nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics

Autores
Chuang, Chia Hsun; Zhao, Cheng; Prada, Francisco; Munari, Emiliano; Avila, Santiago; Izard, Albert; Kitaura, Francisco Shu; Manera, Marc; Monaco, Pierluigi; Murray, Steven; Knebe, Alexander; Scoccola, Claudia Graciela; Yepes, Gustavo; Garcia Bellido, Juan; Marín, Felipe A.; Müller, Volker; Skibba, Ramin; Crocce, Martin; Fosalba, Pablo; Gottlöber, Stefan; Klypin, Anatoly A.; Power, Chris; Tao, Charling; Turchaninov, Victor
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present a comparison of major methodologies of fast generating mock halo or galaxy catalogues. The comparison is done for two-point (power spectrum and two-point correlation function in real and redshift space), and the three-point clustering statistics (bispectrum and three-point correlation function). The reference catalogues are drawn from the BigMultiDark N-body simulation. Both friend-of-friends (including distinct haloes only) and spherical overdensity (including distinct haloes and subhalos) catalogues have been used with the typical number density of a large volume galaxy surveys. We demonstrate that a proper biasing model is essential for reproducing the power spectrum at quasi-linear and even smaller scales. With respect to various clustering statistics, a methodology based on perturbation theory and a realistic biasing model leads to very good agreement with N-body simulations. However, for the quadrupole of the correlation function or the power spectrum, only the method based on semi-N-body simulation could reach high accuracy (1 per cent level) at small scales, i.e. r < 25 h-1 Mpc or k > 0.15 h Mpc-1. Full N-body solutions will remain indispensable to produce reference catalogues. Nevertheless, we have demonstrated that the more efficient approximate solvers can reach a few per cent accuracy in terms of clustering statistics at the scales interesting for the large-scale structure analysis. This makes them useful for massive production aimed at covariance studies, to scan large parameter spaces, and to estimate uncertainties in data analysis techniques, such as baryon acoustic oscillation reconstruction, redshift distortion measurements, etc.
Fil: Chuang, Chia Hsun. Universidad Autónoma de Madrid; España. Consejo Superior de Investigaciones Científicas; España
Fil: Zhao, Cheng. Tsinghua University; China
Fil: Prada, Francisco. Consejo Superior de Investigaciones Científicas; España. Universidad Autónoma de Madrid; España
Fil: Munari, Emiliano. Università degli Studi di Trieste; Italia. Istituto Nazionale di Astrofisica. Osservatorio astronomico di Trieste; Italia
Fil: Avila, Santiago. Consejo Superior de Investigaciones Científicas; España. Universidad Autónoma de Madrid; España
Fil: Izard, Albert. Consejo Superior de Investigaciones Científicas; España. Universitat Autònoma de Barcelona; España
Fil: Kitaura, Francisco Shu. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Manera, Marc. University College London; Reino Unido
Fil: Monaco, Pierluigi. Università degli Studi di Trieste; Italia. Istituto Nazionale di Astrofisica. Osservatorio astronomico di Trieste; Italia
Fil: Murray, Steven. University of Western Australia; Australia. ARC Centre of Excellence for All-Sky Astrophysics; Australia
Fil: Knebe, Alexander. Universidad Autónoma de Madrid; España
Fil: Scoccola, Claudia Graciela. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Área Física Teórica; Argentina
Fil: Yepes, Gustavo. Universidad Autónoma de Madrid; España
Fil: Garcia Bellido, Juan. Universidad Autónoma de Madrid; España
Fil: Marín, Felipe A.. University of Technology; Australia. Consejo Superior de Investigaciones Científicas; España
Fil: Müller, Volker. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Skibba, Ramin. University of California; Estados Unidos
Fil: Crocce, Martin. Universitat Autònoma de Barcelona; España
Fil: Fosalba, Pablo. Universitat Autònoma de Barcelona; España
Fil: Gottlöber, Stefan. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Klypin, Anatoly A.. New Mexico State University; Estados Unidos
Fil: Power, Chris. University of Western Australia; Australia. ARC Centre of Excellence for All-Sky Astrophysics; Australia
Fil: Tao, Charling. Tsinghua University; China. Universite Aix-Marseille; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Turchaninov, Victor. Russian Academy of Sciences; Rusia
Materia
Cosmology: Observations
Distance Scale
Large-Scale Structure of Universe
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/77652

