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dc.contributor.authorAvila, Santiago
dc.contributor.authorVos-Gines, Bernhard
dc.contributor.authorCunnington, Steven
dc.contributor.authorStevens, Adam R.H.
dc.contributor.authorYepes Alonso, Gustavo 
dc.contributor.authorKnebe, Alexander 
dc.contributor.authorChuang, Chia Hsun
dc.contributor.otherUAM. Departamento de Física Teóricaes_ES
dc.date.accessioned2022-09-26T14:19:43Z
dc.date.available2022-09-26T14:19:43Z
dc.date.issued2021-11-26
dc.identifier.citationMonthly Notices of the Royal Astronomical Society 510.1 (2022): 292-308es_ES
dc.identifier.issn0035-8711 (print)es_ES
dc.identifier.issn1365-2966 (online)es_ES
dc.identifier.urihttp://hdl.handle.net/10486/704285
dc.descriptionThis is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Monthly Notices of the Royal Astronomical Society 510.1 (2022): 292-308 is available online at: https://academic.oup.com/mnras/article-abstract/510/1/292/6442269?redirectedFrom=fulltext#no-access-messagees_ES
dc.description.abstractWe study the clustering of H i intensity maps (IM) produced from simulations with a focus on baryonic acoustic oscillations (BAOs) and the effects induced by telescope beam smoothing and foreground cleaning. We start by creating an H i catalogue at z = 1.321 based on the Semi-Analytic Galaxy Evolution (SAGE) model applied to the UNIT simulations. With this catalogue, we investigate the relation between model H i and the dark matter haloes and we also study the abundance of H i, Omega rm{H small {rm I}}, predicted by this model. We then create synthetic H i IM with a nearest-grid-point approach. In order to simulate the telescope beam effect, a Gaussian smoothing is applied on the plane perpendicular to the line of sight. The effect of foreground removal methods is simulated by exponentially damping the largest wavelength Fourier modes on the radial direction. We study the anisotropic 2-point correlation function (2PCF) ζ(rpdbl, rpdbl) and how it is affected by the aforementioned observational effects. In order to better isolate the BAO signal, we study several 2PCF μ-wedges (with a restricted range of orientations μ) tailored to address the systematics effects and we compare them with different definitions of radial 2PCFs. Finally, we discuss our findings in the context of an SKA-like survey, finding a clear BAO signal in most of the estimators here proposedes_ES
dc.format.extent19 pag.es_ES
dc.format.mimetypeapplication/pdfes_ES
dc.language.isoenges_ES
dc.publisherRoyal Astronomical Societyes_ES
dc.publisherOxford University Presses_ES
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyes_ES
dc.rights© 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Societyes_ES
dc.subject.otherGalaxies: Evolutiones_ES
dc.subject.otherGalaxies: Haloeses_ES
dc.subject.otherLarge-Scale Structure of Universees_ES
dc.subject.otherCosmology: Theoryes_ES
dc.subject.otherRadio Lines: Galaxieses_ES
dc.titleH I IM correlation function from UNIT simulations: BAO and observationally induced anisotropyes_ES
dc.typearticlees_ES
dc.subject.ecienciaFísicaes_ES
dc.relation.publisherversionhttps://doi.org/10.1093/mnras/stab3406es_ES
dc.identifier.doi10.1093/mnras/stab3406es_ES
dc.identifier.publicationfirstpage292es_ES
dc.identifier.publicationissue1es_ES
dc.identifier.publicationlastpage308es_ES
dc.identifier.publicationvolume510es_ES
dc.relation.projectIDinfo:eu-repo/grantAgreement/EC/H2020/713366/EU//InterTalentumes_ES
dc.relation.projectIDGobierno de España. PGC2018-094975-C21es_ES
dc.type.versioninfo:eu-repo/semantics/acceptedVersiones_ES
dc.rights.accessRightsopenAccesses_ES
dc.facultadUAMFacultad de Cienciases_ES
dc.institutoUAMInstituto de Física Teórica (IFT)es_ES
dc.institutoUAMCentro de Investigación Avanzada en Física Fundamental (CIAFF)es_ES


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