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dc.contributor.authorPozzetti, L.
dc.contributor.authorHirata, C.~M.
dc.contributor.authorGeach, J.~E.
dc.contributor.authorCimatti, A.
dc.contributor.authorBaugh, C.
dc.contributor.authorCucciati, O.
dc.contributor.authorMerson, A.
dc.contributor.authorNorberg, P.
dc.contributor.authorShi, D.
dc.date.accessioned2016-12-21T16:35:36Z
dc.date.available2016-12-21T16:35:36Z
dc.date.issued2016-06-01
dc.identifier.citationPozzetti , L , Hirata , C M , Geach , J E , Cimatti , A , Baugh , C , Cucciati , O , Merson , A , Norberg , P & Shi , D 2016 , ' Modelling the number density of H$ emitters for future spectroscopic near-IR space missions ' , Astronomy & Astrophysics , vol. 590 , A3 . https://doi.org/10.1051/0004-6361/201527081
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 10175456
dc.identifier.otherPURE UUID: 683cb5ce-2b72-4f84-a26d-50b014aed860
dc.identifier.otherBibtex: urn:bb82c042806f081bc9641fe9bf169077
dc.identifier.otherScopus: 84966322224
dc.identifier.urihttp://hdl.handle.net/2299/17456
dc.descriptionReproduced with permission from Astronomy & Astrophysics, © ESO
dc.description.abstractContext. The future space missions Euclid and WFIRST-AFTA will use the Hα emission line to measure the redshifts of tens of millions of galaxies. The Hα luminosity function at z> 0.7 is one of the major sources of uncertainty in forecasting cosmological constraints from these missions.Aims. We construct unified empirical models of the Hα luminosity function spanning the range of redshifts and line luminosities relevant to the redshift surveys proposed with Euclid and WFIRST-AFTA.Methods. By fitting to observed luminosity functions from Hα surveys, we build three models for its evolution. Different fitting methodologies, functional forms for the luminosity function, subsets of the empirical input data, and treatment of systematic errors are considered to explore the robustness of the results.Results. Functional forms and model parameters are provided for all three models, along with the counts and redshift distributions up to z ~ 2.5 for a range of limiting fluxes (FHα> 0.5 − 3 × 10-16 erg cm-2 s-1) that are relevant for future space missions. For instance, in the redshift range 0.90 <z< 1.8, our models predict an available galaxy density in the range 7700–130 300 and 2000–4800 deg-2 respectively at fluxes above FHα> 1 and 2 × 10-16 erg cm-2 s-1, and 32 000–48 0000 for FHα> 0.5 × 10-16 erg cm-2 s-1 in the extended redshift range 0.40 <z< 1.8. We also consider the implications of our empirical models for the total Hα luminosity density of the Universe, and the closely related cosmic star formation history.en
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysics
dc.subjectgalaxies: evolution, galaxies: high-redshift, galaxies: star formation, galaxies: luminosity function, mass function, cosmology: observations
dc.titleModelling the number density of H$ emitters for future spectroscopic near-IR space missionsen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201527081
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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