The new generation of astronomical instruments are not only in need of the highest sensitivity but require also well-controlled and known instrumental systematic effects. This is particularly relevant for projects dedicated to the study of the Cosmic Microwave background (CMB). Following the success of the Planck mission in providing the most detailed picture of the CMB temperature anisotropy to date, the next generation of CMB projects such as COrE (a potential future mission) and QUBIC (a ground based instrument) will be aiming to study the polarisation anisotropy of the CMB. However, the expected B mode signal from the CMB is several orders of magnitude weaker than the temperature counterpart. Hence the calibration procedures will have to be more stringent than the ones that have been adopted for Planck, to get a proper detection of the primordial B mode signal. For instance, measurements for the receiver and optical systematic effects must be taken into consideration to get a proper reconstruction of the B modepower spectrum. This thesis is focused on the impact of real individual receiver and optical componentson the observation of the primordial B modes. To achieve this, several receiver and quasioptical components have been measured and modelled for their instrumental systematic effects. An analysis pipeline has also been developed, to assess the impact of such instrumental systematic effects on the observation of the primordial B modes. Using the results from the measurements and the analysis pipeline, the instrumental systematic effects that are of concern to the observation of primordial B modes have been identified. This is assuming that no effort has been made to mitigate such instrumental systematic effects.