Pavel D. Naselsky

Gauss - Legendre sky pixelization (GLESP) for CMB maps

A new scheme of sky pixelization is developed for CMB maps. The scheme is based on the Gauss–Legendre polynomials zeros and allows one to create strict orthogonal expansion of the map. A corresponding code has been implemented and comparison with other methods has been done.

Ionization History of the Cosmic Plasma in the Light of the Recent Cosmic Background Imager and Future Planck Data

This paper is devoted to the methods of the determination of cosmological parameters and distortions of ionization history from recent cosmic microwave background (CMB) observations. We show that the more complex models of kinetics of recombination with a few missing parameters describing the recombination process provide better agreement between the measured and the expected characteristics of the CMB anisotropy. In particular, we consider external sources of resonance and ionizing radiation and a model with strong clustering of the baryonic component. These factors can constrain the estimates of the cosmological parameters usually discussed. We also demonstrate that the measurements of the CMB polarization can improve these estimates and, for the precision expected from the Planck mission, allow the discrimination of a wide class of models.

An adaptive filter for the construction of the Planck Compact Source Catalogue

We develop a linear algorithm for extracting extragalactic point sources for the Compact Source Catalogue of the upcoming PLANCK mission. This algorithm is based on a simple top-hat filter in the harmonic domain with an adaptive filtering range which does not require a priori knowledge of the CMB power spectrum and the experiment parameters such as the beam size and shape nor pixel noise level.

Ionization history of the universe as a test for superheavy dark matter particles

In this paper we discuss the possible distortions of the ionization history of the universe caused by an injection of nonthermal energy due to decays of hypothetical superheavy dark matter (SHDM) particles. These particles are usually considered as a possible source of ultrahigh energy cosmic rays in the framework of the top-down model. Estimates of the fraction of energy of decays converted to the UV range show that, for suitable parameters of the SHDM particles, significant distortions of the power spectra of the cosmic microwave background anisotropy appear. A comparison with the observed power spectrum allows us to restrict some properties of the SHDM particles. These decays can also increase by about 5char21{}10 times the degree of ionization of hydrogen at redshifts

General Statistical Properties of the Cosmic Microwave Background Polarization Field

zensuremath{sim}10char21{}50,

Amplitude-Phase Analysis of Cosmic Microwave Background Maps

which essentially accelerates the formation of molecules of

A combined multifrequency map for point source subtraction

{mathrm{H}}_{2}

The primordial baryonic clouds and their contribution to the cosmic microwave background anisotropy and polarization formation

and the first stars during the ``dark ages.

Asymmetry of the PLANCK antenna beam shape and its manifestation in the CMB data

The distribution of the polarization of the cosmic microwave background (CMB) in the sky is determined by the hypothesis of random Gaussian distribution of the primordial density perturbations. This hypotheses is well motivated by the inflationary cosmology. Therefore, a test of the consistency of the statistical properties of the CMB polarization field with the Gaussianity of primordial density fluctuations is a realistic way to study the nature of primordial inhomogeneities in the universe. This paper contains theoretical predictions of the general statistical properties of the CMB polarization field. All results were obtained under the assumption of the Gaussian nature of the signal. We pay special attention to the following two problems: first, the classification and statistics of the singular points of the polarization field where polarization is equal to zero, and second, the topology of the contours of the value of the degree of polarization. We have investigated the percolation properties for the zones of strong and weak polarization. We have also calculated Minkowski functionals for the CMB polarization field. All results are analytical.The distribution of the polarization of the Cosmic Microwave Background (CMB) in the sky is determined by the hypothesis of random Gaussian distribution of the primordial density perturbations. This hypotheses is well motivated by the inflationary cosmology. Therefore, the test of consistency of the statistical properties of the CMB polarization field with the Gaussianity of primordial density fluctuations is a realistic way to study the nature of primordial inhomogeneities in the Universe. This paper contains the theoretical predictions of the general statistical properties of the CMB polarization field. All results obtained under assumption of the Gaussian nature of the signal. We pay the special attention to the following two problems. First, the classification and statistics of the singular points of the polarization field where polarization is equal to zero. Second, the topology of contours of the value of the degree of polarization. We have investigated the percolation properties for the zones of ``strong and ``weak polarization. We also have calculated Minkowski functionals for the CMB polarization field. All results are analytical.

POWER FILTRATION OF CMB OBSERVATIONAL DATA

We propose a method for the extraction of point sources from cosmic microwave background (CMB) maps. This method is based on the analysis of the phase distribution of the Fourier components for the observed signal and relatively high peaks in the ΔT/T maps. The aim of our paper is to show how, using our algorithm, the contribution from point sources can be separated from the resulting signal on all scales. Our approach can, therefore, complement other methods of CMB power-spectrum reconstruction for future high-resolution maps and can be used as a tool to produce a catalog of point sources based on future Planck data.