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The Cosmic Microwave Background anisotropies are difficult to measure atlarge angular scales. In this paper, we present a new analysis of the \Planck\High Frequency Instrument data that brings the cosmological part and its majorforeground signal close to the detector noise. The solar dipole signal, inducedby the motion of the solar system with respect to the CMB, is a very efficienttool to calibrate a detector or a set of detectors with high accuracy. In thiswork, the solar dipole signal is used to extract corrections of the frequencymaps offsets reducing significantly uncertainties. The solar dipole parametersare refined together with the improvement of the high frequency foregrounds,and of the CMB large scales cosmological anisotropies. The stability of thesolar dipole parameters is a powerful way to control the galactic foregroundsremoval in the component separation process. It is used to build a model forSpectral Energy Distribution spatial variations of the interstellar dustemission. The knowledge of these variations will help future CMB analyses inintensity, and also in polarization to measure faint signal related to theoptical reionization depth and the tensor-to-scalar ratio of the primordialanisotropies. The results of this work are: improved solar dipole parameters, anew interstellar dust model, and a large scale cosmological anisotropies map.

Improved large scales interstellar dust foreground model and CMB solar dipole measurement