Ponente
Descripción
We study the viability of the detection of the primordial polarization B-mode of the cosmic microwave background (CMB) from the ground, but operating on the microwave low-frequency range (e.g., from 10GHz-120GHz). The reason to choose this frequency range is twofold: one the one hand, the instrumental costing is, in principle, lower than at higher frequencies and, on the other hand, it could serve as a complement to future satellite missions like LiteBIRD, which cover frequencies above 40GHz. As it is well-known, the detection of this signal is challenging from the data analysis point of view, due to the relative low amplitude compared to foregrounds, the lensing contamination coming from the leakage of E-modes, and the instrumental noise. Our component separation approach grounds on a full-parametric maximum likelihood method to retrieve the polarized CMB, which also characterise the residual foregrounds at the angular power spectrum level. The sky simulations include galactic emission from synchrotron, dust (which are the main foreground contaminants to the polarized CMB) as well as the anomalous microwave emission (AME). We explore different configurations of the distribution of the frequency channels, in order to find an optimal instrumental design, and taking into account the limitations imposed by the atmosphere. We show that this kind of experiments are feasible and able to provide a clear detection of primordial B-modes corresponding to a tensor-to-scalar ratio parameter of r~0.002, when a delensing of around 50% is assumed.