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## (from tabmap V6.0 (2016-08-18)) 2024-04-29T11:23:24 #--------------------------------------------------------------------------- #-- III/117 MK Classifications of Close Visual Binaries (Corbally, 1984) #-------------------------------------------------------------------------- #---Table: III/117/./notes.dat Notes to tables (691 records) #------------------------------------------------------------------------------- # Label Format Unit Explanations #------------------------------------------------------------------------------- # Tno A1 --- [AB] "A" when notes to Table 1A (HW binaries) # "B" when notes to Table 1B (remainder) # Name A9 --- Name of the binary; repeated for continuation # lines # Comp A4 --- Component or type of the note # --- A1 --- [:] # Text A43 --- Text of the note (1) #------------------------------------------------------------------------------- #Note (1): the following keys are used for abbreviations: # p = period in years # a = semi-major axis in arcseconds # par. = parallax # Ma = mass of A component in solar mass units # Mb = mass of B component in solar mass units # m.s. = main sequence # HB = horizontal branch star # BSC4 = Bright Star Catalogue, 4th edition (Hoffleit and Jaschek, Cat. V/50) # IDS = Index Catalogue of Double Stars (Jeffers et al. 1963; see Cat. I/107) # FS = Finsen and Worley 1970 # ISO = results from isochrone investigation (Corbally 1983, PhD) #------------------------------------------------------------------------------- ------------------------------------------------------------ T| | n| | o|Name |Comp Text -|---------|------------------------------------------------ A|HR 377 | B:metals G8 in strength. A|HR 377 | C&D:notes for these components are A|HR 377 | also to be found in Table 1b A|HR 377 | under HD 7693. Their photo- A|HR 377 | metry is from Ra only. A|HR 380 | B:metals and CaII K are A3 in A|HR 380 | strength; UV continuum strong. A|HR 380 | Apparent metal weakness from A|HR 380 | contamination. A|HR 436 | B:blue region indicates G2. A|HR 487 | DYN:p 483.66; a 7.81689 (FS). A|HR 487 | par. 0.106; Ma 0.88; Mb 0.86 A|HR 897 | B:MgII 4481 weak. A|HR 963 | DYN:p 314; a 4.367 (BSC4). A|HR 963 | par. 0.066; Ma 2.11; Mb 0.80 A|HR 963 | p 154.5; a 2.700 (FS). A|HR 963 | par. 0.066; Ma 2.13; Mb 0.80 A|HR 963 | ISO:A is class IV-V since not optical. A|HR 1058 | A&B:Possibly reddened (A: 0.10; B: A|HR 1058 | 0.05), but not given by 2-color A|HR 1058 | diagram. A|HR 1058 | ISO:B double, which can explain B's A|HR 1058 | color. A|HR 1168 | ISO:A is HB star, or optical pair if B A|HR 1168 | confirmed as class V. A|HR 1271 | B:Metals strength A5, CaII K near A2 A|HR 1271 | and broad. Apparent metal weakness A|HR 1271 | from contamination. A|HR 1372 | B:New Am star. A|HR 1504 | DYN:p 552.30; a 3.164 (FS). A|HR 1504 | par. 0.036; Ma 1.13; Mb 1.06 A|HR 1506 | B:SrII strong (as class II), G band A|HR 1506 | slightly weak (F3). Morgan and Abt A|HR 1506 | (1972) note: "CaII H & K greatly A|HR 1506 | weakened; SrII 4077 strong. This A|HR 1506 | star has a close spectroscopic A|HR 1506 | resemblance to some of the delta Scuti A|HR 1506 | stars..." A|HR 2158 | A:CaI 4226 slightly strong. A|HR 2158 | B:washed out lines: see ISO. A|HR 2158 | C:This is HR 2157. CPM with A & B. A|HR 2158 | ISO:B probably pre-m.s. and red- A|HR 2158 | dened [E(B-V) = O.05] A|HR 2162 | DYN:p 463.5; a 2.94 (FS). A|HR 2162 | par. 0.039; Ma 1.09; Mb 0.95 A|HR 2162 | A&B:both have E(B-V) ~ 0.09. A|HR 2162 | ISO:both may be pre-m.s. A|HR 2412 | A:Variable H-alpha emission (BSC4). A|HR 