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G.J. Larson, E.F. Bunn, V. Kasliwal, M. McCann (University of Richmond)
Galactic dust is a major contaminant in CMB anisotropy data sets. Dust maps contain well-localized filamentary structures, in contrast to the diffuse, Gaussian structure of CMB anisotropy. As a result, dust maps are highly compressible in both wavelet and radon transform bases. It is therefore plausible that low levels of dust contamination would be easier to diagnose and remove by examining a contaminated map in wavelet or radon bases.
We examine simulated CMB maps with known amounts of dust contamination in a variety of different wavelet and radon transform bases. We quantitatively assess which wavelet families are most efficient at compressing dust maps (keeping the largest fraction of dust power in the fewest wavelet coefficients). We also assess whether low levels of dust contamination are more easily diagnosed by filtering the maps to keep only the ``dustiest'' wavelet and radon coefficients.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.