.-
dc.contributor.authorPiranomonte, S.-
dc.contributor.authorSanchez-Ramirez, R.-
dc.contributor.authorSavaglio, S.-
dc.contributor.authorSelsing, J.-
dc.contributor.authorTagliaferri, G.-
dc.contributor.authorVreeswijk, P. M.-
dc.contributor.authorWatson, D. J.-
dc.contributor.authorXu, D.-
dc.date.accessioned2015-11-10T13:22:42Z-
dc.date.available2015-11-10T13:22:42Z-
dc.date.issued2015-09-21-
dc.identifier.citationAstronomy and Astrophysics, 2015, 581en
dc.identifier.issn0004-6361-
dc.identifier.urihttp://www.aanda.org/articles/aa/abs/2015/09/aa25561-14/aa25561-14.htmlen
dc.identifier.urihttp://hdl.handle.net/2381/33527-
dc.description.abstractWe present data and initial results from VLT/X-Shooter emission-line spectroscopy of 96 galaxies selected by long γ-ray bursts (GRBs) at 0.1 <z< 3.6, the largest sample of GRB host spectra available to date. Most of our GRBs were detected by Swift and 76% are at 0.5 <z< 2.5 with a median z [Subscript: med] ~ 1.6. Based on Balmer and/or forbidden lines of oxygen, nitrogen, and neon, we measure systemic redshifts, star formation rates (SFR), visual attenuations (AV), oxygen abundances (12 + log (O/H)), and emission-line widths (σ). We study GRB hosts up to z ~ 3.5 and find a strong change in their typical physical properties with redshift. The median SFR of our GRB hosts increases from SFR[Subscript: med] ~ 0.6 M[Subscript: ⊙] yr [Superscript: -1] at z ~ 0.6 up to SFR[Subscript: med] ~ 15 M [Subscript: ⊙] yr[Superscript: -1] at z ~ 2. A higher ratio of [O iii]/[O ii]  at higher redshifts leads to an increasing distance of GRB-selected galaxies to the locus of local galaxies in the Baldwin-Phillips-Terlevich diagram. There is weak evidence for a redshift evolution in AV and σ, with the highest values seen at z ~ 1.5 (AV) or z ~ 2 (σ). Oxygen abundances of the galaxies are distributed between 12 + log (O/H) = 7.9 and 12 + log (O/H) = 9.0 with a median 12 + log (O/H) [Subscript: med] ~ 8.5. The fraction of GRB-selected galaxies with super-solar metallicities is ~20% at z< 1 in the adopted metallicity scale. This is significantly less than the fraction of total star formation in similar galaxies, illustrating that GRBs are scarce in high metallicity environments. At z ~ 3, sensitivity limits us to probing only the most luminous GRB hosts for which we derive metallicities of Z ≲ 0.5 Z [Subscript: ⊙] . Together with a high incidence of Z ~ 0.5 Z [Subscript: ⊙] galaxies at z ~ 1.5, this indicates that a metallicity dependence at low redshift will not be dominant at z ~ 3. Significant correlations exist between the hosts’ physical properties. Oxygen abundance, for example, relates to AV (12 + log (O/H) ∝ 0.17·AV), line width (12 + log (O/H) ∝ σ [Superscript: 0.6] ), and SFR (12 + log (O/H) ∝ SFR [Superscript: 0.2]). In the last two cases, the normalization of the relations shift to lower metallicities at z> 2 by ~0.4 dex. These properties of GRB hosts and their evolution with redshift can be understood in a cosmological context of star-forming galaxies and a picture in which the hosts’ properties at low redshift are influenced by the tendency of GRBs to avoid the most metal-rich environments.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: generalen
dc.subjectgalaxies: high-redshiften
dc.subjectgalaxies: star formationen
dc.subjectgalaxies: evolutionen
dc.subjectSTAR-FORMING GALAXIESen
dc.subjectMASS-METALLICITY RELATIONen
dc.subjectDIGITAL SKY SURVEYen
dc.subjectCORE-COLLAPSE SUPERNOVAEen
dc.subjectCOSMIC CHEMICAL EVOLUTIONen
dc.subjectHIGH-REDSHIFT GALAXIESen
dc.subjectFORMATION RATE DENSITYen
dc.subjectLYMAN BREAK GALAXIESen
dc.subjectLY-ALPHA EMITTERSen
dc.subjectGRB HOST GALAXIESen
dc.titleGRB hosts through cosmic time VLT/X-Shooter emission-line spectroscopy of 96 gamma-ray-burst-selected galaxies at 0.1 < z < 3.6en
dc.typeJournal Articleen
dc.identifier.doi10.1051/0004-6361/201425561-
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

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