Planck 2015 results IX. Diffuse component separation: CMB maps
Metadatos
Mostrar el registro completo del ítemAutor
Battaner López, EduardoEditorial
EDP Sciences
Materia
Cosmology: observations Polarization Cosmic background radiation Diffuse radiation
Fecha
2016Referencia bibliográfica
Bartlett, J. G., Bucher, M., Cardoso, J. F., Castex, G., Delabrouille, J., Ganga, K., ... & Racine, B. (2016). Planck 2015 results: IX. Diffuse component separation: CMB maps. Astronomy and Astrophysics, 594, A9-A9. [DOI: 10.1051/0004-6361/201525936]
Patrocinador
Planck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states and led by Principal Investigators from France and Italy, telescope reflectors provided through a collaboration between ESA and a scientific consortium led and funded by Denmark, and additional contributions from NASA (USA).Resumen
We present foreground-reduced cosmic microwave background (CMB) maps derived from the full Planck data set in both temperature and polarization. Compared to the corresponding Planck 2013 temperature sky maps, the total data volume is larger by a factor of 3.2 for frequencies
between 30 and 70 GHz, and by 1.9 for frequencies between 100 and 857 GHz. In addition, systematic errors in the forms of temperature-topolarization leakage, analogue-to-digital conversion uncertainties, and very long time constant errors have been dramatically reduced, to the extent
that the cosmological polarization signal may now be robustly recovered on angular scales ` & 40. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with ` < 20 are accordingly suppressed in the
current polarization maps by high-pass filtering. As in 2013, four different CMB component separation algorithms are applied to these observations, providing a measure of stability with respect to algorithmic and modelling choices. The resulting polarization maps have rms instrumental
noise ranging between 0.21 and 0.27 µK averaged over 550 pixels, and between 4.5 and 6.1 µK averaged over 3.04 pixels. The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the 1σ level with the Planck 2015 likelihood. Unresolved
mismatches between the noise properties of the data and simulations prevent a satisfactory description of the higher-order statistical properties of
the polarization maps. Thus, the primary applications of these polarization maps are those that do not require massive simulations for accurate
estimation of uncertainties, for instance estimation of cross-spectra and cross-correlations, or stacking analyses. However, the amplitude of primordial non-Gaussianity is consistent with zero within 2σ for all local, equilateral, and orthogonal configurations of the bispectrum, including for
polarization E-modes. Moreover, excellent agreement is found regarding the lensing B-mode power spectrum, both internally among the various
component separation codes and with the best-fit Planck 2015 Λ cold dark matter model.