AHR 377 B: metals G8 in strength. AHR 377 C&D: notes for these components are AHR 377 also to be found in Table 1b AHR 377 under HD 7693. Their photo- AHR 377 metry is from Ra only. AHR 380 B: metals and CaII K are A3 in AHR 380 strength; UV continuum strong. AHR 380 Apparent metal weakness from AHR 380 contamination. AHR 436 B: blue region indicates G2. AHR 487 DYN: p 483.66; a 7.81689 (FS). AHR 487 par. 0.106; Ma 0.88; Mb 0.86 AHR 897 B: MgII 4481 weak. AHR 963 DYN: p 314; a 4.367 (BSC4). AHR 963 par. 0.066; Ma 2.11; Mb 0.80 AHR 963 p 154.5; a 2.700 (FS). AHR 963 par. 0.066; Ma 2.13; Mb 0.80 AHR 963 ISO: A is class IV-V since not optical. AHR 1058 A&B: Possibly reddened (A: 0.10; B: AHR 1058 0.05), but not given by 2-color AHR 1058 diagram. AHR 1058 ISO: B double, which can explain B's AHR 1058 color. AHR 1168 ISO: A is HB star, or optical pair if B AHR 1168 confirmed as class V. AHR 1271 B: Metals strength A5, CaII K near A2 AHR 1271 and broad. Apparent metal weakness AHR 1271 from contamination. AHR 1372 B: New Am star. AHR 1504 DYN: p 552.30; a 3.164 (FS). AHR 1504 par. 0.036; Ma 1.13; Mb 1.06 AHR 1506 B: SrII strong (as class II), G band AHR 1506 slightly weak (F3). Morgan and Abt AHR 1506 (1972) note: "CaII H & K greatly AHR 1506 weakened; SrII 4077 strong. This AHR 1506 star has a close spectroscopic AHR 1506 resemblance to some of the delta Scuti AHR 1506 stars..." AHR 2158 A: CaI 4226 slightly strong. AHR 2158 B: washed out lines: see ISO. AHR 2158 C: This is HR 2157. CPM with A & B. AHR 2158 ISO: B probably pre-m.s. and red- AHR 2158 dened [E(B-V) = O.05] AHR 2162 DYN: p 463.5; a 2.94 (FS). AHR 2162 par. 0.039; Ma 1.09; Mb 0.95 AHR 2162 A&B: both have E(B-V) ~ 0.09. AHR 2162 ISO: both may be pre-m.s. AHR 2412 A: Variable H-alpha emission (BSC4). AHR 2412 Rotation ~ 200 km/s. AHR 2412 B: Hydrogen near A8; CaII K is A0 AHR 2412 strength and very broad, AHR 2412 diffuse; Mg 4481 and Fe 4383 AHR 2412 only other metal lines visible. AHR 2412 Apparent metal weakness pro- AHR 2412 bably from contamination since AHR 2412 Delta-V and B-V agree with normal AHR 2412 F0V allowing for fast rotation AHR 2412 of A. Hurly's suggestion AHR 2412 (1976) of reddened B star and AHR 2412 optical not confirmed by AHR 2412 spectrum. AHR 2412 ISO: System not metal weak. AHR 2468 B: metals G4 strength. Photometry AHR 2468 suggests K4V. AHR 2468 ISO: Contamination on B probably AHR 2468 larger than indicated rather AHR 2468 than metal weak. AHR 2482 A: luminosity near V, but SrII and AHR 2482 FeII 4179 are about class II AHR 2482 strength. AHR 2497 B: CaII K is A3n in appearance, AHR 2497 metals A4, G-band weak. AHR 2497 A&B: Sco-Cen association. AHR 2497 ISO: B possibly pre-m.s. AHR 2501 A: emission in H-beta,gamma,delta. AHR 2501 Also H-alpha emission (BSC4). AHR 2501 Rotation (~ 350 km/s) may AHR 2501 account for poor fit to Delta-V, but AHR 2501 see ISO. AHR 2501 B: HeI 3820 slightly weak. AHR 2501 ISO: A seems class III. AHR 2546 B: Image tube spectrum. AHR 2726 B: Contamination gives appearance AHR 2726 of B6Vn, but hydrogen wings, AHR 2726 CaII K and