FN Archimer Export Format
PT J
TI Dust polarization spectral dependence from Planck HFI data. Turning point for cosmic microwave background polarization-foreground modeling
BT 
AF Ritacco, Alessia
   Boulanger, François
   Guillet, Vincent
   DELOUIS, Jean Marc
   Puget, Jean-Loup
   Aumont, Jonathan
   Vacher, Léo
AS 1:1,2,3;2:2;3:3,4;4:5;5:2,3;6:6;7:6;
FF 1:;2:;3:;4:;5:;6:;7:;
C1 INAF-Osservatorio Astronomico di Cagliari, Via della Scienza 5, 09047 Selargius, ITaly
   Laboratoire de Physique de l’Ecole Normale Superieure, ENS, Universite PSL, CNRS, Sorbonne Universite, Universite de Paris, 75005 Paris, France
   Institut d’Astrophysique Spatiale, CNRS, Université Paris-Saclay, CNRS, Bât. 121, 91405 Orsay, France
   Laboratoire Univers et Particules de Montpellier, Université de Montpellier, CNRS/IN2P3, CC 72, Place Eugéne Bataillon, 34095 Montpellier Cedex 5, France
   Laboratoire d’Océanographie Physique et Spatiale (LOPS), Univ. Brest, CNRS, Ifremer, IRD, Brest, France
   IRAP, Universite de Toulouse, CNRS, CNES, UPS, (Toulouse), France
C2 INAF, ITALY
   ENS, FRANCE
   UNIV PARIS SACLAY, FRANCE
   UNIV MONTPELLIER, FRANCE
   CNRS, FRANCE
   UNIV TOULOUSE, FRANCE
UM LOPS
IN WOS Cotutelle UMR
   copubli-france
   copubli-europe
   copubli-univ-france
IF 6.5
TC 5
UR https://archimer.ifremer.fr/doc/00814/92601/100102.pdf
LA English
DT Article
DE ;cosmic background radiation;cosmology;observations;diffuse radiation;polarization
AB The search for the primordial B-modes of the cosmic microwave background (CMB) relies on the separation from the brighter foreground dust signal. In this context, the characterization of the spectral energy distribution (SED) of thermal dust in polarization has become a critical subject of study. We present a power-spectra analysis of Planck data, which improves upon previous studies by using the newly released SRoll2 maps that include corrections on residual data systematics and by extending the analysis to regions near the Galactic plane. Our analysis focuses on the lowest multipoles between `=4 and 32, as well as three sky areas with sky fractions of fsky = 80%, 90%, and 97%. The mean dust SED for polarization and the 353 GHz Q and U maps are used to compute residual maps at 100, 143, and 217 GHz, highlighting variations of the dust polarization SED on the sky and along the line of sight. Residuals are detected at the three frequencies for the three sky areas. We show that models based on total-intensity data end up underestimating (by a significant factor) the complexity of dust polarized CMB foreground. Our analysis emphasizes the need to include variations of the polarization angles of the dust polarized CMB foreground. The frequency dependence of the EE and BB power spectra of the residual maps yields further insight. We find that the moments expansion to the first order of the modified black-body (MBB) spectrum provides a good fit to the EE power-spectra. This result suggests that the residuals could follow mainly from variations of the dust MBB spectral parameters. However, this conclusion is challenged by cross-spectra showing that the residuals maps at the three frequencies are not fully correlated, as well as the fact that the BB power-spectra do not match the first order moment expansion of a MBB SED. This work sets new requirements for simulations of the dust-polarized foreground and component separation methods, showing that a significant refinement to the dust modeling is necessary to ensure an unbiased detection of the CMB primordial B-modes at the precision required by future CMB experiments. Further works would also be required to theoretically model the impact of polarization-angle variations on the EE and BB power spectra of residual maps. 
PY 2023
PD FEB
SO Astronomy & Astrophysics
SN 0004-6361
PU EDP Sciences
VL 670
IS A163
UT 000936919800001
DI 10.1051/0004-6361/202244269
ID 92601
ER

EF