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spelling nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statisticsChuang, Chia HsunZhao, ChengPrada, FranciscoMunari, EmilianoAvila, SantiagoIzard, AlbertKitaura, Francisco ShuManera, MarcMonaco, PierluigiMurray, StevenKnebe, AlexanderScoccola, Claudia GracielaYepes, GustavoGarcia Bellido, JuanMarín, Felipe A.Müller, VolkerSkibba, RaminCrocce, MartinFosalba, PabloGottlöber, StefanKlypin, Anatoly A.Power, ChrisTao, CharlingTurchaninov, VictorCosmology: ObservationsDistance ScaleLarge-Scale Structure of Universehttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present a comparison of major methodologies of fast generating mock halo or galaxy catalogues. The comparison is done for two-point (power spectrum and two-point correlation function in real and redshift space), and the three-point clustering statistics (bispectrum and three-point correlation function). The reference catalogues are drawn from the BigMultiDark N-body simulation. Both friend-of-friends (including distinct haloes only) and spherical overdensity (including distinct haloes and subhalos) catalogues have been used with the typical number density of a large volume galaxy surveys. We demonstrate that a proper biasing model is essential for reproducing the power spectrum at quasi-linear and even smaller scales. With respect to various clustering statistics, a methodology based on perturbation theory and a realistic biasing model leads to very good agreement with N-body simulations. However, for the quadrupole of the correlation function or the power spectrum, only the method based on semi-N-body simulation could reach high accuracy (1 per cent level) at small scales, i.e. r < 25 h-1 Mpc or k > 0.15 h Mpc-1. Full N-body solutions will remain indispensable to produce reference catalogues. Nevertheless, we have demonstrated that the more efficient approximate solvers can reach a few per cent accuracy in terms of clustering statistics at the scales interesting for the large-scale structure analysis. This makes them useful for massive production aimed at covariance studies, to scan large parameter spaces, and to estimate uncertainties in data analysis techniques, such as baryon acoustic oscillation reconstruction, redshift distortion measurements, etc.Fil: Chuang, Chia Hsun. Universidad Autónoma de Madrid; España. Consejo Superior de Investigaciones Científicas; EspañaFil: Zhao, Cheng. Tsinghua University; ChinaFil: Prada, Francisco. Consejo Superior de Investigaciones Científicas; España. Universidad Autónoma de Madrid; EspañaFil: Munari, Emiliano. Università degli Studi di Trieste; Italia. Istituto Nazionale di Astrofisica. Osservatorio astronomico di Trieste; ItaliaFil: Avila, Santiago. Consejo Superior de Investigaciones Científicas; España. Universidad Autónoma de Madrid; EspañaFil: Izard, Albert. Consejo Superior de Investigaciones Científicas; España. Universitat Autònoma de Barcelona; EspañaFil: Kitaura, Francisco Shu. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; AlemaniaFil: Manera, Marc. University College London; Reino UnidoFil: Monaco, Pierluigi. Università degli Studi di Trieste; Italia. Istituto Nazionale di Astrofisica. Osservatorio astronomico di Trieste; ItaliaFil: Murray, Steven. University of Western Australia; Australia. ARC Centre of Excellence for All-Sky Astrophysics; AustraliaFil: Knebe, Alexander. Universidad Autónoma de Madrid; EspañaFil: Scoccola, Claudia Graciela. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Área Física Teórica; ArgentinaFil: Yepes, Gustavo. Universidad Autónoma de Madrid; EspañaFil: Garcia Bellido, Juan. Universidad Autónoma de Madrid; EspañaFil: Marín, Felipe A.. University of Technology; Australia. Consejo Superior de Investigaciones Científicas; EspañaFil: Müller, Volker. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; AlemaniaFil: Skibba, Ramin. University of California; Estados UnidosFil: Crocce, Martin. Universitat Autònoma de Barcelona; EspañaFil: Fosalba, Pablo. Universitat Autònoma de Barcelona; EspañaFil: Gottlöber, Stefan. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; AlemaniaFil: Klypin, Anatoly A.. New Mexico State University; Estados UnidosFil: Power, Chris. University of Western Australia; Australia. ARC Centre of Excellence for All-Sky Astrophysics; AustraliaFil: Tao, Charling. Tsinghua University; China. Universite Aix-Marseille; Francia. Centre National de la Recherche Scientifique; FranciaFil: Turchaninov, Victor. Russian Academy of Sciences; RusiaWiley Blackwell Publishing, Inc2015-04-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/77652Chuang, Chia Hsun; Zhao, Cheng; Prada, Francisco; Munari, Emiliano; Avila, Santiago; et al.; nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 452; 1; 8-4-2015; 686-7000035-87111365-2966CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv1289info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/452/1/686/1749747info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1412.7729info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:16:47Zoai:ri.conicet.gov.ar:11336/77652instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:16:47.852CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics
title nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics
spellingShingle nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics
Chuang, Chia Hsun
Cosmology: Observations
Distance Scale
Large-Scale Structure of Universe
title_short nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics
title_full nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics
title_fullStr nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics
title_full_unstemmed nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics
title_sort nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics
dc.creator.none.fl_str_mv Chuang, Chia Hsun
Zhao, Cheng
Prada, Francisco
Munari, Emiliano
Avila, Santiago
Izard, Albert
Kitaura, Francisco Shu
Manera, Marc
Monaco, Pierluigi
Murray, Steven
Knebe, Alexander
Scoccola, Claudia Graciela
Yepes, Gustavo
Garcia Bellido, Juan
Marín, Felipe A.
