A joint 2-and 3-point clustering analysis of the VIPERS PDR2 catalogue at z ∼ 1: Breaking the degeneracy of cosmological parameters

We measure the galaxy two- and three-point correlation functions at z = [0.5, 0.7] and z = [0.7, 0.9], from the Public Data Release 2 (PDR2) of the VIMOS Public Extragalactic Redshift Survey (VIPERS). We model the two statistics including a non-linear one-loop model for the two-point function and a...

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Detalles Bibliográficos
Autores: Veropalumbo, Alfonso, Sáez Casares, Iñigo, Branchini, Enzo, Granett, Benjamin R., Guzzo, Luigi, Marulli, Federico, Moresco, Michele, Moscardini, Lauro, Pezzotta, Andrea, Torre, Sylvain de la
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2021
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/253866
Acceso en línea:http://hdl.handle.net/10261/253866
Access Level:acceso abierto
Palabra clave:Galaxies: statistics
Large-scale structure of the universe
Cosmology: observations
Descripción
Sumario:We measure the galaxy two- and three-point correlation functions at z = [0.5, 0.7] and z = [0.7, 0.9], from the Public Data Release 2 (PDR2) of the VIMOS Public Extragalactic Redshift Survey (VIPERS). We model the two statistics including a non-linear one-loop model for the two-point function and a tree-level model for the three-point function, and perform a joint likelihood analysis. The entire process and non-linear corrections are tested and validated through the use of the 153 highly realistic VIPERS mock catalogues, showing that they are robust down to scales as small as 10 h-1 Mpc. The mocks are also adopted to compute the covariance matrix that we use for the joint two- and three-point analysis. Despite the limited statistics of the two (volume-limited) subsamples analysed, we demonstrate that such a combination successfully breaks the degeneracy existing at two-point level between clustering amplitude σ8, linear bias b1, and the linear growth rate of fluctuations f. For the latter, in particular, we measure f(z=0.61)=0.64+0.55-0.37 and f(z = 0.8) = 1.0 ± 1.0, while the amplitude of clustering is found to be σ8(z = 0.61) = 0.50 ± 0.12 and σ8(z=0.8)=0.39+0.11-0.13}. These values are in excellent agreement with the extrapolation of a Planck cosmology.

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