1 sp.bin. 96.7d (e=0.5). 5 companion @ 13", Am=4.4. 8 sp.bin. of long per. (Vilhu 1978). 12 sp.bin. 106.3d (Renson 1966). 14 sp.bin. 273d (e=0.5) (Preston & Wolff 1970). 18 1 ADS 1507A, companion @ 8" often confused with the Ap star, the 18 2 luminosity being almost the same (Am<0.1), thus gue alf (note the 18 3 components are switched in the GC and BSC catalogues with respect 18 4 to HD), this is why we have indicated gam Ari (S) (=southern 18 5 component) rather than A. 20 ADS 1615A, companion @ 3.6", Am=0.9. 23 1 ADS 1860A, companions @ 2" (Am=2.9) and @ 7" (Am=3.8), + close 23 2 companion @ 0.1", revol. in 52.4 years 24 1 ADS 1849a, companion @ 12", Am=3.1; sp.bin. 2.9978d (Babcock 24 2 1958a,b). 34 1 sp.bin. 2.9753d, ellipsoidal variable (photometric period = P/2) 34 2 (Hube 1981). 35 sp.bin. 5.954d, 2sp. 37 sp.bin. 7.2274d. 39 sp.bin. 4.45d. 43 ADS 3305A, companion @ 1.5", Am=4.8. 44 companion @ 0.2", Am=0.3. 52 ADS 3767A, companion @ 0.1", Am=0.5. 53 ecl. bin. (the period indicated is that of the eclipses). 57 ADS 4116A, companion @ 0.1", Am=0.5. 62 sp.bin. 19d. 74 ADS 4566A, companion @ 3", Am=4.5. 80 ADS 4799A, companion @ 1", Am=2.5. 86 largest known variation for V(0.16mag) amongst Ap stars. 89 companion @ 27.5", Am=3.5 (+ two others more distant). 90 sp.bin. 46.3d, 2 sp. 102 1 sp.bin. 2380d (e=0.6) (Scholz 1978); 8.0248 was erroneously 102 2 printed 8.0228 in Babcock 1960. 103 sp.bin. 9d ? (Abt & Levy 1972). 105 companion @ 2.3", Am=2.7. 106 companion @ 28", Am=3.0. 108 sp.bin. 585.4d (e=0.2). 109 algol bin.(the per. indicated is that of the eclipses). 114 sp.bin. 1400D. 115 1 tight triple star of which the three components have nearly the 115 2 same magnitude. 116 1 two components having almost the same magnitude separated by 0.1" 116 2 (revol. in 59 yrs) + one less luminous component @ 1.8". 117 companion @ 3.3", Am=2.7. 118 1 1.08d was omitted in the printing of the I.B.V.S.1280 118 2 (Renson 1977a): cf. correction @ the end of the I.B.V.S.1300. 120 1 the notation 30 H.UMa refers to the numeration of Hevelius, often 120 2 used for this star, which has unfortunately causes confusion with 120 3 30 UMa = phi UMa (the J. was effectively forgotten by Babcock 120 4 (1958a,b) in his catalogue); sp.bin. 11.579d. 122 sp.bin.?, 2 sp.? 123 sp.bin. 12658d ? 127 companion @ 2", Am=2.6. 129 1 ADS 8115A, less luminous companion (Am=5.4) @ 1" (+ optical 129 2 component @ 1'). 130 companion @ 1", Am=0.7:. 131 ADS 8568A, 17 ComB(+C) is @ 145". 137 1 prototype of this category of variable stars (type alf CVn) and 137 2 also the first with a determined period; ADS 8706A; the other 137 3 component, alf1 CVn, is @ 20" with Am=2.7. 148 1 first star in which Babcock (1947) found a magnetic field 148 2 variation, with change of sign, synchronous with variations of 148 3 line intensities; sp.bin. 1643d (Abt & Snowden 1973, p.158). 149 large variation in v, y and c1 of the system of Stromgren. 153 ADS 9338A; the other component, pi.2 Boo, is @ 5.5" with Am=0.9. 154 ADS 9477A, companion @ 36", Am=2.5. 157 sp.bin. 3834d (e=0.4) (+320d,e=0.7). 164 sp.bin. 35.47d (e=0.5), 2 sp. (Dworetsky 1980). 167 sp.bin. 560d (e=0.5). 169 1 in the article by Borra and Landstreet (1980), it is by error that 169 2 the period of Winzer is designated as being 1.3049 one of the 169 3 two times it is cited p.437. 179 ADS 10310A, companion @ 20", Am=4.8:. 186 sp.bin. 12d ? (Jones & Wolff 1974). 187 1 ADS 11311A, very close companion (distance on the order of 0.2") 187 2 with Am=1.8; sp.bin. (proposed period of 26.77d with e=0.4 187 3 uncertain). 190 1 ADS 11477A, companion @ 10" with Am=5.9 and @ 30" (BD+4 3802) with 190 2 Am=2.7. 198 sp.bin. 35d ? 199 1 the value 2.85 in lieu of 2.88 given for the period in the 199 2 I.B.V.S. 1391 is a printing error. 203 1 very large variation in the luminosity for an Ap star, about the 203 2 same order as for HD215441. 204 sp.bin. 690:d ? (Leeman 1964). 211 sp.bin.? (Abt & Snowden 1973). 217 ADS 14962A, companion @ 20", Am=5.5. 218 MVC 373. 220 ADS 15325A, companion @ 4.5", Am=3. 224 1 ADS 15578A, companion @ 0.8", Am=2.5 (+ other less luminous and @ 224 2 >20"). 228 ADS 16064A, companion @ 1.8", Am=4.5. 230 1 largest known variation of luminosity for an Ap star for the 230 2 total of the visible and the near ultraviolet (0.1 mag in V 230 3 and 0.2 mag in U) and larger variation of effective magnetic field 230 4 He (in the neighborhood of +4 @ +22 kilogauss), but weak variation 230 5 of intensity of the spectral lines for which the anomalies are 230 6 not very marked. 231 1 ADS 16252B, component of a triple system (optical ?) of which the 231 2 brightest (ZZ Cep) is at least at 4" (Am=0.3:) and the other, about 231 3 the same luminosity as the Ap star, @ 17" from it. 232 sp.bin. 16d ? (Floquet 1979). 233 1 ADS 16474A, optical companion @ 20" with Am=3.3 (+ two others 233 2 more distant. 234 sp.bin. 48.3d (e=0.5) (Ouhrabka & Grygar 1979, Huhe 1979). 239 1 sp.bin. 159d (+ long.per.>1 yr?)(Kodaira 1976); large variation of 239 2 y, v and c1 of Stromgren's system (almost like HD 125630, except 239 3 for the period). 242 1 ADS 17020A, companion @ less than 1", Am=0.7 (+ optical companion 242 2 in the neighborhood of 50"). 247 1 the authors cited suspect that the observed variations arise from 247 2 the eclipses. 248 1 optical companion of HD 110956=HR 4848 (@ a little less than 1'); 248 2 record variation in v and in c1 (of syst. of Stromgren): 0.24 and 248 3 0.45 mag resp.