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
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/77652
Ver los metadatos del registro completo
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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 Técnicas2025-10-22T11:46:56Zoai: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:34982025-10-22 11:46:56.989CONICET 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) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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12.982451 |