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http://hdl.handle.net/2445/119259
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DC Field | Value | Language |
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dc.contributor.author | D'Odorico, V. | - |
dc.contributor.author | Cristiani, S. | - |
dc.contributor.author | Pomante, E. | - |
dc.contributor.author | Carswell, R. F. | - |
dc.contributor.author | Viel, Matteo | - |
dc.contributor.author | Barai, P. | - |
dc.contributor.author | Becker, G. D. | - |
dc.contributor.author | Calura, F. | - |
dc.contributor.author | Cupani, G. | - |
dc.contributor.author | Fontanot, F. | - |
dc.contributor.author | Haehnelt, M. G. | - |
dc.contributor.author | Kim, T.-S. | - |
dc.contributor.author | Miralda Escudé, Jordi | - |
dc.contributor.author | Rorai, A. | - |
dc.contributor.author | Tescari, E. | - |
dc.contributor.author | Vanzella, E. | - |
dc.date.accessioned | 2018-01-24T11:56:16Z | - |
dc.date.available | 2018-01-24T11:56:16Z | - |
dc.date.issued | 2016-08-26 | - |
dc.identifier.issn | 0035-8711 | - |
dc.identifier.uri | http://hdl.handle.net/2445/119259 | - |
dc.description.abstract | In this work, we investigate the abundance and distribution of metals in the intergalactic medium (IGM) at 〈z〉 ≃ 2.8 through the analysis of an ultra-high signal-to-noise ratio UVES spectrum of the quasar HE0940-1050. In the C IV forest, our deep spectrum is sensitive at 3σ to lines with column density down to log NCIV ≃ 11.4 and in 60 per cent of the considered redshift range down to ≃11.1. In our sample, all H I lines with log NHI ≥ 14.8 show an associated C IV absorption. In the range 14.0 ≤ log NHI < 14.8, 43 per cent of H I lines has an associated C IV absorption. At log NHI < 14.0, the detection rates drop to <10 per cent, possibly due to our sensitivity limits and not to an actual variation of the gas abundance properties. In the range log NHI ≥ 14, we observe a fraction of H I lines with detected C IV a factor of 2 larger than the fraction of H I lines lying in the circumgalactic medium (CGM) of relatively bright Lyman-break galaxies hosted by dark matter haloes with 〈M〉 ∼ 1012 M⊙. The comparison of our results with the output of a grid of photoionization models and of two cosmological simulations implies that the volume filling factor of the IGM gas enriched to a metallicity logZ/Z⊙≳−3 logZ/Z⊙≳−3 should be of the order of ∼10-13 per cent. In conclusion, our results favour a scenario in which metals are found also outside the CGM of bright star-forming galaxies, possibly due to pollution by lower mass objects and/or to an early enrichment by the first sources. | - |
dc.format.extent | 18 p. | - |
dc.format.mimetype | application/pdf | - |
dc.language.iso | eng | - |
dc.publisher | Royal Astronomical Society | - |
dc.relation.isformatof | Reproducció del document publicat a: https://doi.org/10.1093/mnras/stw2161 | - |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society, 2016, vol. 463, num. 3, p. 2690-2707 | - |
dc.relation.uri | https://doi.org/10.1093/mnras/stw2161 | - |
dc.rights | (c) D'Odorico, V. et al., 2016 | - |
dc.source | Articles publicats en revistes (Institut de Ciències del Cosmos (ICCUB)) | - |
dc.subject.classification | Galàxies | - |
dc.subject.classification | Quàsars | - |
dc.subject.classification | Cosmologia | - |
dc.subject.other | Galaxies | - |
dc.subject.other | Quasars | - |
dc.subject.other | Cosmology | - |
dc.title | Metals in the z ∼ 3 intergalactic medium: results from an ultra-high signal-to-noise ratio UVES quasar spectrum | - |
dc.type | info:eu-repo/semantics/article | - |
dc.type | info:eu-repo/semantics/publishedVersion | - |
dc.identifier.idgrec | 669447 | - |
dc.date.updated | 2018-01-24T11:56:16Z | - |
dc.relation.projectID | info:eu-repo/grantAgreement/EC/FP7/320596/EU//EMERGENCE | - |
dc.relation.projectID | info:eu-repo/grantAgreement/EC/FP7/257670/EU//COSMOIGM | - |
dc.rights.accessRights | info:eu-repo/semantics/openAccess | - |
Appears in Collections: | Articles publicats en revistes (Institut de Ciències del Cosmos (ICCUB)) Publicacions de projectes de recerca finançats per la UE |
Files in This Item:
File | Description | Size | Format | |
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669447.pdf | 1.97 MB | Adobe PDF | View/Open |
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