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FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE * OBSERVATIONS: GALACTIC FOREGROUND EMISSION

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B. Gold1, C. L. Bennett1, R. S. Hill2, G. Hinshaw3, N. Odegard2, L. Page4, D. N. Spergel5,6, J. L. Weiland2, J. Dunkley4,6,7, M. Halpern8, N. Jarosik4, A. Kogut3, E. Komatsu9, D. Larson1, S. S. Meyer10, M. R. Nolta11, E. Wollack3 and E. L. Wright12

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We present a new estimate of foreground emission in the Wilkinson Microwave Anisotropy Probe (WMAP) data, using a Markov chain Monte Carlo method. The new technique delivers maps of each foreground component for a variety of foreground models with estimates of the uncertainty of each foreground component, and it provides an overall goodness-of-fit estimate. The resulting foreground maps are in broad agreement with those from previous techniques used both within the collaboration and by other authors. We find that for WMAP data, a simple model with power-law synchrotron, free-free, and thermal dust components fits 90% of the sky with a reduced χ2 ν of 1.14. However, the model does not work well inside the Galactic plane. The addition of either synchrotron steepening or a modified spinning dust model improves the fit. This component may account for up to 14% of the total flux at the Ka band (33 GHz). We find no evidence for foreground contamination of the cosmic microwave background temperature map in the 85% of the sky used for cosmological analysis.


Footnote
WMAP is the result of a partnership between Princeton University and NASA's Goddard Space Flight Center. Scientific guidance is provided by the WMAP Science Team.
Keywords

cosmic microwave background; cosmology: observations; diffuse radiation; Galaxy: halo; Galaxy: structure; ISM: structure


Dates

Issue 2 (2009 February)

Received 2008 March 4, accepted for publication 2008 June 19

Published 2009 February 11



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