Kriging Interpolating Cosmic Velocity Field

Abstract

[abridged] Volume-weighted statistics of large scale peculiar velocity is preferred by peculiar velocity cosmology, since it is free of uncertainties of galaxy density bias entangled in mass-weighted statistics. However, measuring the volume-weighted velocity statistics from galaxy (halo/simulation particle) velocity data is challenging. For the first time, we apply the Kriging interpolation to obtain the volume-weighted velocity field. Kriging is a minimum variance estimator. It predicts the most likely velocity for each place based on the velocity at other places. We test the performance of Kriging quantified by the E-mode velocity power spectrum from simulations. Dependences on the variogram prior used in Kriging, the number $n_k$ of the nearby particles to interpolate and the density $n_P$ of the observed sample are investigated. First, we find that Kriging induces $1\%$ and $3\%$ systematics at $k\sim 0.1h{\mathrm{Mpc}}^{-1}$ when $n_P\sim 6\times 10^{-2}(\mathrm{Mpc}/h{)}^{-3}$ and $n_P\sim 6\times 10^{-3}(\mathrm{Mpc}/h{)}^{-3}$, respectively. The deviation increases for decreasing $n_P$ and increasing $k$. When $n_P\lesssim 6\times 10^{-4}(\mathrm{Mpc}/h{)}^{-3}$, a smoothing effect dominates small scales, causing significant underestimation of the velocity power spectrum. Second, increasing $n_k$ helps to recover small scale power. However, for $n_P\lesssim 6\times 10^{-4}(\mathrm{Mpc}/h{)}^{-3}$ cases, the recovery is limited. Finally, Kriging is more sensitive to the variogram prior for lower sample density. The most straightforward application of Kriging on the cosmic velocity field does not show obvious advantages over the nearest-particle method (Zheng et al. 2013) and could not be directly applied to cosmology so far. However, whether potential improvements may be achieved by more delicate versions of Kriging is worth further investigation.

11 pages, 5 figures, published in PRD

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• Evolution mapping II: describing statistics of the non-linear cosmic velocity field
• The Halo Boltzmann Equation
• Lagrangian displacement field estimators in cosmology
• Estimating power spectrum of discrete cosmic momentum field with fast Fourier transform