Mg 4481 indicate AHR 2726 B9V. AHR 2736 A&B: Colors not a good match to AHR 2736 classifications. AHR 2736 ISO: B double; implies photometry AHR 2736 probably correct. AHR 2813 B: BSC4 notes sharp central CaII H AHR 2813 & K emission. Not seen at AHR 2813 120 A/mm. AHR 2813 ISO: B is pre-m.s. or double. AHR 3079 B: washed out lines from con- AHR 3079 tamination. Colors suggest AHR 3079 K4V. AHR 3205 AB: "metallic lines strong for AHR 3205 helium type, B8p" (BSC4). AHR 3205 Separate spectra are normal in AHR 3205 appearance. AHR 3223 A: "possibly secondary spectrum" AHR 3223 (BSC4). Not seen at 120 A/mm. AHR 3251 B: spectrum blue of CaII K and AHR 3251 photometry indicate F4V; rest AHR 3251 of spectrum appears as F9V and AHR 3251 is contaminated. AHR 3267 A: a classic composite spectrum: AHR 3267 B7V shown by blue region and AHR 3267 hydrogen lines; G8III shown by AHR 3267 Cr/Fe and Sr/Fe ratios. The B7 AHR 3267 dominates a washed out G8 AHR 3267 spectrum. The composite as AHR 3267 listed would give the observed AHR 3267 photometry of HW. AHR 3327 A: Algol-type eclipsing binary. AHR 3327 BC: secondary is double: sep. 0"1 AHR 3327 in 1956, Delta-m = 0.2 (IDS). AHR 3327 V: not consistent with calculated AHR 3327 Delta-V, (=1.70) when duplicities AHR 3327 are considered. A typographi- AHR 3327 cal error is unlikely since HW AHR 3327 gives Delta-V along with the V AHR 3327 magnitudes. AHR 3327 ISO: Probably A is optical with AHR 3327 respect to BC system. AHR 3358 A: Comparison of Delta-V with classifi- AHR 3358 cations suggests Delta-m = 1.7 mag AHR 3358 for double primary rather than AHR 3358 the 0.0 mag given in the IDS. AHR 3359 A: has interstellar CaII K line. AHR 3373 A: Delta-V fits class IV not V. This AHR 3373 is probably a rotation effect AHR 3373 (Strittmatter 1966) since AHR 3373 spectrum clearly shows class V. AHR 3373 C: underexposed spectrum. AHR 3399 B: Contamination (up to 40%) AHR 3399 beginning redwards of CaI 4226. AHR 3432 A: Photometry suggests KOIII. AHR 3432 B: Slight CN contamination seen. AHR 3432 Photometry suggests G2V. AHR 3439 A: New pec. star. Si, Cr weak but AHR 3439 present. lambda-4077 probably Si AHR 3439 since SrII 4216 absent. CaII AHR 3439 K-line almost absent (~ B8 AHR 3439 strength). Overall line AHR 3439 strength A6. Temperature AHR 3439 type from hydrogen lines. AHR 3439 Their wings and FeII appear as AHR 3439 class V, but Delta-V suggests class AHR 3439 III. AHR 3439 B: washed out lines and hydrogen AHR 3439 strong in UV indicate 50% AHR 3439 contamination. Photometry AHR 3439 suggests F8V. AHR 3455 B: Photometry suggests G5. AHR 3455 ISO: B probably pre-m.s. else AHR 3455 optical. AHR 3489 A&B: Colors indicate B is later than AHR 3489 A. Interchange possible in AHR 3489 observation, but Delta-V shows AHR 3489 agreement with classifications. AHR 3542 B: B-V indicates A8. If so, then AHR 3542 spectrum slightly contaminated. AHR 3542 ISO: B probably pre-m.s. AHR 3574 B: High contamination seen on AHR 3574 spectrum. Photometry indicates AHR 3574 A6V. AHR 3661 AB: primary is double: Delta-m 0.5, AHR 3661 sep 