Orateur
Description
In the quest for the faint primordial B-modes of the Cosmic Microwave
Background, three are the key features for any present or future experiment: an utmost sensitivity, excellent control over instrumental systematic effects and over Galactic foreground contamination.
Bolometric Interferometry (BI) is a novel technique that matches them all by combining the sensitivity from bolometric detectors, the control of instrumental systematics from interferometry and a software-based spectral resolution of ∆ν/ν ∼ 0.04, due to the ability to recover the sky signal in several sub-bands within the physical band during data analysis (spectral imaging).
Moreover, the software-based nature of spectral imaging allows to reanalyze the data with different spectral configurations, which can help detecting biases in our results.
In this talk, we present a study to investigate how the increased spectral resolution provided by BI can help controlling foregrounds contamination in the case of unaccounted Galactic dust frequency decorrelations, by focusing on the next generation of ground-based CMB experiments, CMB-S4, and comparing its anticipated sensitivities, frequency and sky coverage with an hypothetical bolometric interferometry version of the same experiment (CMB-S4-BI).
We will show results from a Monte-Carlo analysis based on parametric component separation methods (FGBuster and Commander), highlighting how BI increased spectral resolution provides an unmatched capability to diagnose the presence of foreground contamination in estimates of the tensor-to-scalar ratio $r$.
