An estimation of the Local growth rate from Cosmicflows peculiar velocities. (arXiv:1901.03530v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dupuy_A/0/1/0/all/0/1">A. Dupuy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Courtois_H/0/1/0/all/0/1">H. M. Courtois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graziani_R/0/1/0/all/0/1">R. Graziani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kubik_B/0/1/0/all/0/1">B. Kubik</a>
This article explores three usual estimators, noted as $v_{12}$, $psi_1$ and
$psi_2$, of the observed two-point galaxy peculiar velocity correlation
functions. These estimators are tested on mock samples of Cosmicflows-3 dataset
(Tully et al. 2016) , derived from a numerical cosmological simulation, and
also on a number of constrained realizations of this dataset. Observational
measurements errors and cosmic variance are taken into consideration in the
study. The result is a local measurement of $f sigma_8 = 0.43 left( pm 0.03
right)_mathrm{obs} left( pm 0.11 right)_mathrm{cosmic}$ out to $z=0.05$,
in support of a $Lambda$CDM cosmology.
This article explores three usual estimators, noted as $v_{12}$, $psi_1$ and
$psi_2$, of the observed two-point galaxy peculiar velocity correlation
functions. These estimators are tested on mock samples of Cosmicflows-3 dataset
(Tully et al. 2016) , derived from a numerical cosmological simulation, and
also on a number of constrained realizations of this dataset. Observational
measurements errors and cosmic variance are taken into consideration in the
study. The result is a local measurement of $f sigma_8 = 0.43 left( pm 0.03
right)_mathrm{obs} left( pm 0.11 right)_mathrm{cosmic}$ out to $z=0.05$,
in support of a $Lambda$CDM cosmology.
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