0.11" (BSC4). AHR 3661 HeI 4121 & 4144 slightly strong AHR 3661 for B7. H-delta,H-gamma cores sharp. AHR 3661 Probably composite of B7V and AHR 3661 B8V. AHR 3781 A&B: reddening from classification. AHR 3817 B: Thackeray (1969) reports pecu- AHR 3817 liarities similar to HR 5210 A, AHR 3817 but more diffuse and weaker. AHR 3817 No such peculiarities seen in AHR 3817 the one spectrum taken. Its AHR 3817 B-V is slightly bluer than A's, AHR 3817 and this would fit a spectrum AHR 3817 variable. AHR 3831 A: Spectra from 3 different nights AHR 3831 (JD 2444000 +708.5/ +721.5/ AHR 3831 +982.5) showed variable Sr, Eu AHR 3831 and a line at lambda-4422. Cr is AHR 3831 enhanced. First confirmation AHR 3831 of spectrum variability, though AHR 3831 it has been listed variously as AHR 3831 A5 Sr, Si (Bertaud 1959), FOp AHR 3831 SrEuCr (Jaschek and Jaschek AHR 3831 1959) and A7p Sr (BSC4; notes). AHR 3831 B: slight contamination probable AHR 3831 since slight variability in Sr AHR 3831 (the strongest of the variable AHR 3831 lines in A) seen. Colors AHR 3831 suggest G3V. Then Delta-V would AHR 3831 imply A is class V. AHR 3831 AB: Photometric variable: ampli- AHR 3831 tude 0.05 in V, p 1.428 days. AHR 3890 B: Classification is good despite AHR 3890 apparent contamination. Hurly AHR 3890 (1976) comments correctly that AHR 3890 B is a reddened B-star. AHR 3925 A: Slightly asymmetrical lines AHR 3925 (red wings larger than blue) AHR 3925 indicate spectroscopic binary. AHR 3925 A&B: Reddening different for each AHR 3925 component. AHR 3925 ISO: The pair is probably optical. AHR 4074 A: quite steep cut-off to violet AHR 4074 edges of most lines. Slettebak AHR 4074 (1975) noted similar asymmetry. AHR 4074 Hoffleit (1953) comments that AHR 4074 the two earliest plates in 1893 AHR 4074 and 1895 show emission. AHR 4074 B: a new Silicon star (lambda- AHR 4074 4128-31 and faintly at 4200). AHR 4074 This detection explains the dif- AHR 4074 ferent reddenings found by AHR 4074 Hurly (1976). Reddening AHR 4074 adopted here is from classifi- AHR 4074 cation of A. AHR 4074 ISO: system seems quite young (<0.1 AHR 4074 Gyrs). A is probably lumino- AHR 4074 sity class II. AHR 4118 B: H-beta weak (~ G5 strength), other AHR 4118 lines slightly diffuse, but AHR 4118 ratios are F8. Since no con- AHR 4118 tamination for this very wide AHR 4118 pair (sep 11"), B is genuinely AHR 4118 highly reddened. AHR 4118 ISO: B pre-m.s., so reddening of B AHR 4118 probably circumstellar. AHR 4262 A: H-alpha emission (Kucewicz 1975). AHR 4262 A&B: True Mv's may be about 1 mag AHR 4262 (Strittmatter 1966) higher than AHR 4262 given since both components are AHR 4262 fast rotators (A ~ 300 km/s; B AHR 4262 ~ 350 km/s). AHR 4370 A: Colors suggest F2V. AHR 4370 B: Colors suggest F4V. AHR 4401 A: luminosity could be V from AHR 4401 spectrum. Delta-V indicates A is AHR 4401 half a luminosity class lower AHR 4401 than B. AHR 4401 ISO: B pre-m.s. if A is class V. AHR 4401 Otherwise pair is optical. AHR 4577 ISO: Metal weakness of both com- AHR 4577 ponents confirmed. A may be HB AHR 4577 star. AHR 4615 