2412 | Rotation ~ 200 km/s. A|HR 2412 | B:Hydrogen near A8; CaII K is A0 A|HR 2412 | strength and very broad, A|HR 2412 | diffuse; Mg 4481 and Fe 4383 A|HR 2412 | only other metal lines visible. A|HR 2412 | Apparent metal weakness pro- A|HR 2412 | bably from contamination since A|HR 2412 | Delta-V and B-V agree with normal A|HR 2412 | F0V allowing for fast rotation A|HR 2412 | of A. Hurly's suggestion A|HR 2412 | (1976) of reddened B star and A|HR 2412 | optical not confirmed by A|HR 2412 | spectrum. A|HR 2412 | ISO:System not metal weak. A|HR 2468 | B:metals G4 strength. Photometry A|HR 2468 | suggests K4V. A|HR 2468 | ISO:Contamination on B probably A|HR 2468 | larger than indicated rather A|HR 2468 | than metal weak. A|HR 2482 | A:luminosity near V, but SrII and A|HR 2482 | FeII 4179 are about class II A|HR 2482 | strength. A|HR 2497 | B:CaII K is A3n in appearance, A|HR 2497 | metals A4, G-band weak. A|HR 2497 | A&B:Sco-Cen association. A|HR 2497 | ISO:B possibly pre-m.s. A|HR 2501 | A:emission in H-beta,gamma,delta. A|HR 2501 | Also H-alpha emission (BSC4). A|HR 2501 | Rotation (~ 350 km/s) may A|HR 2501 | account for poor fit to Delta-V, but A|HR 2501 | see ISO. A|HR 2501 | B:HeI 3820 slightly weak. A|HR 2501 | ISO:A seems class III. A|HR 2546 | B:Image tube spectrum. A|HR 2726 | B:Contamination gives appearance A|HR 2726 | of B6Vn, but hydrogen wings, A|HR 2726 | CaII K and Mg 4481 indicate A|HR 2726 | B9V. A|HR 2736 | A&B:Colors not a good match to A|HR 2736 | classifications. A|HR 2736 | ISO:B double; implies photometry A|HR 2736 | probably correct. A|HR 2813 | B:BSC4 notes sharp central CaII H A|HR 2813 | & K emission. Not seen at A|HR 2813 | 120 A/mm. A|HR 2813 | ISO:B is pre-m.s. or double. A|HR 3079 | B:washed out lines from con- A|HR 3079 | tamination. Colors suggest A|HR 3079 | K4V. A|HR 3205 | AB:"metallic lines strong for A|HR 3205 | helium type, B8p" (BSC4). A|HR 3205 | Separate spectra are normal in A|HR 3205 | appearance. A|HR 3223 | A:"possibly secondary spectrum" A|HR 3223 | (BSC4). Not seen at 120 A/mm. A|HR 3251 | B:spectrum blue of CaII K and A|HR 3251 | photometry indicate F4V; rest A|HR 3251 | of spectrum appears as F9V and A|HR 3251 | is contaminated. A|HR 3267 | A:a classic composite spectrum: A|HR 3267 | B7V shown by blue region and A|HR 3267 | hydrogen lines; G8III shown by A|HR 3267 | Cr/Fe and Sr/Fe ratios. The B7 A|HR 3267 | dominates a washed out G8 A|HR 3267 | spectrum. The composite as A|HR 3267 | listed would give the observed A|HR 3267 | photometry of HW. A|HR 3327 | A:Algol-type eclipsing binary. A|HR 3327 | BC:secondary is double: sep. 0"1 A|HR 3327 | in 1956, Delta-m = 0.2 (IDS). A|HR 3327 | V:not consistent with calculated A|HR 3327 | Delta-V, (=1.70) when duplicities A|HR 3327 | are considered. A typographi- A|HR 3327 | cal error is unlikely since HW A|HR 3327 | gives Delta-V along with the V A|HR 3327 | magnitudes. A|HR 3327 | ISO:Probably A is optical with A|HR 3327 | respect to BC system. A|HR 3358 | A:Comparison of Delta-V with classifi- A|HR 3358 | cations suggests Delta-m = 1.7 mag A|HR 3358 | for double primary rather than A|HR 3358 | the 0.0 mag given in the IDS. A|HR 3359 | A:has interstellar CaII K line. A|HR 3373 | A:Delta-V fits class IV not V. This A|HR 3373 | is probably a rotation effect A|HR 3373 | (Strittmatter 1966) since A|HR 3373 | spectrum clearly shows class V. A|HR 3373 | C:underexposed spectrum. A|HR 3399 | B:Contamination (up to 40%) A|HR 3399 | beginning redwards of CaI 4226. A|HR 3432 | A:Photometry suggests KOIII. A|HR 3432 | B:Slight CN contamination seen. A|HR 3432 | Photometry