Constraining galaxy-halo connection with high-order statistics

We investigate using three-point statistics in constraining the galaxy–halo connection. We show that for some galaxy samples, the constraints on the halo occupation distribution parameters are dominated by the three-point function signal (over its two-point counterpart). We demonstrate this on mock...

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Detalhes bibliográficos
Autores: Zhang, Hanyu, Samushia, Lado, Brooks, David, Macorra, Axel de la, Doel, Peter, Gaztañaga, Enrique, Gontcho, Satya, Honscheid, Klaus, Kehoe, Robert, Kisner, Theodore, Meisner, Aaron, Poppett, Claire L., Schubnell, Michael, Tarlé, Gregory, Zhang, Kai, Zou, Hu
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2022
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/296564
Acesso em linha:http://hdl.handle.net/10261/296564
Access Level:acceso abierto
Palavra-chave:Cosmology: theory
Galaxies: haloes
Large-scale structure of the universe
Descrição
Resumo:We investigate using three-point statistics in constraining the galaxy–halo connection. We show that for some galaxy samples, the constraints on the halo occupation distribution parameters are dominated by the three-point function signal (over its two-point counterpart). We demonstrate this on mock catalogues corresponding to the Luminous red galaxies (LRGs), Emission-line galaxies (ELGs), and quasars (QSOs) targeted by the Dark Energy Spectroscopic Instrument (DESI) Survey. The projected three-point function for triangle sides less up to 20 h−1 Mpc measured from a cubic Gpc of data can constrain the characteristic minimum mass of the LRGs with a preci sion of 0.46 per cent. For comparison, similar constraints from the projected two-point function are 1.55 per cent. The improvements for the ELGs and QSOs targets are more modest. In the case of the QSOs, it is caused by the high shot-noise of the sample, and in the case of the ELGs, it is caused by the range of halo masses of the host haloes. The most time-consuming part of our pipeline is the measurement of the three-point functions. We adopt a tabulation method, proposed in earlier works for the two-point function, to significantly reduce the required compute time for the three-point analysis.

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