AB: primary is double. Delta-m 0.0; AHR 4615 sep 0.1" (BSC4). AHR 4615 Spectrum is composite as indi- AHR 4615 cated. If both components were AHR 4615 giants, they would give com- AHR 4615 bined light colors as observed. AHR 4615 C: Line appear weak (~ Fe-2) with AHR 4615 bowl-shaped profiles. AHR 4615 Spectroscopic binary with near AHR 4615 equal components. AHR 4615 AB&C: The observed Delta-V implies that B AHR 4615 is class V rather than III. AHR 4615 The conflict with the color AHR 4615 photometry is unresolved. AHR 4628 B: New proto-Am star. AHR 4636 B: Slightly washed out lines indi- AHR 4636 cate contamination on this AHR 4636 image tube spectrum. AHR 4636 Photometry gives G1V. The U-B AHR 4636 has a large excess (0.15). AHR 4636 ISO: If B is double (with a hot AHR 4636 subdwarf for the U-B excess?), AHR 4636 then binary fits isochrone. AHR 4636 Otherwise A is HB star. AHR 4652 A&B: classification, but not 2-color AHR 4652 diagram, indicates reddenings AHR 4652 of 0.09 and 0.05 respectively. AHR 4718 B: This component is evolved, as AHR 4718 was suggested by Hurly (1976) AHR 4718 from its 2-color position 0.06 AHR 4718 below the m.s. AHR 4730 B: HeI 3820 appears weak. AHR 4730 C: This is HR 4729. It has CPM AHR 4730 with A and B. AHR 4804 A: Shell star (BSC4). No shell AHR 4804 lines seen in this classifica- AHR 4804 tion, but it is a very fast AHR 4804 rotator (~ 350 km/s). Hurly AHR 4804 (1976) notes different red- AHR 4804 dening of primary (0.18) to AHR 4804 secondary (0.10). AHR 4804 B: Spectrum underexposed and pro- AHR 4804 bably contaminated. Photometry AHR 4804 gives A7. AHR 4819 DYN: p 84.50; a 0.930 (FS). AHR 4819 par. 0.018 AHR 4819 A&B: Reddening from the classifica- AHR 4819 tions. Possible member of AHR 4819 Hyades group, discussed by AHR 4819 Rodgers (1967). AHR 4844 DYN: p 383.12; a 1.735 (FS). AHR 4844 par. 0.012 AHR 4844 Mv's suggest parallax near AHR 4844 0.006 AHR 4952 A: Classification based on Hiltner AHR 4952 and Schild criteria (1966). AHR 4952 Absorption lines are slightly AHR 4952 washed out, especially near H-delta, AHR 4952 but HeII/HeI ratios and SiIV AHR 4952 have BOIII appearance, though AHR 4952 this luminosity is underlumi- AHR 4952 nous with respect to the WC AHR 4952 component. Garrison et al. AHR 4952 (1977) have WC5+BOIa, which is AHR 4952 more likely. AHR 4952 B: The classification is good and AHR 4952 from two uncontaminated AHR 4952 spectra, which give no evidence AHR 4952 for duplicity. AHR 4952 AB: Spectrum appears as for A AHR 4952 alone, but all absorption lines AHR 4952 are less washed out. AHR 5122 B: Marginally strong CN probably AHR 5122 indicates contamination since AHR 5122 Delta-V and B-V give F8Va. AHR 5122 ISO: B double, or A is HB star. AHR 5141 A: Rotation ~ 350 km/s. AHR 5189 B: Image tube spectrum. B-V AHR 5189 suggests K6. AHR 5210 A: Spectrum appears normal. AHR 5210 Previously classified at 35-57 AHR 5210 A/mm as B5IV with PII and PIII, AHR 5210 and HeI somewhat weak (Bidelman AHR 5210 1960) and as B5Vp (Slettebak AHR 5210 1963). AHR 5210 B: Spectrum appears normal. AHR 5210 