suggests G2V. A|HR 3439 | A:New pec. star. Si, Cr weak but A|HR 3439 | present. lambda-4077 probably Si A|HR 3439 | since SrII 4216 absent. CaII A|HR 3439 | K-line almost absent (~ B8 A|HR 3439 | strength). Overall line A|HR 3439 | strength A6. Temperature A|HR 3439 | type from hydrogen lines. A|HR 3439 | Their wings and FeII appear as A|HR 3439 | class V, but Delta-V suggests class A|HR 3439 | III. A|HR 3439 | B:washed out lines and hydrogen A|HR 3439 | strong in UV indicate 50% A|HR 3439 | contamination. Photometry A|HR 3439 | suggests F8V. A|HR 3455 | B:Photometry suggests G5. A|HR 3455 | ISO:B probably pre-m.s. else A|HR 3455 | optical. A|HR 3489 | A&B:Colors indicate B is later than A|HR 3489 | A. Interchange possible in A|HR 3489 | observation, but Delta-V shows A|HR 3489 | agreement with classifications. A|HR 3542 | B:B-V indicates A8. If so, then A|HR 3542 | spectrum slightly contaminated. A|HR 3542 | ISO:B probably pre-m.s. A|HR 3574 | B:High contamination seen on A|HR 3574 | spectrum. Photometry indicates A|HR 3574 | A6V. A|HR 3661 | AB:primary is double: Delta-m 0.5, A|HR 3661 | sep 0.11" (BSC4). A|HR 3661 | HeI 4121 & 4144 slightly strong A|HR 3661 | for B7. H-delta,H-gamma cores sharp. A|HR 3661 | Probably composite of B7V and A|HR 3661 | B8V. A|HR 3781 | A&B:reddening from classification. A|HR 3817 | B:Thackeray (1969) reports pecu- A|HR 3817 | liarities similar to HR 5210 A, A|HR 3817 | but more diffuse and weaker. A|HR 3817 | No such peculiarities seen in A|HR 3817 | the one spectrum taken. Its A|HR 3817 | B-V is slightly bluer than A's, A|HR 3817 | and this would fit a spectrum A|HR 3817 | variable. A|HR 3831 | A:Spectra from 3 different nights A|HR 3831 | (JD 2444000 +708.5/ +721.5/ A|HR 3831 | +982.5) showed variable Sr, Eu A|HR 3831 | and a line at lambda-4422. Cr is A|HR 3831 | enhanced. First confirmation A|HR 3831 | of spectrum variability, though A|HR 3831 | it has been listed variously as A|HR 3831 | A5 Sr, Si (Bertaud 1959), FOp A|HR 3831 | SrEuCr (Jaschek and Jaschek A|HR 3831 | 1959) and A7p Sr (BSC4; notes). A|HR 3831 | B:slight contamination probable A|HR 3831 | since slight variability in Sr A|HR 3831 | (the strongest of the variable A|HR 3831 | lines in A) seen. Colors A|HR 3831 | suggest G3V. Then Delta-V would A|HR 3831 | imply A is class V. A|HR 3831 | AB:Photometric variable: ampli- A|HR 3831 | tude 0.05 in V, p 1.428 days. A|HR 3890 | B:Classification is good despite A|HR 3890 | apparent contamination. Hurly A|HR 3890 | (1976) comments correctly that A|HR 3890 | B is a reddened B-star. A|HR 3925 | A:Slightly asymmetrical lines A|HR 3925 | (red wings larger than blue) A|HR 3925 | indicate spectroscopic binary. A|HR 3925 | A&B:Reddening different for each A|HR 3925 | component. A|HR 3925 | ISO:The pair is probably optical. A|HR 4074 | A:quite steep cut-off to violet A|HR 4074 | edges of most lines. Slettebak A|HR 4074 | (1975) noted similar asymmetry. A|HR 4074 | Hoffleit (1953) comments that A|HR 4074 | the two earliest plates in 1893 A|HR 4074 | and 1895 show emission. A|HR 4074 | B:a new Silicon star (lambda- A|HR 4074 | 4128-31 and faintly at 4200). A|HR 4074 | This detection explains the dif- A|HR 4074 | ferent reddenings found by A|HR 4074 | Hurly (1976). Reddening A|HR 4074 | adopted here is from classifi- A|HR 4074 | cation of A. A|HR 4074 | ISO:system seems quite young (<0.1 A|HR 4074 | Gyrs). A is probably lumino- A|HR 4074 | sity class II. A|HR 4118 | B:H-beta weak (~ G5 strength), other A|HR 4118 | lines slightly diffuse, but A|HR 4118 | ratios are F8. Since no con- A|HR 4118 | tamination for this very