Highest S/N SDSS spectra of a sample of stars for which we identified for Zeeman splittings, indicative of fields from 14 to 1.3 MG. (a) Plate-MJD-Fibre = 1954-53357-393, 13 MG, SDSS J101428.10+365724.40; (b) 0415-51879-378, 11 MG, J033145.69+004517.04; (c) 1616-53169-423, 2.4 MG, 123414.11+124829.58; (d) 2277-53705-484, 2.2 MG, 083945.56+200015.76; (e) 2772-54529-217, 2.2 MG, 141309.30+191832.01; (f) 2694-54199-175, 1.7 MG, 064607.86+280510.14; (g) 2376-53770-534, 2.6 MG, 103532.53+212603.56; (h) 2417-53766-568, 9.9 MG, 031824.20+422651.00; (i) 2585-54097-030, 14 MG, 100759.81+162349.64; (j) 2694-54199-528, 1.3 MG, 065133.34+284423.44; (k) 0810-52672-391, 11 MG, 033145.69+004517.04; (l) 1798-53851-233, 14 MG, 131508.97+093713.87; (m) 2006-53476-332, 19 MG, 125715.54+341439.38; (n) 2644-54210-167, 1.9 MG, 121033.24+221402.64; (o) 2430-53815-229, 2.5 MG, 085106.13+120157.84. DA models, without magnetic field, resulting from least-squares fits to the spectra are plotted in red, obviously inadequate.