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2011MNRAS.418..888M - Mon. Not. R. Astron. Soc., 418, 888-905 (2011/December-1)
Galactic foreground contributions to the 5-year Wilkinson Microwave Anisotropy Probe maps.
MACELLARI N., PIERPAOLI E., DICKINSON C. and VAILLANCOURT J.E.
Abstract (from CDS):
The polarization fraction of the synchrotron emission is constant in frequency and increases with latitude from ≈ 5 per cent near the Galactic plane up to ≈ 40 per cent in some regions at high latitudes; the average value for|b| < 20° is 8.6±1.7 (stat)±0.5 (sys) per cent, while for|b| > 20°, it is 19.3±0.8 (stat)±0.5 (sys) per cent. Anomalous dust and free–free emissions appear to be relatively unpolarized. Monte Carlo simulations showed that there were biases of the method due to cross-talk between the components, at up to ≈ 5 per cent in any given pixel, and ≈ 1.5 per cent on average, when the true polarization fraction is low (a few per cent or less). Nevertheless, the average polarization fraction of dust-correlated emission at the K band is 3.2±0.9 (stat)±1.5 (sys) per cent or less than 5 per cent at 95 per cent confidence. When comparing real data with simulations, eight regions show a detected polarization above the 99th percentile of the distribution from simulations with no input foreground polarization, six of which are detected at above 2σ and display polarization fractions between 2.6 and 7.2 per cent, except for one anomalous region, which has 32±12 per cent. The dust polarization values are consistent with the expectation from spinning dust emission, but polarized dust emission from magnetic-dipole radiation cannot be ruled out. Free–free emission was found to be unpolarized with an upper limit of 3.4 per cent at 95 per cent confidence.
Abstract Copyright: 2011 The Authors Monthly Notices of the Royal Astronomical Society2011 RAS
Journal keyword(s): polarization - ISM: general - Galaxy: general - cosmic background radiation - diffuse radiation - radio continuum: ISM
Simbad objects: 4
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