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dc.contributor.authorAguirre, Anthony
dc.contributor.authorSchaye, Joop
dc.contributor.authorHernquist, Lars
dc.contributor.authorKay, Scott
dc.contributor.authorSpringel, Volker
dc.contributor.authorTheuns, Tom
dc.date.accessioned2019-09-20T10:31:11Z
dc.date.issued2005
dc.identifier.citationAguirre, Anthony, Joop Schaye, Lars Hernquist, Scott Kay, Volker Springel, and Tom Theuns. 2005. “Confronting Cosmological Simulations with Observations of Intergalactic Metals.” The Astrophysical Journal 620 (1): L13–17. https://doi.org/10.1086/428498.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41381594*
dc.description.abstractUsing the statistics of pixel optical depths, we compare H i, C iv, and C iii absorption in a set of six high- quality z similar to 3-4 different state- of- the- art cosmological simulations that include galactic outflows. We find that the simulations predict far too little C iv absorption, unless the UV background is extremely soft, and always predict far too small C iii/ C iv ratios. We note, however, that much of the enriched gas is in a phase (T similar to 10(5) - 10(7) K, rho/(rho) similar to 0.1-10, Z greater than or similar to 0.1 Z.) that should cool by metal line emission- which was not included in our simulations. When the effect of cooling is modeled, the predicted C iv absorption increases substantially, but the C iii/ C iv ratios are still far too small because the density of the enriched gas is too low. Finally, we find that the predicted metal distribution is much too inhomogeneous to reproduce the observed probability distribution of C iv absorption. These findings suggest that strong winds cannot fully explain the z less than or similar to 6 observed enrichment and that an additional ( perhaps higher z) contribution is required.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleConfronting Cosmological Simulations with Observations of Intergalactic Metals
dc.typeJournal Article
dc.description.versionAccepted Manuscript
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorHernquist, Lars Eric::39d9dfe7535406d002e4507056194fd1::600
dc.date.available2019-09-20T10:31:11Z
dash.workflow.comments1Science Serial ID 96951
dc.identifier.doi10.1086/428498
dash.source.volume620;1
dash.source.pageL13-L17


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