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Theoretical study of an LAE-C IV absorption pair at z = 5.7

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dc.contributor.authorGarcía, L. A.en
dc.contributor.authorTescari, E.en
dc.contributor.authorRyan-Weber, E. V.en
dc.contributor.authorWyithe, J. S.B.en
dc.date.accessioned2026-01-02T09:41:15Z
dc.date.available2026-01-02T09:41:15Z
dc.date.issued2017en
dc.description.abstractWe present a theoretical model to predict the properties of an observed z=5.72Lyman a emitter galaxy-C IV absorption pair separated by 1384 comoving kpc h-1. We use the separation of the pair and an outflow velocity/time travelling argument to demonstrate that the observed galaxy cannot be the source of metals for the C IV absorber. We find a plausible explanation for the metal enrichment in the context of our simulations: a dwarf galaxy with M∗= 1.87 × 109M⊙located 119 comoving kpc h-1away with a wind velocity of ~100 km s-1launched at z ~ 7. Such a dwarf (MUV= -20.5) is fainter than the detection limit of the observed example. In a general analysis of galaxy-C IV absorbers, we find galaxies with - 20.5 MUV < -18.8 are responsible for the observed metal signatures. In addition, we find no correlation between the mass of the closest galaxy to the absorber and the distance between them, but a weak anti-correlation between the strength of the absorption and the separation of galaxy-absorber pairs.en
dc.description.sponsorshipParts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAAS-TRO), through project number CE110001020. This work was supported by the Flagship Allocation Scheme of the NCI National Facility at the ANU. The authors acknowledge CAASTRO for funding and allocating time for the project Diagnosing Hydrogen Reioniza-tion with metal absorption line ratios (fy6) during 2015 and 2016. We also thank the anonymous referee for their insightful comments. EVR-W acknowledges ARC DP 1095600. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. This work was supported by the Flagship Allocation Scheme of the NCI National Facility at the ANU. The authors acknowledge CAASTROfor funding and allocating time for the project Diagnosing Hydrogen Reionization with metal absorption line ratios (fy6) during 2015 and 2016. We also thank the anonymous referee for their insightful comments. EVR-W acknowledges ARC DP 1095600.en
dc.description.statusPeer-revieweden
dc.format.extent5en
dc.identifier.issn1745-3925en
dc.identifier.otherORCID:/0000-0001-7956-9758/work/195266043en
dc.identifier.scopus85090704987en
dc.identifier.urihttps://hdl.handle.net/1885/733802377
dc.language.isoenen
dc.rightsPublisher Copyright: © 2020 American Institute of Physics Inc.. All rights reserved.en
dc.sourceMonthly Notices of the Royal Astronomical Society: Lettersen
dc.subjectCosmology: theoryen
dc.subjectIntergalactic mediumen
dc.subjectMethods: numericalen
dc.titleTheoretical study of an LAE-C IV absorption pair at z = 5.7en
dc.typeJournal articleen
dspace.entity.typePublicationen
local.bibliographicCitation.lastpageL57en
local.bibliographicCitation.startpageL53en
local.contributor.affiliationGarcía, L. A.; Swinburne University of Technologyen
local.contributor.affiliationTescari, E.; ARC Centre of Excellence for All-sky Astrophysicsen
local.contributor.affiliationRyan-Weber, E. V.; Swinburne University of Technologyen
local.contributor.affiliationWyithe, J. S.B.; ARC Centre of Excellence for All-sky Astrophysicsen
local.identifier.citationvolume469en
local.identifier.doi10.1093/mnrasl/slx053en
local.identifier.pureed83a950-4dbb-407f-b718-3a44e6979aacen
local.identifier.urlhttps://www.scopus.com/pages/publications/85090704987en
local.type.statusPublisheden

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