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We study a possibility of constraining isotropic cosmic birefringence withhelp of cosmic microwave background polarisation data in the presence ofpolarisation angle miscalibration without relying on any assumptions about theGalactic foreground angular power spectra and in particular on their EBcorrelation. We propose a new analysis framework based on a generalisedparametric component separation approach, which accounts simultaneously on thepresence of galactic foregrounds, relevant instrumental effects and externalpriors. We find that upcoming multi-frequency CMB data with appropriatecalibration priors will allow producing an instrumental-effect-corrected andforeground-cleaned CMB map, which can be used to estimate the isotropicbirefringence angle and the tensor-to-scalar ratio, accounting on statisticaland systematic uncertainties incurred during the entire procedure. Inparticular, in the case of a Simons Observatory-like, three Small ApertureTelescopes, we derive an uncertainty on the birefringence angle of$\sigma(\beta_{b}) = 0.07^\circ$ (0.1$^\circ$), assuming the standard cosmologyand calibration priors for all (single) frequency channels with the precisionof $\sigma(\alpha_i)= 0.1^\circ$ as aimed at by the near future ground-basedexperiments. This implies that these experiments could confirm or disprove therecently detected value of $\beta_b=0.35^\circ$ with a significance between $3$and $5 \sigma$. [abridged version]

Characterising cosmic birefringence in the presence of galactic foregrounds and instrumental systematic effects