Unbiased Reconstruction of the Large Scale Structure

Details Unbiased Reconstruction of the Large Scale Structure Unbiased Reconstruction of the Large Scale Structure

2000-10-27

arxiv.org/abs/astro-ph/0010561v2

Mon.Not.Roy.Astron.Soc. 331 (2002) 901

Astronomy and Astrophysics

Astrophysics

Revised version with new section and figures. To appear in MNRAS

Scientific paper

10.1046/j.1365-8711.2002.05229.x

We present a new Unbiased Minimal Variance (UMV) estimator for the purpose of reconstructing the large--scale structure of the universe from noisy, sparse and incomplete data. Similar to the Wiener Filter (WF), the UMV estimator is derived by requiring the linear minimal variance solution given the data and an assumed prior model specifying the underlying field covariance matrix. However, unlike the WF, the minimization is carried out with the added constraint of an unbiased reconstructed mean field. The new estimator does not necessitate a noise model to estimate the underlying field; however, such a model is required for evaluating the errors at each point in space. The general application of the UMV estimator is to predict the values of the reconstructed field in un-sampled regions of space (e.g., interpolation in the unobserved Zone of Avoidance), and to dynamically transform from one measured field to another (e.g., inversion of radial peculiar velocities to over-densities). Here, we provide two very simple applications of the method. The first, is to recover a 1D signal from noisy, convolved data with gaps, e.g., CMB time-ordered data. The second application is a reconstruction of the density and 3D peculiar velocity fields from mock SEcat galaxy peculiar velocity catalogs.

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