François Levrier

TL;DR: In this article, the authors presented an overview of the polarized sky as seen by Planck HFI at 353 GHz, which is the most sensitive Planck channel for dust polarization.

TL;DR: Within ten nearby (d < 450 pc) Gould Belt molecular clouds, the relative orientation between the magnetic field projected on the plane of sky, inferred from the polarized thermal emission of Galactic dust observed by Planck at 353 GHz, and the gas column density structures, quantified by the gradient of the column density, was evaluated pixel by pixel and analyzed in bins of column density using the novel statistical tool called "Histogram of Relative Orientations".

TL;DR: Aghanim et al. as mentioned in this paper used the same data set to derive a 95% upper bound of 0.020 using the principal component analysis (PCA) model and uniform priors on the PCA mode amplitudes.

TL;DR: In this article, the authors constructed all-sky Compton parameters maps, y-maps, of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 30 to 857 GHz frequency channel maps from the Planck satellite.

TL;DR: In this paper, the authors exploit the Planck HFI polarization data from 100 to 353GHz to measure the dust angular power spectra over the range $40<\ell<600$ well away from the Galactic plane.