Here we presant a method for reconstructing the intensity profile, I, formed in tho magnetic elements which have diameters smaller than the best presently achlevable spatial resolutlon. It follows the same line as In Solankl and Stenflo (1984). As a starting point we use I and V (fourth Stokes parameter, whIch originates oniy In magnetic reglons) of the facula and the I observed In the quiet Sun. The filling factor, and the ratio between the continuum intensity of the magnetic and non-magnetic parts of the photosphere can be obtalned Indlrectly. For that purpose onIy the Unno equatlons, 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 (FTS) data (Stenflo et al., 1984) wlth promlsing results. As the absolute continuum intensities are unknown, rendering inaccurate the evaluatlon of the filling factor and the continuum contrast, oniy the normalised I profile Is obtained.