Volume 391, Number 1, August III 2002
|Page(s)||361 - 368|
|Section||Numerical methods and codes|
|Published online||29 July 2002|
Wavelet tomography of the Galactic magnetic field
I. The method
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
Corresponding author: R. Stepanov, email@example.com
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 data.
Key words: ISM: magnetic fields / polarization / methods: data analysis / Galaxy: structure
© ESO, 2002
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