+40 12 May be B7 II. +39 472 May be cA. +39 552 ADS 14314AB. The published delta m (Aitken, A New General Catalogue +39 552 of Double Stars Within 120 deg of the North Pole) is so large that +39 552 the observed spectrum must actually be entirely that of the primary. +39 552 The primary is said to be composite in the Henry Draper Catalogue, +39 552 and for this reason the star is given two HD numbers, HD 198287/8. +39 552 The spectrum does not appear composite on our plates, and was charac- +39 552 terized by Hynek (Perkins Contribution 1, No. 10, 1938) as one simu- +39 552 lating compositeness because of high luminosity. This conclusion is +39 552 almost certainly correct. +38 172 May be B6 Ia. +38 832 May be B7 Ib. +37 352 May be B8 II. +37 722 May be B7 Ir. +36 82 May be B7 II. +36 112 May be cA. +36 862 ADS 14724A. +35 332 ADS 13374A. +35 612 May be B9 II. +35 732 May be cA. +34 122 May be B8 Ib. +32 152 ADS 13335A. +31 12 H-beta in emission. +31 152 The type given here is purely descriptive; among the grounds for +31 152 doubting it is the fact that the spectrum shows no reddening despite +31 152 its low Galactic latitude. On the plate covering its position, an +31 152 absorption feature which may be H-gamma is strong, while all other +31 152 features, including the Balmer discontinuity, are at the limit of +31 152 visiblity. +30 172 May be B7 II. +30 372 HR 8084. +29 22 May be cA. +29 52 P Cyg type. Strong H-alpha emission. +29 62 Similar to AG Peg. +29 222 May be cA. +28 22 May be cA. +24 262 B7 IV(e), Osawa, Ap. J. 130, 159, 1959. +22 22 May be B8 Ib. +22 32 ADS 12287AB. +22 62 BDS 9287A. +21 72 May be cA. +17 32 ADS 11884A. +16 42 Nucleus of planetary nebula No. 220 in Vorontsov-Velyaminov's catalogue +16 42 (Gaseous Nebulae and New Stars, p. 563 ff. Moscow-Leningrad: Soviet +16 42 Academy of Sciences, 1948). +16 92 Perhaps B7 IIle. +15 76 Weak ultraviolet. +13 22 May be cA. +13 96 Abnormal Balmer decrement. +13 102 May be B6 Iab. +11 22 ADS 12000AB. +11 24 Flat continuum. +11 36 K-line possibly present. +11 52 Only one absorption spectrum is clearly identifiable in this overlap, +11 52 and is assumed to belong to Aitken's component A. +11 76 Weak ultraviolet. +11 96 Ultraviolet also considered weak in this star. +11 126 HR 2370, ADS 5153AB. +10 24 Flat continuum. +10 86 Nebulosity surrounds the star. +09 34 May be composite. +09 136 Precedes BD+09 1332 by only a few seconds of arc. +09 146 ADS 5322AB, also S Mon; the slit classification is presumably for +09 146 component A. +09 156 ADS 5327AB. +08 24 May be A0 I-II. +08 36 May be composite. +08 86 Probably not a true Wolf-Rayet, since Hiltner (Ap.J. Suppl. 2, No. 24, +08 86 1956) refers to this star merely as showing high-excitation emission +08 86 superposed on about an O9 spectrum. +08 116 K-line present. +08 126 Nebulosity surrounds the star. +07 24 May be composite. +07 76 K-line and perhaps 4026 present. +06 16 Appears to be composite. +06 26 K-line may be present. +06 24 Very flat continuum. +06 54 Flat continuum. +06 64 G band possibly visible. +05 34 Rather flat continuum. +05 64 May be composite. +05 136 Probably a double star. +05 206 H-epsilon somewhat enhanced. +05 216 K-line may be present; ultraviolet weak; composite? +05 256 May be composite. +04 14 Weak or variable K-line? +04 86 May be composite. +04 166 Helium I lines appear to be visible. +04 356 K-line may be present. +03 66 May be composite. +03 124 May be composite. +02 136 The small angular separation of this binary star assures that the pub- +02 136 lished spectral type of B0 III:p pertains to the combined light of the +02 136 system. +02 146 Possibly composite. +02 166 K-line may be present. +01 54 May be composite. +01 84 May be composite. +01 104 May be composite. +00 16 AGK2 asumes Aitken's position angle for AC is 180 degrees in error and +00 16 calls this star component C; this seems true on a blue plate, but our +00 16 red (H-alpha) plate supports Aitken. +00 34 Flat continuum. +00 54 Classified only from H-alpha plates. +00 104 May be B8 II. +00 214 Flat continuum. -00 54 May be B7 II. -00 76 May be composite. -00 154 K-line visible? -00 204 Composite? -01 16 ADS 4141AB. -01 166 May be B7 III. -01 184 May be composite. -02 16 ADS 4241ABC; a published spectral type of O9.5 V exists. -02 34 K-line may be variable on our plates. -02 64 May be B8 II-III. -02 106 The published spectral type of B0.5 IV (2) must refer to the combined -02 106 light of both components, in view of their small angular separation. -02 144 May be composite. -02 284 May be B8 II-III. -03 94 Roberts 90. -03 136 A spectral type of O9 V has been published for what is presumably -03 136 component A. -03 196 Flat continuum. -04 84 May be composite. -04 144 Roberts 89. -04 246 May be B7 II-III. -04 334 Roberts 91. -05 16 May be double. -05 126 K-line probably present. -05 304 Composite? -06 16 Nebulosity surrounds this star. -06 74 Roberts 88. -06 114 K-line present? -06 294 K-line present? -07 34 Composite? -07 174 Composite? -07 184 May be B7 II-III. -07 244 May be B8 II-III. -07 314 Flat continuum. -08 274 K-line visible? -08 294 K-line visible? -09 76 Ultraviolet continuum weak. -09 104 May be B7 II. -09 114 Lambda 4686 emission? -09 294 K-line visible? -10 114 ADS 11414A; component B may be A- type. -10 154 May be B7 II-III. -10 164 May be B7 II. -10 184 Composite? -10 244 ADS 11670AB. -10 294 Flat continuum. -11 144 Roberts 85. -11 154 Spectral appearance differs considerably between two plates; may be -11 154 less luminous than OB-. -11 204 Of? -11 334 May be B7 II. -12 54 The published spectral type is taken form Hiltner, but does not check -12 54 with the star's appearance on our plates. -12 564 May be composite. -12 594 Classified only from an H-alpha plate. -13 164 Close pair, both OB stars, originally classified as one star. The -13 164 magnitude refers to the combined light. -13 404 Roberts 86. -13 714 May be composite. -14 564 Roberts 87.