wide A|HR 4118 | pair (sep 11"), B is genuinely A|HR 4118 | highly reddened. A|HR 4118 | ISO:B pre-m.s., so reddening of B A|HR 4118 | probably circumstellar. A|HR 4262 | A:H-alpha emission (Kucewicz 1975). A|HR 4262 | A&B:True Mv's may be about 1 mag A|HR 4262 | (Strittmatter 1966) higher than A|HR 4262 | given since both components are A|HR 4262 | fast rotators (A ~ 300 km/s; B A|HR 4262 | ~ 350 km/s). A|HR 4370 | A:Colors suggest F2V. A|HR 4370 | B:Colors suggest F4V. A|HR 4401 | A:luminosity could be V from A|HR 4401 | spectrum. Delta-V indicates A is A|HR 4401 | half a luminosity class lower A|HR 4401 | than B. A|HR 4401 | ISO:B pre-m.s. if A is class V. A|HR 4401 | Otherwise pair is optical. A|HR 4577 | ISO:Metal weakness of both com- A|HR 4577 | ponents confirmed. A may be HB A|HR 4577 | star. A|HR 4615 | AB:primary is double. Delta-m 0.0; A|HR 4615 | sep 0.1" (BSC4). A|HR 4615 | Spectrum is composite as indi- A|HR 4615 | cated. If both components were A|HR 4615 | giants, they would give com- A|HR 4615 | bined light colors as observed. A|HR 4615 | C:Line appear weak (~ Fe-2) with A|HR 4615 | bowl-shaped profiles. A|HR 4615 | Spectroscopic binary with near A|HR 4615 | equal components. A|HR 4615 |AB&C:The observed Delta-V implies that B A|HR 4615 | is class V rather than III. A|HR 4615 | The conflict with the color A|HR 4615 | photometry is unresolved. A|HR 4628 | B:New proto-Am star. A|HR 4636 | B:Slightly washed out lines indi- A|HR 4636 | cate contamination on this A|HR 4636 | image tube spectrum. A|HR 4636 | Photometry gives G1V. The U-B A|HR 4636 | has a large excess (0.15). A|HR 4636 | ISO:If B is double (with a hot A|HR 4636 | subdwarf for the U-B excess?), A|HR 4636 | then binary fits isochrone. A|HR 4636 | Otherwise A is HB star. A|HR 4652 | A&B:classification, but not 2-color A|HR 4652 | diagram, indicates reddenings A|HR 4652 | of 0.09 and 0.05 respectively. A|HR 4718 | B:This component is evolved, as A|HR 4718 | was suggested by Hurly (1976) A|HR 4718 | from its 2-color position 0.06 A|HR 4718 | below the m.s. A|HR 4730 | B:HeI 3820 appears weak. A|HR 4730 | C:This is HR 4729. It has CPM A|HR 4730 | with A and B. A|HR 4804 | A:Shell star (BSC4). No shell A|HR 4804 | lines seen in this classifica- A|HR 4804 | tion, but it is a very fast A|HR 4804 | rotator (~ 350 km/s). Hurly A|HR 4804 | (1976) notes different red- A|HR 4804 | dening of primary (0.18) to A|HR 4804 | secondary (0.10). A|HR 4804 | B:Spectrum underexposed and pro- A|HR 4804 | bably contaminated. Photometry A|HR 4804 | gives A7. A|HR 4819 | DYN:p 84.50; a 0.930 (FS). A|HR 4819 | par. 0.018 A|HR 4819 | A&B:Reddening from the classifica- A|HR 4819 | tions. Possible member of A|HR 4819 | Hyades group, discussed by A|HR 4819 | Rodgers (1967). A|HR 4844 | DYN:p 383.12; a 1.735 (FS). A|HR 4844 | par. 0.012 A|HR 4844 | Mv's suggest parallax near A|HR 4844 | 0.006 A|HR 4952 | A:Classification based on Hiltner A|HR 4952 | and Schild criteria (1966). A|HR 4952 | Absorption lines are slightly A|HR 4952 | washed out, especially near H-delta, A|HR 4952 | but HeII/HeI ratios and SiIV A|HR 4952 | have BOIII appearance, though A|HR 4952 | this luminosity is underlumi- A|HR 4952 | nous with respect to the WC A|HR 4952 | component. Garrison et al. A|HR 4952 | (1977) have WC5+BOIa, which is A|HR 4952 | more likely. A|HR 4952 | B:The classification is good and A|HR 4952 | from two uncontaminated A|HR 4952 | spectra, which give no evidence A|HR 4952 | for duplicity. A|HR 4952 | AB:Spectrum appears as for A A|HR 4952 | alone, but all absorption lines A|HR 4952 | are less washed out. A|HR 