Constraining the halo bispectrum in real and redshift space from perturbation theory and non-linear stochastic bias
Entidad
UAM. Departamento de Física TeóricaEditor
Oxford University Press on behalf of the Royal Astronomical Society.Fecha de edición
2015-06-21Cita
10.1093/mnras/stv645
Monthly Notices of the Royal Astronomical Society 450.2 (2015): 1836-1845
ISSN
0035-8711 (print); 1365-2966 (online)DOI
10.1093/mnras/stv645Financiado por
HGM is grateful for support from the UK Science and Technology Facilities Council through the grant ST/I001204/1. CGS acknowledges funding from the Spanish Ministry of Economy and Competitiveness (MINECO) under the project AYA2012-3972-C02-01. CC and FP were supported by (MINECO) under the project AYA2012-3972-C02-01. CC and FP were supported by the Spanish MICINNs Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064 and AYA2010-21231-C02-01 grant, the Comunidad de Madrid under grant HEPHACOS S2009/ESP-1473, and Spanish MINECOs Centro de Excelencia Severo Ochoa Programme under grant SEV-2012-0249. GY and FP acknowledge support from the Spanish MINECO under research grants AYA2012-31101, FPA2012-34694, AYA2010-21231, Consolider Ingenio SyeC CSD2007-0050 and from Comunidad de Madrid under ASTROMADRID project (S2009/ESP-1496)Proyecto
Gobierno de España. AYA2012-3972-C02-01; Gobierno de España. CSD2009-00064; Gobierno de España. AYA2010-21231-C02- 01; Comunidad de Madrid. S2009/ESP-1473/HEPHACOS; Gobierno de España. AYA2012-31101; Gobierno de España. FPA2012-34694; Gobierno de España. AYA2010-21231; Gobierno de España. SEV-2012-0249; Gobierno de España. CSD2007-0050; Comunidad de Madrid. S2009/ESP-1496/ASTROMADRIDVersión del editor
http://dx.doi.org/10.1093/mnras/stv645Materias
Catalogues; Galaxies: clusters: general; Galaxies: statistics; Large-scale structure of Universe; FísicaNota
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2015 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reservedDerechos
© 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reservedResumen
We present a method to produce mock galaxy catalogues with efficient perturbation theory schemes, which match the number density, power spectra and bispectra in real and in redshift space from N-body simulations. The essential contribution of this work is the way in which we constrain the bias parameters of the PATCHY-code. In addition to aiming at reproducing the two-point statistics, we seek the set of bias parameters, which constrain the univariate halo probability distribution function (PDF) encoding higher order correlation functions. We demonstrate that halo catalogues based on the same underlying dark matter field with a fix halo number density, and accurately matching the power spectrum (within 2 per cent) can lead to very different bispectra depending on the adopted halo bias model. A model ignoring the shape of the halo PDF can lead to deviations up to factors of 2. The catalogues obtained additionally constraining the shape of the halo PDF can significantly lower the discrepancy in the three-point statistics, yielding closely unbiased bispectra both in real and in redshift space; which are in general compatible with those corresponding to an N-body simulation within 10 per cent (deviating at most up to 20 per cent). Our calculations show that the constant linear bias of ~2 for luminous red galaxy (LRG) like galaxies found in the power spectrum, mainly comes from sampling haloes in high-density peaks, choosing a high-density threshold rather than from a factor multiplying the dark matter density field. Our method contributes towards an efficient modelling of the halo/galaxy distribution required to estimate uncertainties in the clustering measurements from galaxy redshift surveys. We have also demonstrated that it represents a powerful tool to test various bias models
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Google Scholar:Kitaura, Francisco Shu
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Gil-Marín, Héctor
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Scóccola, Claudia G.
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Chuang, Chia Hsun
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Müller, Volker
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Yepes Alonso, Gustavo
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Prada, Francisco
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