EDP Sciences
Free access
Volume 373, Number 2, July II 2001
Page(s) L13 - L16
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:20010676

A&A 373, L13-L16 (2001)
DOI: 10.1051/0004-6361:20010676

Error estimation for the MAP experiment

S. Prunet1, R. Teyssier2, S. T. Scully3, F. R. Bouchet4 and R. Gispert5

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

(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 $\ell_{\rm max}=512$ on the fraction of the sky defined by $\vert b\vert > 20^{\circ}$. We find that the reconstruction errors are reasonably well fitted by a Gaussian with an rms of 24 $\mu $K, 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 (1999), which entailed a number of assumptions this work removes.

Key words: methods: data analysis -- cosmic microwave background

Offprint request: S. Prunet, prunet@cita.utoronto.ca

© ESO 2001