Müller, Volker
Skibba, Ramin
Crocce, Martin
Fosalba, Pablo
Gottlöber, Stefan
Klypin, Anatoly A.
Power, Chris
Tao, Charling
Turchaninov, Victor
author Chuang, Chia Hsun
author_facet Chuang, Chia Hsun
Zhao, Cheng
Prada, Francisco
Munari, Emiliano
Avila, Santiago
Izard, Albert
Kitaura, Francisco Shu
Manera, Marc
Monaco, Pierluigi
Murray, Steven
Knebe, Alexander
Scoccola, Claudia Graciela
Yepes, Gustavo
Garcia Bellido, Juan
Marín, Felipe A.
Müller, Volker
Skibba, Ramin
Crocce, Martin
Fosalba, Pablo
Gottlöber, Stefan
Klypin, Anatoly A.
Power, Chris
Tao, Charling
Turchaninov, Victor
author_role author
author2 Zhao, Cheng
Prada, Francisco
Munari, Emiliano
Avila, Santiago
Izard, Albert
Kitaura, Francisco Shu
Manera, Marc
Monaco, Pierluigi
Murray, Steven
Knebe, Alexander
Scoccola, Claudia Graciela
Yepes, Gustavo
Garcia Bellido, Juan
Marín, Felipe A.
Müller, Volker
Skibba, Ramin
Crocce, Martin
Fosalba, Pablo
Gottlöber, Stefan
Klypin, Anatoly A.
Power, Chris
Tao, Charling
Turchaninov, Victor
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Cosmology: Observations
Distance Scale
Large-Scale Structure of Universe
topic Cosmology: Observations
Distance Scale
Large-Scale Structure of Universe
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We present a comparison of major methodologies of fast generating mock halo or galaxy catalogues. The comparison is done for two-point (power spectrum and two-point correlation function in real and redshift space), and the three-point clustering statistics (bispectrum and three-point correlation function). The reference catalogues are drawn from the BigMultiDark N-body simulation. Both friend-of-friends (including distinct haloes only) and spherical overdensity (including distinct haloes and subhalos) catalogues have been used with the typical number density of a large volume galaxy surveys. We demonstrate that a proper biasing model is essential for reproducing the power spectrum at quasi-linear and even smaller scales. With respect to various clustering statistics, a methodology based on perturbation theory and a realistic biasing model leads to very good agreement with N-body simulations. However, for the quadrupole of the correlation function or the power spectrum, only the method based on semi-N-body simulation could reach high accuracy (1 per cent level) at small scales, i.e. r < 25 h-1 Mpc or k > 0.15 h Mpc-1. Full N-body solutions will remain indispensable to produce reference catalogues. Nevertheless, we have demonstrated that the more efficient approximate solvers can reach a few per cent accuracy in terms of clustering statistics at the scales interesting for the large-scale structure analysis. This makes them useful for massive production aimed at covariance studies, to scan large parameter spaces, and to estimate uncertainties in data analysis techniques, such as baryon acoustic oscillation reconstruction, redshift distortion measurements, etc.