Previously classified as B8V AHR 5210 (Bidelman 1960, de Vaucouleurs AHR 5210 1951) and as B9V (Slettebak AHR 5210 1963). AHR 5234 A: Photometry suggests A1IV, but AHR 5234 may be affected by large rota- AHR 5234 tion ~ 250 km/s. Previously AHR 5234 classified as A0V (Corbally and AHR 5234 Garrison 1980). AHR 5234 B: Photometry suggests A2V. AHR 5234 Previously classified as A1V AHR 5234 (Corbally and Garrison 1980) AHR 5234 ISO: Possibly B is blue straggler. AHR 5242 A: Metals seem very slightly weak AHR 5242 (Fe-0.5), but CN normal. AHR 5242 ISO: A double. This would explain AHR 5242 metal weakening. AHR 5362 B: Slightly strong CN (+1) and AHR 5362 colors indicate contamination. AHR 5362 Photometry gives F4IV-V. AHR 5362 ISO: B double or A is HB star. AHR 5371 ISO: A is possibly HB star. AHR 5375 AB: Primary is double, with separa- AHR 5375 tion 0.2". AHR 5375 C: Classification uncertain due to AHR 5375 contamination. AHR 5428 ISO: A is HB star. AHR 5497 A: Sr and FeII strong. Hydrogen AHR 5497 wings give class V. Both Delta-V and AHR 5497 isochrones agree with this lumi- AHR 5497 nosity. Malaroda (1975) has AHR 5497 F2III-IV. AHR 5497 B: All lines appear slightly AHR 5497 strong. Colors suggest G2V. AHR 5559 A&B: B-V gives B earlier than A. AHR 5559 U-B vice-versa. AHR 5559 ISO: Both components fit if B-V's AHR 5559 are interchanged. Probable AHR 5559 identification error; otherwise AHR 5559 an optical pair. AHR 5683 AB: H-alpha emission (Kucewicz 1967). AHR 5697 A: SiII 4128 and 4200 slightly AHR 5697 variable on two plates. Sr AHR 5697 4077, 4216 and Cr 4172 slightly AHR 5697 enhanced and variable also. AHR 5697 Hydrogen wings indicate class AHR 5697 IV. AHR 5697 B: Seems genuine weak lined star, AHR 5697 and not affected by contamination. AHR 5697 ISO: probably B is pre-m.s., or AHR 5697 possibly A is class V. AHR 5756 A: Spectrum appears composite from AHR 5756 flat, broad profile of hydrogen AHR 5756 and CaII K. AHR 5756 B: Spectrum appears composite from AHR 5756 line weakness (Fe-1) which AHR 5756 increases towards the violet. AHR 5756 Composite could be F7 + G0. AHR 5756 THe binary is too wide (11") AHR 5756 for contamination from A AHR 5756 component. AHR 5781 AB: Shell star (BSC4). Neither A AHR 5781 nor B show shell features in AHR 5781 their spectra. AHR 5781 B: Delta-V and colors give B9V, which AHR 5781 confirms slight contamination AHR 5781 on B's spectrum. AHR 5846 B: Spectrum has faint G band, weak AHR 5846 CaII K and slightly weak metal AHR 5846 lines. Colors agree with AHR 5846 hydrogen strength. Probably AHR 5846 not composite, but new proto-Am AHR 5846 star. AHR 5846 ISO: B has luminosity class IV-V. AHR 5900 A: Hydrogen and metal line pat- AHR 5900 tern, save weak CaII K, is near AHR 5900 F3II. Sr has class Ib AHR 5900 strength. Earlier grating AHR 5900 spectra at 42 A/mm yielded AHR 5900 A3/A7/FOII-III (with lambda-4078 AHR 5900 strong) (Jaschek and Jaschek AHR 5900 1960). AHR 5900 B: HW notes it falls 0.13 below AHR 5900 2-color m.s., but classifica- AHR 5900 tion is good at class V. AHR 5904 B: High errors in colors (+ 