I will discuss the limitations and prospects for the detection of more tenuous high latitude clouds and the reconstruction of the cloud shape, as well as the inferences from the 3D map on the debated distance to the conspicuous Loop I structure. After a brief review of existing maps and their specificity, I will focus on the most recent inversion (Vergely et al, 2022) and show how high- latitude dust clouds compare with the Galactic dust opacity deduced from Planck. Progress is currently being made in this field thanks to the Gaia mission and massive ground-based stellar surveys. Finally, I will present avenues for further investigation through existing and future datasets with focus on the upcoming survey PASIPHAE.ģD maps of dust extinction density in the Milky Way can be constructed by inversion of large catalogues of direction, distance and extinction for individual target stars. I will discuss the potential of combining stellar polarization datasets with polarized dust and synchrotron emission to improve foreground modeling, map 3D magnetic fields, and explore dust microphysics. I will review recent advances in the field that make use of this powerful tracer of the magnetized ISM. With knowledge of stellar distances, stellar polarization can be used to disentangle 3D information about dust and magnetic field properties along the line of sight. Interstellar dust grains impart a polarization on starlight that can be used to trace the magnetic field, similarly to polarized dust emission. Synergies between CMB data and stellar polarimetry These QUIJOTE MFI maps are used to characterise the radio foreground components in the northern sky, with special emphasis on the synchrotron and AME components. I will present the final maps of the survey and their main characteristics (noise levels, calibration uncertainties, power spectra, etc), and I will summarize the list of scientific publications that constitute the MFI wide survey release. In particular, I will discuss the scientific results associated with the wide survey carried out with the first QUIJOTE instrument (MFI) at 11, 13, 17 and 19GHz, covering approximately 29000 deg$^2$ with polarisation sensitivities in the range of 35-40 $\mu$K/deg. Project with the aim of characterising the polarisation of the Cosmic Microwave Background, and other galactic or extragalactic physical processes that emit in microwaves in the frequency range 10-42GHz, and at large angular scales (1 degree resolution). I will review the current status of the QUIJOTE (Q-U-I JOint TEnerife) experiment, a The QUIJOTE MFI wide survey: A northern sky survey in intensity and polarization at 10–20GHz Finally, I will present some of the potential ISM science breakthroughs that can be foreseen with future CMB datasets. I will present our current understanding of the Galactic foregrounds as well as the remaining questions that have to be addressed. In this review talk, I will start by giving an overview of the most important scientific goals of CMB experiments. In turn, these unique millimeter observations provide the ISM science with abundant new data from which rich findings can be drawn. Yet, in order to achieve these thrilling scientific goals, the separation from the foregrounds must be achieved at a precision that require dedicated instrumental and data analysis strategies, as well as additional astrophysical knowledge. Current and next-generation CMB experiments will scrutinize the millimeter sky with exquisite sensitivities, in search for the imprints of primordial gravitational waves generated during inflation, weak gravitational lensing, neutrino mass and hierarchy, light relics or cosmic birefringence. The wealth of cosmological information carried by the cosmic microwave background (CMB) is obscured by the foreground emission from the interstellar medium (ISM) of our Galaxy. CMB and ISM interconnection in millimeter observations
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