Abstract

Component separation is one of the key stages of any modern cosmic microwave background data analysis pipeline. It is an inherently nonlinear procedure and typically involves a series of sequential solutions of linear systems with similar but not identical system matrices, derived for different data models of the same data set. Sequences of this type arise, for instance, in the maximization of the data likelihood with respect to foreground parameters or sampling of their posterior distribution. However, they are also common in many other contexts. In this work we consider solving the component separation problem directly in the measurement (time-) domain. This can have a number of important benefits over the more standard pixel-based methods, in particular if non-negligible time-domain noise correlations are present, as is commonly the case. The approach based on the time-domain, however, implies significant computational effort because the full volume of the time-domain data set needs to be manipulated. To address this challenge, we propose and study efficient solvers adapted to solving time-domain-based component separation systems and their sequences, and which are capable of capitalizing on information derived from the previous solutions. This is achieved either by adapting the initial guess of the subsequent system or through a so-called subspace recycling, which allows constructing progressively more efficient two-level preconditioners. We report an overall speed-up over solving the systems independently of a factor of nearly 7, or 5, in our numerical experiments, which are inspired by the likelihood maximization and likelihood sampling procedures, respectively.

Highlights

  • Measurements registered by cosmic microwave background (CMB) experiments contain, in addition to the sought-after signal of cosmological origin, contributions from astrophysical sources

  • It is commonly performed in a pixel domain and uses maps of the sky estimated for each frequency band and their statistical uncertainties as inputs

  • Where p(t) denotes the pixel observed at time t, we do not include the total intensity, and Qc and Uc stand for Q and U Stokes parameters of the combined, CMB + foregrounds, sky signal observed at frequency νc

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Summary

Context and motivation

Measurements registered by cosmic microwave background (CMB) experiments contain, in addition to the sought-after signal of cosmological origin, contributions from astrophysical sources. (Here λ is a time-domain noise correlation length and can reach many thousands of samples.) The full computations quickly become prohibitively expensive This is the case even if the explicit inversion of the covariance matrix is replaced by some iterative procedure, which typically requires O(niter n2pix) flops, where the number of iterations, niter is usually on the order of 102. A general solution to the problem would be to avoid relying on the frequency maps at all and to perform all the calculation directly on the time-domain data This would typically require memory on the order of O(nt) and O(p niter nt ln λ) flops. Material that is more technical in nature or that is added for completeness is as usual deferred to the appendices

Preliminaries
Data model
Component mixing
Block-diagonal preconditioner
PCG with deflation and two-level preconditioners
Effect of the eigenvalue multiplicity
Choice of the initial guess
Previous solution as the initial guess
Adapted previous solution as the new initial guess
Pointing matrix
Sky maps
Results
Conclusions and further perspectives
Approximating the eigenvalues using Krylov subspace methods
Ritz value and harmonic Ritz value approximations
Arnoldi and Lanczos methods
Restarted variants
Deflation and two-level preconditioners
Full Text
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