0.05) AHR 5904 are probably observational (HW). AHR 5904 A&B: Hurly's (1976) suggested red- AHR 5904 dening (0.10) is the mean of AHR 5904 the spectroscopic reddenings AHR 5904 and is applied to both com- AHR 5904 ponents. It might be higher AHR 5904 since this binary is embedded AHR 5904 in a reflection nebula (Sco AHR 5904 OB2). AHR 5904 ISO: suggest A is IV, but A's posi- AHR 5904 tion above m.s. may simply be AHR 5904 due to its fast rotation. AHR 5925 A&B: Reddening from the classifica- AHR 5925 tions. AHR 5952 AB: Though IDS gives Delta-m = 4.5 for AHR 5952 double primary, Delta-V indicates a AHR 5952 Delta-m of ~ 0.5 only. AHR 6006 AB: composite has weak G band and AHR 6006 strong CN. G1 is a mean between AHR 6006 the slightly stronger H-delta AHR 6006 and the weaker H-gamma. AHR 6029 B: Low level metals have F2 AHR 6029 strength. Classified as F2V by AHR 6029 Garrison (1967). AHR 6029 ISO: B probably pre-m.s. rather than AHR 6029 optical. It is in Sco OB2. AHR 6097 A&B: Reddening from the AHR 6097 classifications. AHR 6097 C: spectrum underexposed on plate. AHR 6106 A: H-gamma slightly stronger than H-delta. AHR 6134 B: Washed out lines show con- AHR 6134 tamination of between 5% in AHR 6134 violet to 25% in green region. AHR 6134 Luminosity not certain due to AHR 6134 this contamination. AHR 6134 AB: No emission lines were seen at AHR 6134 120 A/mm dispersion for this AHR 6134 system which has been likened AHR 6134 to a wide VV Cephei star AHR 6134 (Cowley 1969). AHR 6134 A&B: Despite HW's caution that this AHR 6134 variable system may have photo- AHR 6134 metric errors, their Delta-V and AHR 6134 colors agree quite well with AHR 6134 the classifications. Ra seem AHR 6134 off in U but are within the AHR 6134 variability for the other AHR 6134 photometry. AHR 6134 DYN: p 878; a 2.90 (BSC4). AHR 6134 par. 0.011. AHR 6134 This parallax gives A's Mv = AHR 6134 -3.9, which disagrees with A's AHR 6134 spectral type. The Mv's based AHR 6134 on the classification of B and AHR 6134 Delta-V suggest a parallax of 0.004, AHR 6134 the same as the dynamical AHR 6134 parallax estimated by Russell AHR 6134 and Moore (1940). The orbital AHR 6134 elements in BSC4 are probably AHR 6134 inexact. AHR 6236 B: FeII indicated class V; Sr AHR 6236 indicated IV. Class IV agrees AHR 6236 with Delta-V. AHR 6236 ISO: The B-V's of the components, AHR 6236 when interchanged, fit the AHR 6236 isochrones. Components may AHR 6236 have been confused by HW. AHR 6244 A: Previously classified as B9p Si AHR 6244 (Jaschek and Jaschek 1960), but AHR 6244 no peculiarities seen in our AHR 6244 spectrum. AHR 6244 B: Hydrogen wings are very AHR 6244 slightly asymmetrical with the AHR 6244 violet steeper than the red. AHR 6244 BSC4 notes that the velocity AHR 6244 separation for this SB2 com- AHR 6244 ponent is 258 km/s, and both AHR 6244 are B9V. AHR 6244 A&B: reddening of B adopted since A AHR 6244 is not on m.s. AHR 6402 DYN: p 548.7; a 13.91 (FS) par. AHR 6402 0.182; Ma 0.74; Mb 0.73 AHR 6416 DYN: p 693.4; a 10.415 (FS); but BSC4 AHR 6416 notes that periods range AHR 6416 242