EDP Sciences
Free access
Issue A&A
Volume 391, Number 1, August III 2002
Page(s) 361 - 368
Section Instruments, observational techniques and data processing
DOI http://dx.doi.org/10.1051/0004-6361:20020552

A&A 391, 361-368 (2002)
DOI: 10.1051/0004-6361:20020552

Wavelet tomography of the Galactic magnetic field

I. The method
R. Stepanov1, P. Frick1, A. Shukurov2 and D. Sokoloff3

1  Institute of Continuous Media Mechanics, Korolyov str. 1, 614061 Perm, Russia
2  Department of Mathematics, University of Newcastle, Newcastle upon Tyne NE1 7RU, UK
3  Department of Physics, Moscow University, 119992, Moscow, Russia

(Received 8 June 2001 / Accepted 11 March 2002)

We suggest a two-dimensional wavelet devised to deduce the large-scale structure of a physical field (e.g., the Galactic magnetic field) from its integrals along straight paths from irregularly spaced data points to a fixed interior point (the observer). The method can be applied to the analysis of pulsar rotation and dispersion measures in terms of the large-scale Galactic magnetic field and electron density. The method does not use any a priori assumptions about the physical field and can be considered as an algorithm of wavelet differentiation. We argue that a certain combination of the wavelet transformation with model fitting would be most efficient in the interpretation of the available pulsar ${\it RM}$ data.

Key words: ISM: magnetic fields -- polarization -- methods: data analysis -- Galaxy: structure

Offprint request: R. Stepanov, rodion@icmm.ru

© ESO 2002

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Editor-in-Chief: T. Forveille
Letters Editor-in-Chief: J. Alves
Managing Editor: C. Bertout

ISSN: 0004-6361 ; e-ISSN: 1432-0746
Frequency: 12 volumes per year
Published by: EDP Sciences

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