Open AccessCosmology with the Planck cluster sample
Author(s) -
Geisbüsch Jörn,
Hobson Michael P.
Publication year - 2007
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2007.12169.x
Subject(s) - physics , planck , cosmic microwave background , astrophysics , redshift , galaxy cluster , cosmology , cold dark matter , dark energy , cluster (spacecraft) , cosmic background radiation , observational cosmology , dark matter , matter power spectrum , hubble's law , galaxy , astronomy , anisotropy , quantum mechanics , computer science , programming language
It has been long recognized that, besides being a formidable experiment to observe the primordial cosmic microwave background (CMB) anisotropies, Planck will also have the capability to detect galaxy clusters via their Sunyaev–Zel'dovich (SZ) imprint. In this paper constraints on cosmological parameters derivable from the Planck cluster candidate sample are examined for the first time as a function of cluster sample selection and purity obtained from realistic simulations of the microwave sky at the Planck observing frequency bands, observation process modelling and a cluster extraction pipeline. In particular, we employ a multifrequency matched filtering (MFMF) method to recover clusters from mock simulations of Planck observations. Obtainable cosmological constraints under realistic assumptions of priors and knowledge about cluster redshifts are discussed. Just relying on cluster redshift abundances without making use of recovered cluster fluxes, it is shown that from the Planck cluster catalogue cosmological constraints comparable to the ones derived from recent primordial CMB power spectrum measurements can be achieved. For example, for a concordance Λ cold dark matter (ΛCDM) model and a redshift binning of Δ z = 0.1 , the 1σ uncertainties on the values of Ω m and σ 8 are ΔΩ m ≈ 0.031 and Δσ 8 ≈ 0.014 , respectively. Furthermore, we find that the constraint of the matter density depends strongly on the prior which can be imposed on the Hubble parameter by other observational means.