Wavelet tomography of the Galactic magnetic field. I. The method

Abstract

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 RM data.

arXiv comment8 pages, 12 Postscript figures, submitted to A&A

References in corpus (3)

• Structures in the RM sky
• Binary and Millisecond Pulsars at the New Millennium
• HI line measurements of pulsars towards the Galactic Centre and the electron density in the inner Galaxy

Cited by in corpus (5)

• The Origin and Evolution of Cosmic Magnetism
• Magnetic Fields in the Milky Way
• Observations of magnetic fields in the Milky Way and in nearby galaxies with a Square Kilometre Array
• The Square Kilometre Array: A new probe of cosmic magnetism
• Probing magnetic fields with Square Kilometre array and its precursors