Fil: Chuang, Chia Hsun. Universidad Autónoma de Madrid; España. Consejo Superior de Investigaciones Científicas; España
Fil: Zhao, Cheng. Tsinghua University; China
Fil: Prada, Francisco. Consejo Superior de Investigaciones Científicas; España. Universidad Autónoma de Madrid; España
Fil: Munari, Emiliano. Università degli Studi di Trieste; Italia. Istituto Nazionale di Astrofisica. Osservatorio astronomico di Trieste; Italia
Fil: Avila, Santiago. Consejo Superior de Investigaciones Científicas; España. Universidad Autónoma de Madrid; España
Fil: Izard, Albert. Consejo Superior de Investigaciones Científicas; España. Universitat Autònoma de Barcelona; España
Fil: Kitaura, Francisco Shu. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Manera, Marc. University College London; Reino Unido
Fil: Monaco, Pierluigi. Università degli Studi di Trieste; Italia. Istituto Nazionale di Astrofisica. Osservatorio astronomico di Trieste; Italia
Fil: Murray, Steven. University of Western Australia; Australia. ARC Centre of Excellence for All-Sky Astrophysics; Australia
Fil: Knebe, Alexander. Universidad Autónoma de Madrid; España
Fil: Scoccola, Claudia Graciela. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Área Física Teórica; Argentina
Fil: Yepes, Gustavo. Universidad Autónoma de Madrid; España
Fil: Garcia Bellido, Juan. Universidad Autónoma de Madrid; España
Fil: Marín, Felipe A.. University of Technology; Australia. Consejo Superior de Investigaciones Científicas; España
Fil: Müller, Volker. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Skibba, Ramin. University of California; Estados Unidos
Fil: Crocce, Martin. Universitat Autònoma de Barcelona; España
Fil: Fosalba, Pablo. Universitat Autònoma de Barcelona; España
Fil: Gottlöber, Stefan. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Klypin, Anatoly A.. New Mexico State University; Estados Unidos
Fil: Power, Chris. University of Western Australia; Australia. ARC Centre of Excellence for All-Sky Astrophysics; Australia
Fil: Tao, Charling. Tsinghua University; China. Universite Aix-Marseille; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Turchaninov, Victor. Russian Academy of Sciences; Rusia
description We present a comparison of major methodologies of fast generating mock halo or galaxy catalogues. The comparison is done for two-point (power spectrum and two-point correlation function in real and redshift space), and the three-point clustering statistics (bispectrum and three-point correlation function). The reference catalogues are drawn from the BigMultiDark N-body simulation. Both friend-of-friends (including distinct haloes only) and spherical overdensity (including distinct haloes and subhalos) catalogues have been used with the typical number density of a large volume galaxy surveys. We demonstrate that a proper biasing model is essential for reproducing the power spectrum at quasi-linear and even smaller scales. With respect to various clustering statistics, a methodology based on perturbation theory and a realistic biasing model leads to very good agreement with N-body simulations. However, for the quadrupole of the correlation function or the power spectrum, only the method based on semi-N-body simulation could reach high accuracy (1 per cent level) at small scales, i.e. r < 25 h-1 Mpc or k > 0.15 h Mpc-1. Full N-body solutions will remain indispensable to produce reference catalogues. Nevertheless, we have demonstrated that the more efficient approximate solvers can reach a few per cent accuracy in terms of clustering statistics at the scales interesting for the large-scale structure analysis. This makes them useful for massive production aimed at covariance studies, to scan large parameter spaces, and to estimate uncertainties in data analysis techniques, such as baryon acoustic oscillation reconstruction, redshift distortion measurements, etc.
publishDate 2015
dc.date.none.fl_str_mv 2015-04-08
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/77652
Chuang, Chia Hsun; Zhao, Cheng; Prada, Francisco; Munari, Emiliano; Avila, Santiago; et al.; nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 452; 1; 8-4-2015; 686-700
0035-8711
1365-2966
CONICET Digital
CONICET
url http://hdl.handle.net/11336/77652
identifier_str_mv Chuang, Chia Hsun; Zhao, Cheng; Prada, Francisco; Munari, Emiliano; Avila, Santiago; et al.; nIFTy Cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 452; 1; 8-4-2015; 686-700
0035-8711
1365-2966
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv1289
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/452/1/686/1749747
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1412.7729
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
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reponame_str CONICET Digital (CONICET)
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instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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