EDP Sciences
Free access
Volume 401, Number 1, April I 2003
Page(s) 389 - 404
Section Physical and chemical processes
DOI http://dx.doi.org/10.1051/0004-6361:20030099

A&A 401, 389-404 (2003)
DOI: 10.1051/0004-6361:20030099

Digital deblurring of CMB maps: Performance and efficient implementation

R. Vio1, 2, J. G. Nagy3, L. Tenorio4, P. Andreani5, C. Baccigalupi6 and W. Wamsteker2

1  Chip Computers Consulting s.r.l., Viale Don L. Sturzo 82, S. Liberale di Marcon, 30020 Venice, Italy
2  ESA-VILSPA, Apartado 50727, 28080 Madrid, Spain
    e-mail: willem.wamsteker@esa.int
3  Department of Mathematics and Computer Science, Emory University, Atlanta, GA 30322, USA
    e-mail: nagy@mathcs.emory.edu
4  Department of Mathematical and Computer Sciences, Colorado School of Mines, Golden CO 80401, USA
    e-mail: ltenorio@Mines.EDU
5  Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, 35122 Padua, Italy
    e-mail: andreani@pd.astro.it
6  SISSA/ISAS, Via Beirut 4, 34014 Trieste, Italy
    e-mail: bacci@sissa.it

(Received 30 August 2002 / Accepted 14 January 2003)

Digital deblurring of images is an important problem that arises in multifrequency observations of the Cosmic Microwave Background (CMB) where, because of the width of the point spread functions (PSF), maps at different frequencies suffer a different loss of spatial resolution. Deblurring is useful for various reasons: first, it helps to restore high frequency components lost through the smoothing effect of the instrument's PSF; second, emissions at various frequencies observed with different resolutions can be better studied on a comparable resolution; third, some map-based component separation algorithms require maps with similar level of degradation. Because of computational efficiency, deblurring is usually done in the frequency domain. But this approach has some limitations as it requires spatial invariance of the PSF, stationarity of the noise, and is not flexible in the selection of more appropriate boundary conditions. Deblurring in real space is more flexible but usually not used because of its high computational cost. In this paper (the first in a series on the subject) we present new algorithms that allow the use of real space deblurring techniques even for very large images. In particular, we consider the use of Tikhonov deblurring of noisy maps with applications to PLANCK. We provide details for efficient implementations of the algorithms. Their performance is tested on Gaussian and non-Gaussian simulated CMB maps, and PSFs with both circular and elliptical symmetry. Matlab code is made available.

Key words: methods: data analysis -- methods: statistical -- cosmology: cosmic microwave background

Offprint request: R. Vio, robertovio@tin.it

© ESO 2003

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