A Bayesian method for point source polarisation estimation

The estimation of the polarisation P extragalactic compact sources in cosmic microwave background (CMB) images is a very important task order to clean these for cosmological purposes –for example, constrain tensor-to-scalar ratio primordial fluctuations during inflation– and also obtain relevant astrophysical information about themselves frequency range, ν ∼ 10–200 GHz, where observations have only recently started become available. In this paper, we propose Bayesian maximum posteriori approach scheme which incorporates prior distribution fraction between 1 100 GHz. We apply white noise simulations more realistic that include CMB intensity, Galactic foregrounds, instrumental with characteristics QUIJOTE (Q U I JOint TEnerife) experiment wide survey at 11 Using simulations, compare our method frequentist filtered fusion has been already used Wilkinson Microwave Anisotropy Probe data Planck mission. find allows us decrease threshold feasible levels below ∼100 mJy (as compared ∼500 was equivalent fusion). bias introduced by it be small absolute terms. Finally, test robustness estimator against uncertainties flux density sources. robust moderate changes parameters almost insensitive errors estimated photometry