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

C.H. Chuang, C. Zhao, F. Prada, E. Munari, S. Avila, A. Izard, F.S. Kitaura, M. Manera, P. Monaco, S. Murray, A. Knebe, C.G. Scóccola, G. Yepes, J. Garcia-Bellido, F.A. Marín, V. Müller, R. Skibba, M. Crocce, P. Fosalba, S. Gottlöber & 4 others A.A. Klypin, Chris Power, C. Tao, V. Turchaninov

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Abstract

© 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. 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.
Original languageEnglish
Pages (from-to)686-700
JournalMonthly Notices of the Royal Astronomical Society
Volume452
Issue number1
Early online date8 Jul 2015
DOIs
Publication statusPublished - 1 Sep 2015

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cosmology
catalogs
halos
statistics
galaxies
power spectra
simulation
methodology
acoustics
oscillation
perturbation
baryons
perturbation theory
quadrupoles
oscillations
comparison
project
estimates

Cite this

Chuang, C. H., Zhao, C., Prada, F., Munari, E., Avila, S., Izard, A., ... Turchaninov, V. (2015). nIFTy cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics. Monthly Notices of the Royal Astronomical Society, 452(1), 686-700. https://doi.org/10.1093/mnras/stv1289
Chuang, C.H. ; Zhao, C. ; Prada, F. ; Munari, E. ; Avila, S. ; Izard, A. ; Kitaura, F.S. ; Manera, M. ; Monaco, P. ; Murray, S. ; Knebe, A. ; Scóccola, C.G. ; Yepes, G. ; Garcia-Bellido, J. ; Marín, F.A. ; Müller, V. ; Skibba, R. ; Crocce, M. ; Fosalba, P. ; Gottlöber, S. ; Klypin, A.A. ; Power, Chris ; Tao, C. ; Turchaninov, V. / nIFTy cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics. In: Monthly Notices of the Royal Astronomical Society. 2015 ; Vol. 452, No. 1. pp. 686-700.
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Chuang, CH, Zhao, C, Prada, F, Munari, E, Avila, S, Izard, A, Kitaura, FS, Manera, M, Monaco, P, Murray, S, Knebe, A, Scóccola, CG, Yepes, G, Garcia-Bellido, J, Marín, FA, Müller, V, Skibba, R, Crocce, M, Fosalba, P, Gottlöber, S, Klypin, AA, Power, C, Tao, C & Turchaninov, V 2015, 'nIFTy cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics' Monthly Notices of the Royal Astronomical Society, vol. 452, no. 1, pp. 686-700. https://doi.org/10.1093/mnras/stv1289

nIFTy cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics. / Chuang, C.H.; Zhao, C.; Prada, F.; Munari, E.; Avila, S.; Izard, A.; Kitaura, F.S.; Manera, M.; Monaco, P.; Murray, S.; Knebe, A.; Scóccola, C.G.; Yepes, G.; Garcia-Bellido, J.; Marín, F.A.; Müller, V.; Skibba, R.; Crocce, M.; Fosalba, P.; Gottlöber, S.; Klypin, A.A.; Power, Chris; Tao, C.; Turchaninov, V.

In: Monthly Notices of the Royal Astronomical Society, Vol. 452, No. 1, 01.09.2015, p. 686-700.

Research output: Contribution to journalArticle

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T1 - nIFTy cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics

AU - Chuang, C.H.

AU - Zhao, C.

AU - Prada, F.

AU - Munari, E.

AU - Avila, S.

AU - Izard, A.

AU - Kitaura, F.S.

AU - Manera, M.

AU - Monaco, P.

AU - Murray, S.

AU - Knebe, A.

AU - Scóccola, C.G.

AU - Yepes, G.

AU - Garcia-Bellido, J.

AU - Marín, F.A.

AU - Müller, V.

AU - Skibba, R.

AU - Crocce, M.

AU - Fosalba, P.

AU - Gottlöber, S.

AU - Klypin, A.A.

AU - Power, Chris

AU - Tao, C.

AU - Turchaninov, V.

PY - 2015/9/1

Y1 - 2015/9/1

N2 - © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. 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.

AB - © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. 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.

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DO - 10.1093/mnras/stv1289

M3 - Article

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SP - 686

EP - 700

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

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