5122 | B:Marginally strong CN probably A|HR 5122 | indicates contamination since A|HR 5122 | Delta-V and B-V give F8Va. A|HR 5122 | ISO:B double, or A is HB star. A|HR 5141 | A:Rotation ~ 350 km/s. A|HR 5189 | B:Image tube spectrum. B-V A|HR 5189 | suggests K6. A|HR 5210 | A:Spectrum appears normal. A|HR 5210 | Previously classified at 35-57 A|HR 5210 | A/mm as B5IV with PII and PIII, A|HR 5210 | and HeI somewhat weak (Bidelman A|HR 5210 | 1960) and as B5Vp (Slettebak A|HR 5210 | 1963). A|HR 5210 | B:Spectrum appears normal. A|HR 5210 | Previously classified as B8V A|HR 5210 | (Bidelman 1960, de Vaucouleurs A|HR 5210 | 1951) and as B9V (Slettebak A|HR 5210 | 1963). A|HR 5234 | A:Photometry suggests A1IV, but A|HR 5234 | may be affected by large rota- A|HR 5234 | tion ~ 250 km/s. Previously A|HR 5234 | classified as A0V (Corbally and A|HR 5234 | Garrison 1980). A|HR 5234 | B:Photometry suggests A2V. A|HR 5234 | Previously classified as A1V A|HR 5234 | (Corbally and Garrison 1980) A|HR 5234 | ISO:Possibly B is blue straggler. A|HR 5242 | A:Metals seem very slightly weak A|HR 5242 | (Fe-0.5), but CN normal. A|HR 5242 | ISO:A double. This would explain A|HR 5242 | metal weakening. A|HR 5362 | B:Slightly strong CN (+1) and A|HR 5362 | colors indicate contamination. A|HR 5362 | Photometry gives F4IV-V. A|HR 5362 | ISO:B double or A is HB star. A|HR 5371 | ISO:A is possibly HB star. A|HR 5375 | AB:Primary is double, with separa- A|HR 5375 | tion 0.2". A|HR 5375 | C:Classification uncertain due to A|HR 5375 | contamination. A|HR 5428 | ISO:A is HB star. A|HR 5497 | A:Sr and FeII strong. Hydrogen A|HR 5497 | wings give class V. Both Delta-V and A|HR 5497 | isochrones agree with this lumi- A|HR 5497 | nosity. Malaroda (1975) has A|HR 5497 | F2III-IV. A|HR 5497 | B:All lines appear slightly A|HR 5497 | strong. Colors suggest G2V. A|HR 5559 | A&B:B-V gives B earlier than A. A|HR 5559 | U-B vice-versa. A|HR 5559 | ISO:Both components fit if B-V's A|HR 5559 | are interchanged. Probable A|HR 5559 | identification error; otherwise A|HR 5559 | an optical pair. A|HR 5683 | AB:H-alpha emission (Kucewicz 1967). A|HR 5697 | A:SiII 4128 and 4200 slightly A|HR 5697 | variable on two plates. Sr A|HR 5697 | 4077, 4216 and Cr 4172 slightly A|HR 5697 | enhanced and variable also. A|HR 5697 | Hydrogen wings indicate class A|HR 5697 | IV. A|HR 5697 | B:Seems genuine weak lined star, A|HR 5697 | and not affected by contamination. A|HR 5697 | ISO:probably B is pre-m.s., or A|HR 5697 | possibly A is class V. A|HR 5756 | A:Spectrum appears composite from A|HR 5756 | flat, broad profile of hydrogen A|HR 5756 | and CaII K. A|HR 5756 | B:Spectrum appears composite from A|HR 5756 | line weakness (Fe-1) which A|HR 5756 | increases towards the violet. A|HR 5756 | Composite could be F7 + G0. A|HR 5756 | THe binary is too wide (11") A|HR 5756 | for contamination from A A|HR 5756 | component. A|HR 5781 | AB:Shell star (BSC4). Neither A A|HR 5781 | nor B show shell features in A|HR 5781 | their spectra. A|HR 5781 | B:Delta-V and colors give B9V, which A|HR 5781 | confirms slight contamination A|HR 5781 | on B's spectrum. A|HR 5846 | B:Spectrum has faint G band, weak A|HR 5846 | CaII K and slightly weak metal A|HR 5846 | lines. Colors agree with A|HR 5846 | hydrogen strength. Probably A|HR 5846 | not composite, but new proto-Am A|HR 5846 | star. A|HR 5846 | ISO:B has luminosity class IV-V. A|HR 5900 | A:Hydrogen and metal line pat- A|HR 5900 | tern, save weak CaII K, is near A|HR 5900 | F3II. Sr has class Ib A|HR 5900 | strength. Earlier grating A|HR 5900 | spectra at 42 A/mm yielded A|HR 5900 | A3/A7/FOII-III (with lambda-4078 A|HR 5900 | strong) (Jaschek and Jaschek A|HR 5900 | 1960). A|HR 5900 | B:HW notes it falls 0.13 below A|HR 5900 | 2-color m.s., but classifica- A|HR 5900 | tion is good at class V. A|HR 5904 | B:High errors in colors (+ 0.05) A|HR 5904 | are probably observational (HW). A|HR 5904 | A&B:Hurly's (1976) suggested red- A|HR 5904 | dening (0.10) is the mean of A|HR 5904 | the spectroscopic reddenings A|HR 5904 | and is applied to both com- A|HR 5904 | ponents. It might be higher A|HR 5904 | since this binary is embedded A|HR 5904 | in a reflection nebula (Sco A|HR 5904 | OB2). A|HR 5904 | ISO:suggest A is IV, but A's posi- A|HR 5904 | tion above m.s. may simply be A|HR 5904 | due to its fast rotation. A|HR 5925 | A&B:Reddening from the classifica- A|HR 5925 | tions. A|HR 5952 | AB:Though IDS gives Delta-m = 4.5 for A|HR 5952 | double primary, Delta-V indicates a A|HR 5952 | Delta-m of ~ 0.5 only. A|HR 6006 | AB:composite has weak G band and A|HR 6006 | strong CN. G1 is a mean between A|HR 6006 | the slightly stronger H-delta A|HR 6006 | and the weaker H-gamma. A|HR 6029 | B:Low level metals have F2 A|HR 6029 | strength. Classified as F2V by A|HR 6029 | Garrison (1967). A|HR 6029 | ISO:B probably pre-m.s. rather than A|HR 6029 | optical. It is in Sco OB2. A|HR 6097 | A&B:Reddening from the A|HR 6097 | classifications. A|HR 6097 | C:spectrum underexposed on plate. A|HR 6106 | A:H-gamma slightly stronger than H-delta. A|HR 6134 | B:Washed out lines show con- A|HR 6134 | tamination of between 5% in A|HR 6134 | violet to 25% in green region. A|HR 6134 | Luminosity not certain due to A|HR 6134 | this contamination. A|HR 6134 | AB:No emission lines were seen at A|HR 6134 | 120 A/mm dispersion for this A|HR 6134 | system which has been likened A|HR 6134 | to a wide VV Cephei star A|HR 6134 | (Cowley 1969). A|HR 6134 | A&B:Despite HW's caution that this A|HR 6134 | variable system may have photo- A|HR 6134 | metric errors, their Delta-V and A|HR 6134 | colors agree quite well with A|HR 6134 | the classifications. Ra seem A|HR 6134 | off in U but are within the A|HR 6134 | variability for the other A|HR 6134 | photometry. A|HR 6134 | DYN:p 878; a 2.90 (BSC4). A|HR 6134 | par. 0.011. A|HR 6134 | This parallax gives A's Mv = A|HR 6134 | -3.9, which disagrees with A's A|HR 6134 | spectral type. The Mv's based A|HR 6134 | on the classification of B and A|HR 6134 | Delta-V suggest a parallax of 0.004, A|HR 6134 | the same as the dynamical A|HR 6134 | parallax estimated by Russell A|HR 6134 | and Moore (1940). The orbital A|HR 6134 | elements in BSC4 are probably A|HR 6134 | inexact. A|HR 6236 | B:FeII indicated class V; Sr A|HR 6236 | indicated IV. Class IV agrees A|HR 6236 | with Delta-V. A|HR 6236 | ISO:The B-V's of the components, A|HR 6236 | when interchanged, fit the A|HR 6236 | isochrones. Components may A|HR 6236 | have been confused by HW. A|HR 6244 | A:Previously classified as B9p Si A|HR 6244 | (Jaschek and Jaschek 1960), but A|HR 6244 | no peculiarities seen in our A|HR 6244 | spectrum. A|HR 6244 | B:Hydrogen wings are very A|HR 6244 | slightly asymmetrical with the A|HR 6244 | violet steeper than the red. A|HR 6244 | BSC4 notes that the velocity A|HR 6244 | separation for this SB2 com- A|HR 6244 | ponent is 258 km/s, and both A|HR 6244 | are B9V. A|HR 6244 | A&B:reddening of B adopted since A A|HR 6244 | is not on m.s. A|HR 6402 | DYN:p 548.7; a 13.91 (FS) par. A|HR 6402 | 0.182; Ma 0.74; Mb 0.73 A|HR 6416 | DYN:p 693.4; a 10.415 (FS); but BSC4 A|HR 6416 | notes that periods range A|HR 6416 | 242<p<2205. par. 0.122; A|HR 