Contents of: III/117/./notes.dat

The following document lists the file notes.dat from catalogue III/117.
Also available: plain copy of the file with f77 program to read file into arrays or line by line
File is also available in FITS, Tab-separated format, or in HTML.


## (from tabmap V6.0 (2016-08-18)) 2020-08-13T14:45:50
#---------------------------------------------------------------------------
#-- 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.
------------------------------------------------------------

© Université de Strasbourg/CNRS

    • Contact