TY - JOUR
T1 - Constraining νΛCDM with density-split clustering
AU - Paillas, Enrique
AU - Cuesta-Lazaro, Carolina
AU - Zarrouk, Pauline
AU - Cai, Yan Chuan
AU - Percival, Will J.
AU - Nadathur, Seshadri
AU - Pinon, Mathilde
AU - de Mattia, Arnaud
AU - Beutler, Florian
N1 - Funding Information:
We would like to thank Elena Massara, Zhongxu Zhai, Baojiu Li, Ravi Sheth, Ariel Sánchez, and Oliver Philcox for helpful discussions. We acknowledge the use of MATPLOTLIB (Hunter 2007), SCIPY (Virtanen et al. 2020), and ASTROPY (Astropy Collaboration 2013, 2018) throughout the course of this work. This research was enabled in part by support provided by Compute Ontario (computeontario.ca) and the Digital Research Alliance of Canada (alliancecan.ca). Research at Perimeter Institute is supported in part by the Government of Canada through the Department of Innovation, Science and Economic Development Canada and by the Province of Ontario through the Ministry of Colleges and Universities. SN acknowledges support from an STFC Ernest Rutherford Fellowship, grant reference ST/T005009/2. YC acknowledges the support of the Royal Society through the award of a University Research Fellowship and an Enhancement Award. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement 853291). FB is a University Research Fellow. This work used the DiRAC@Durham facility managed by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). For the purpose of open access, the authors have applied a CC BY public copyright licence to any Author Accepted Manuscript version arising.
Publisher Copyright:
© 2023 The Author(s).
PY - 2023/6/1
Y1 - 2023/6/1
N2 - The dependence of galaxy clustering on local density provides an effective method for extracting non-Gaussian information from galaxy surveys. The two-point correlation function (2PCF) provides a complete statistical description of a Gaussian density field. However, the late-time density field becomes non-Gaussian due to non-linear gravitational evolution and higher-order summary statistics are required to capture all of its cosmological information. Using a Fisher formalism based on halo catalogues from the Quijote simulations, we explore the possibility of retrieving this information using the density-split clustering (DS) method, which combines clustering statistics from regions of different environmental density. We show that DS provides more precise constraints on the parameters of the νΛCDM model compared to the 2PCF, and we provide suggestions for where the extra information may come from. DS improves the constraints on the sum of neutrino masses by a factor of 7 and by factors of 4, 3, 3, 6, and 5 for Ωm, Ωb, h, ns, and σ8, respectively. We compare DS statistics when the local density environment is estimated from the real or redshift-space positions of haloes. The inclusion of DS autocorrelation functions, in addition to the cross-correlation functions between DS environments and haloes, recovers most of the information that is lost when using the redshift-space halo positions to estimate the environment. We discuss the possibility of constructing simulation-based methods to model DS clustering statistics in different scenarios.
AB - The dependence of galaxy clustering on local density provides an effective method for extracting non-Gaussian information from galaxy surveys. The two-point correlation function (2PCF) provides a complete statistical description of a Gaussian density field. However, the late-time density field becomes non-Gaussian due to non-linear gravitational evolution and higher-order summary statistics are required to capture all of its cosmological information. Using a Fisher formalism based on halo catalogues from the Quijote simulations, we explore the possibility of retrieving this information using the density-split clustering (DS) method, which combines clustering statistics from regions of different environmental density. We show that DS provides more precise constraints on the parameters of the νΛCDM model compared to the 2PCF, and we provide suggestions for where the extra information may come from. DS improves the constraints on the sum of neutrino masses by a factor of 7 and by factors of 4, 3, 3, 6, and 5 for Ωm, Ωb, h, ns, and σ8, respectively. We compare DS statistics when the local density environment is estimated from the real or redshift-space positions of haloes. The inclusion of DS autocorrelation functions, in addition to the cross-correlation functions between DS environments and haloes, recovers most of the information that is lost when using the redshift-space halo positions to estimate the environment. We discuss the possibility of constructing simulation-based methods to model DS clustering statistics in different scenarios.
KW - cosmological parameters
KW - large-scale structure of Universe
UR - http://www.scopus.com/inward/record.url?scp=85159782867&partnerID=8YFLogxK
U2 - 10.1093/mnras/stad1017
DO - 10.1093/mnras/stad1017
M3 - Article
AN - SCOPUS:85159782867
SN - 0035-8711
VL - 522
SP - 606
EP - 625
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 1
ER -