tokens: forcing a normalized wavelength of 500 nm everywhere, except when we set a wavelength threshold, in which case we force a normalized Landé factor equal to 1.2. Finally, we correct for any difference in the depth of Stokes profiles, except when the submasks are defined with a line depth threshold. 4.3.2. Outcome for <inline-formula specific-use="simple-math"><italic>β</italic></inline-formula> UMa and <inline-formula specific-use="simple-math"><italic>θ</italic></inline-formula> Leo As a first test, we ran LSD for two submasks containing lines with an average Landé factor lower (resp. greater) than the mean Landé factor of the original line list (see Table B.1 ). Hereafter, we consider the normalizing Landé factors used as part of the LSD procedure, since it is the relevant quantity for direct comparison of different LSD profiles. (The normalizing values follow the same trend as the average Landé factors of the submasks.) The resulting Stokes profiles are plotted in Fig. 2 for the two Am stars and the control Ap star. The Stokes profiles are corrected for a 10% difference in equivalent width observed in their associated Stokes profile. Because of a higher noise level than obtained with the complete line mask, the high- and low- profiles of UMa and Leo do not display any statistically conclusive differences. The overplotted running average helps to improve the situation, showing that the high- signals possess higher amplitudes than their low- counterparts. We note that their amplitude ratio is roughly consistent with the ratio, although this point is difficult to establish with high accuracy (even with the running average) because of the level of noise. Fig. 2 Top : comparison of the Stokes profiles obtained by selecting photospheric lines of low (red thin line) and high (green thin line) magnetic sensitivity for UMa. The thick red and green lines represent a moving average over three spectral bins of the thin lines. Center : same figure for Leo. Bottom : same for CVn. All profiles are normalized to the continuum level. As second test, two sublists were defined from our original list by containing lines with a wavelength lower (resp. greater) than the mean wavelength of the original list (Table B.1 ). For a given star, the Stokes profiles were corrected for the 30% difference in equivalent width observed in their associated Stokes profiles. The outcome of this test is illustrated in Fig. 3 , which illustrates a marginally larger amplitude of the Stokes signal when the wavelength increases. As for the previous test, we computed a moving average of the signal to confirm the trend that is otherwise completely hidden in the noise and to check that the trend observed in both Am stars is consistent with the outcome obtained for 2 CVn. Fig. 3 Same as Fig. 2 for photospheric lines of low (thin blue line) and high (thin red line) wavelength. Fig. 4 Same as Fig. 2 for photospheric lines of low (thin red line) and high (thin green line) central
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