A method is presented for reconstructing the intensity profile, I, formed in the magnetic elements which have diameters smaller than the best presently achievable spatial resolution. It follows the same line as in Solanki and Stenflo (1984). As a starting point I and V of the facula and the I observed in the quiet sun are used. The filling factor, and the ratio between the continuum intensity of the magnetic and nonmagnetic parts of the photosphere can be obtained indirectly. For that purpose only the Unno equations, a triplet Zeeman pattern, a longitudinal magnetic field and a two-component model are needed. The method has been applied to some Fourier transform spectrometer data with promising results. As the absolute continuum intensities are unkown, rendering inaccurate the evaluation of the filling factor and the continuum contrast, only the normalized I profile is obtained.