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

By B. Gold, C. Bennett, R. Hill, Gary F. Hinshaw, N. Odegard, L. Page, David N. Spergel, J. Weiland, J. Dunkley, Mark Halpern and 8 more. 2008

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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 χ2ν 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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/685035d26b2d2a9661baa9320387b287b2cf743f

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Citations in the corpus

NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: FINAL MAPS AND RESULTS (2012, methodology): “The method used here is that applied to five-year Q-, V-, and W-band maps by Chen & Wright (2009) and to seven-year Q-, V-, and W-band maps by Gold et al. (2011).”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, result): “We have checked that the cleaned maps give similar results with slightly larger error bars, which is consistent with the excess noise introduced by the template foreground cleaning procedure (Page et al. 2007; Gold et al. 2009, 2010).”
The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements. (2011, methodology): “Gold et al. (2009) used WMAP 5-year data to derive 17 In a related ARCADE2 study, Fixsen et al. (2011) claim a 3−90 GHz extragalactic background about a factor 6 higher than expected from radio sources at 1 GHz.”
The pre-launch Planck Sky Model: a model of sky emission at submillimetre to centimetre wavelengths (2012, methodology): “The Thomson scattered free-free light is expected to be small (a few percent or likely less, Page et al. 2007; Gold et al. 2011; Macellari et al. 2011), with a maximum of about 10% on the edge of bright H ii regions (e.g., Rybicki & Lightman 1979).”
Planck intermediate results. XIX. An overview of the polarized thermal emission from Galactic dust (2014, methodology): “This model, based on a simple description of the spiral magnetic field structure of the Milky Way, was optimized to match the WMAP and Archeops data (e.g., Fauvet et al. 2011, 2012).”
Galactic synchrotron emission with cosmic ray propagation models (2013, methodology): “In addition to these data, total and polarized data at 23, 33, 41, 61 and 94 GHzWMAP seven-year data were obtained from the LAMBDA website 5 (Gold et al. 2011); see the Appendix for the identification and properties of the datasets actually used here.”