In the frequency range used for CMB observations ( Bouchet and Gispert, 1999), the observed data combine contributions from distinct astrophysical components the recovery of which falls in the frame of component separation.įollowing a standard practice in the field of component or source separation, which has physical grounds here, the observed sky is modeled as a linear mixture of statistically independent components. More precisely, recovering useful scientific information requires disentangling in the CMB data the contribution of several astrophysical components, namely, CMB itself galactic emissions from dust and synchrotron and Sunyaev-Zel’dovich (SZ) clusters ( Sunyaev and Zel’dovich, 1980) to name a few. The forthcoming Planck ESA mission will provide new accurate data requiring effective data analysis tools. (2008)) have already provided large amounts of data and astrophysical information. In the past decade several experiments (Archeops, BOOMERANG, MAXIMA, WMAP see Bennett et al. Indeed, most cosmological parameters can be derived from the study of CMB data. Investigating cosmic microwave background (CMB) data is of great scientific importance as it improves our knowledge of the universe ( Jungman et al., 1996). Mohamed Jalal Fadili, in Advances in Imaging and Electron Physics, 2008 B Application to the Planck Data 1 Introduction to the Planck Data Set
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