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

DOI: 
10.1093/mnras/stv1289
Publication date: 
01/09/2015
Main author: 
Chuang C.-H.
IAA authors: 
Prada F.
Authors: 
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 C., Tao C., Turchaninov V.
Journal: 
Monthly Notices of the Royal Astronomical Society
Publication type: 
Article
Volume: 
452
Pages: 
686-700
Number: 
Abstract: 
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. © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Database: 
WOK
SCOPUS
ADS
URL: 
https://ui.adsabs.harvard.edu/#abs/2015MNRAS.452..686C/abstract
ADS Bibcode: 
2015MNRAS.452..686C
Keywords: 
Cosmology: observations; Distance scale; Large-scale structure of Universe