6416 | Ma 0.84; Mb 0.47 A|HR 6416 | B:CaI and CaII very weak (Ca-3), A|HR 6416 | and Cr triplet weak (Cr-1). A|HR 6416 | Otherwise spectrum and colors A|HR 6416 | give MOV. A|HR 6416 | ISO:binary fits solar abundance A|HR 6416 | isochrones. A|HR 6426 | DYN:p 42.177; a 1.734 (BSC4). A|HR 6426 | par. 0.136; Ma 0.65; Mb 0.51 A|HR 6426 | B:colors suggest K5+V A|HR 6426 | C:photometry is from Eggen A|HR 6426 | (1974). This image tube A|HR 6426 | spectrum might be M1.5. A|HR 6622 | A:Companion of this eclipsing A|HR 6622 | binary estimated from doubled A|HR 6622 | lines seen at lambda-4026, 4144 and A|HR 6622 | 4388, and from the asymmetrical A|HR 6622 | hydrogen lines. A|HR 6622 | ISO:Optical pair, even allowing for A|HR 6622 | A double. A|HR 6693 | B:Delta-V implies B is class Ib-II. A|HR 6693 | Stephenson (1960) has G8II. A|HR 6751 | B:colors give K4V, though no con- A|HR 6751 | tamination apparent in A|HR 6751 | spectrum. A|HR 6751 | AB:underexposed spectrum. A|HR 6832 | B:strong contamination in green A|HR 6832 | region. G7IV-V fits Delta-V and A|HR 6832 | colors. A|HR 6855 | A:Class IIIa from Delta-V and the A|HR 6855 | suggested classification of B. A|HR 6855 | B:colors suggest F8V. A|HR 6855 | ISO:The primary fits with class A|HR 6855 | IIIa, and it could have a A|HR 6855 | collapsed SB secondary itself A|HR 6855 | as noted by BSC4. A|HR 7226 | DYN:p 120.42; a 1.907 (FS). A|HR 7226 | par. 0.051; Ma 1.83; Mb 1.79 A|HR 7398 | B:Ra photometry is considerably A|HR 7398 | in error. A|HR 7959 | A&B:underexposed 67 A/mm spectra A|HR 7959 | gave class V for both com- A|HR 7959 | ponents (Corbally and Garrison A|HR 7959 | 1980). Reddening from the A|HR 7959 | classifications. A|HR 7959 | ISO:Isochrones suggest both com- A|HR 7959 | ponents have luminosities near A|HR 7959 | the m.s. A|HR 7989 | A:previously classified as KOIII A|HR 7989 | (Corbally and Garrison 1980). A|HR 7989 | B:contamination especially A|HR 7989 | obvious below lambda-4200. A|HR 7989 | Photometry indicates F9V. A|HR 7989 | ISO:The binary fits isochrones as A|HR 7989 | classified. If A is class III, A|HR 7989 | then it may be HB star. A|HR 8140 | B:Both spectrum and photometry A|HR 8140 | show GOV, not A7V as in BSC4. A|HR 8140 | AB:composite spectrum is like a A|HR 8140 | proto-Am star. A|HR 8148 | A:spectrum slightly weak-lined A|HR 8148 | around FeI 4143. Possibly this A|HR 8148 | is due to the SB companion. A|HR 8148 | B:heavy contamination shown by a A|HR 8148 | washed-out spectrum. Type from A|HR 8148 | Cr triplet. Photometry indica- A|HR 8148 | tes K7V. A|HR 8202 | A:SrII 4077 and FeII 4172/9 A|HR 8202 | strong (both about class II A|HR 8202 | strength). Delta-V indicates lumi- A|HR 8202 | nosity is class IV. A|HR 8280 | A:all lines slightly washed out. A|HR 8280 | Not clearly metal weak (colors A|HR 8280 | normal), nor contaminated. A|HR 8280 | B:No contamination apparent. A|HR 8280 | Seems genuine new Am star. A|HR 8386 | A:broad lines with sharp central A|HR 8386 | absorption at H-gamma and H-delta. A|HR 8386 | CaII K slightly strong; Mg II 4481 A|HR 8386 | and He I 4026 slightly weak. A|HR 8386 | BSC4 notes H-alpha emission in com- A|HR 8386 | posite spectrum. A|HR 8386 | B:Hydrogen lines slightly washed A|HR 8386 | out; probably from con- A|HR 8386 | tamination. A|HR 8540 | A:Reddening from the A|HR 8540 | classification. A|HR 8540 | B:Hydrogen F9-G1; G band is F5 A|HR 8540 | strength; metals near F0. A|HR 8540 | Spectrum has weakened, fuzzy A|HR 8540 | lines. A|HR 8540 | ISO:Metal weakness confirmed. A|HR 8602 | B:Type very uncertain due to A|HR 8602 | large