We briefly review our work about the polarized foreground contamination of the Cosmic Microwave Background maps. We start by summarizing the main properties of the polarized cosmological signal, resulting in “electric” (E) and “magnetic” (B) components of the polarization tensor field on the sky. Then we describe our present understanding of sub-degree anisotropies from Galactic synchrotron and from extra-Galactic point sources. We discuss their contamination of the cosmological E and B modes.
Polarized foregrounds power spectra vs CMB / Baccigalupi, C.; De Zotti, G.; Burigana, C.; Perrotta, F.. - 609:1(2002), pp. 84-89. (Intervento presentato al convegno ASTROPHYSICAL POLARIZED BACKGROUNDS: Workshop on Astrophysical Polarized Backgrounds tenutosi a Bologna, Italia nel 9-12 Ottobre, 2001) [10.1063/1.1471828].
Polarized foregrounds power spectra vs CMB
Baccigalupi, C.;De Zotti, G.;Perrotta, F.
2002-01-01
Abstract
We briefly review our work about the polarized foreground contamination of the Cosmic Microwave Background maps. We start by summarizing the main properties of the polarized cosmological signal, resulting in “electric” (E) and “magnetic” (B) components of the polarization tensor field on the sky. Then we describe our present understanding of sub-degree anisotropies from Galactic synchrotron and from extra-Galactic point sources. We discuss their contamination of the cosmological E and B modes.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
