Issue |
A&A
Volume 373, Number 2, July II 2001
|
|
---|---|---|
Page(s) | L13 - L16 | |
Section | Letters | |
DOI | https://doi.org/10.1051/0004-6361:20010676 | |
Published online | 15 July 2001 |
Error estimation for the MAP experiment
1
Canadian Institute for Theoretical Astrophysics, McLennan Labs, 60 St George Street, Toronto ON M5S 3H8, Canada
2
CEA/DSM/DAPNIA Service d'Astrophysique, Centre d'Études de Saclay, Bât. 709, 91191 Gif-sur-Yvette Cedex, France
3
Department of Physics and Astronomy, Valparaiso University, Valparaiso, IN 46383, USA
4
Institut d'Astrophysique de Paris, CNRS, 94 Bld. Arago, 75014 Paris, France
5
Institut d'Astrophysique Spatiale, CNRS-Université Paris-Sud, Bât. 121, 91405 Orsay, France
Corresponding author: S. Prunet, prunet@cita.utoronto.ca
Received:
2
January
2001
Accepted:
7
May
2001
We report here the first full sky component separation and CMB power
spectrum estimation using a Wiener filtering technique on simulated data from
the upcoming
MAP experiment, set to launch in early
2001. The simulations included contributions from the three dominant astrophysical
components expected in the five MAP spectral bands, namely CMB
radiation, Galactic dust, and synchrotron emission. We assumed a
simple homogeneous and isotropic white noise model and performed our
analysis up to a spherical harmonic multipole on the
fraction of the sky defined by
. We find that the
reconstruction errors are reasonably well fitted by a Gaussian with an
rms of 24 μK, but with significant deviations in the tails. Our
results further support the predictions on the resulting CMB power
spectrum of a previous estimate by Bouchet & Gispert ([CITE]), which entailed a
number of assumptions this work removes.
Key words: methods: data analysis / cosmic microwave background
© ESO, 2001
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