contamination. Isochrone A|HR 8602 | suggests B has (B-V) = 0.72 A|HR 8602 | (i.e. G6V). A|HR 8635 | B:Image tube spectrum and con- A|HR 8635 | taminated. HW photometry A|HR 8635 | suggests MOV. A|HR 8635 | A&B:Delta-V observed as 4.89 (HW), A|HR 8635 | 3.96 (Ra), 5.08 (Wayman 1962). A|HR 8635 | Suspected variable. A|HR 8635 | ISO:good fit of binary to isochrone A|HR 8635 | implies HW photometry correct. A|HR 8695 | A:very sharp lined spectrum. A|HR 8695 | B:Hydrogen lines appear con- A|HR 8695 | taminated. Rest of spectrum A|HR 8695 | and photometry gives F5 V. A|HR 8760 | A:possibly slight enhancement of A|HR 8760 | BaII 4554. A|HR 8760 | A|HR 8760 | spectrum, though photometry A|HR 8760 | gives F8IV-V. A|HR 8760 | ISO:A is probable HB star. A|HR 8956 | A:colors suggest K3.5III. A|HR 9044 | ISO:B possibly pre-m.s., else A|HR 9044 | optical. A|HD 41628 | A&B:HW comments that combined light A|HD 41628 | photometry is of low weight. A|HD 41628 | Classification shows that V and A|HD 41628 | B are good, but U is too large A|HD 41628 | by ~ 0.06. A|HD 85100 | B:New Ap star with SrII 4077 A|HD 85100 | strong (class III strength). A|HD 99279 | DYN:p 421.5; a 5.760; (FS). A|HD 99279 | par. 0.099; Ma 0.60; Mb 0.50 A|HD 99279 | B:slightly washed out lines con- A|HD 99279 | firm contamination. Photometry A|HD 99279 | gives MOV. A|HD 105563| A:spectrum is composite and shows A|HD 105563| A|HD 105563| 4287, 4358 and 4413. This VV A|HD 105563| Cephei type star has been A|HD 105563| described by Lynga (1973). A|HD 105563| B:Lynga has B2V. The present A|HD 105563| spectrum is rather underex- A|HD 105563| posed, but its classification A|HD 105563| gives the same E(B-V) as the A|HD 105563| 2-color diagram. A|HD 134799| A:New peculiar (SrCrMg) star. A|HD 134799| CaII K weak (A4 strength), A|HD 134799| shallow and diffuse. A|HD 158320| A:Garrison et al. (1977) have A|HD 158320| B0.5II, which agrees with Delta-V. A|HD 158320| A&B:This system was discussed by A|HD 158320| Penny et al. (1975) as the A|HD 158320| optical counterpart of an X-ray A|HD 158320| source. B|HD 7693 | DYN:p 81.29; a 1.078 (FS); B|HD 7693 | Par. 0.050; Ma 0.80; Mb 0.69 B|HD 7693 | ISO:Delta-(B-V) = 0.06, not 0.17 B|HD 7693 | as observed. B|HD 99803 | B:New proto-Am star. B|HD 122510| A&B:No area scanner photometry for B|HD 122510| this Holden 1976 binary. B|HD 130458| A&B:No area scanner photometry for B|HD 130458| this Holden 1975 binary. B|HD 130458| B:No evidence in spectrum for con- B|HD 130458| tamination despite a CF=33. B|HD 130458| AB:Classification is a compromise B|HD 130458| between G2 and G5 III for this B|HD 130458| composite. B|HD 130458| ISO:A is probably HB star, as discussed B|HD 130458| by Corbally and Garrison 1980, who B|HD 130458| classified the components as G8 IIb B|HD 130458| and F8 III. B|HD 163029| A:Spectrum is underexposed. B|HD 163029| ISO:Delta-(B-V) = 0.10, not 0.44 as observed. B|HD 165189| DYN:p 191.23; a 1.062 (FS). par. 0.018; B|HD 165189| Ma 2.89; Mb 2.85 B|HD 165189| B:lines appear double, especially Ca I 4226. B|HD 184189| A:Image-tube spectrum. B|HD 184189| B:Image-tube spectrum. Photometry suggests B|HD 184189| F4 III, so probably contaminated. B|HD 193281| B:Contamination makes type uncertain. B|HD 193281| C:Metals appear weak. Spectrum very like A, B|HD 193281| but greater rotation. Contamination from B|HD 193281| A possible since C is only 4" away. B|HD 194433| DYN:p 232.76; a 1.225 (FS). par. 0.020 B|HD 194433| ISO:B is class IV-V. B|HD 216763| B:Photometry, which fits isochrones, gives B|HD 216763| G5 V. ------------------------------------------------------------