HD   1337A  (AO Cas): SB2, orbit given by Stickland & Lloyd
HD   1337A  (1988Obs...108..174S). Tabulated values are means of measurements
HD   1337A  from SWPs 2489, 4456, and 7666 (spectroscopic phases 0.46, 0.25, and
HD   1337A  0.70). The system shows a strong `Struve-Sahade effect', and the
HD   1337A  results for component B are very scattered: 74, 142, and 96 km/s.
HD  13745   : This beta Cepheid variable (V354 Per) shows a `notched' peak in
HD  13745   the cross-correlation function. Only one high-resolution,
HD  13745   short-wavelength image is available in the archive (SWP 16111;
HD  13745   JD...4997.12).
HD  14434   : Highly structured cross-correlation function.
HD  15137   : Conti & Ebbets (1977ApJ...213..438C) report double lines partially
HD  15137   resolved. The cross-correlation function calculated from the only
HD  15137   high-resolution, short-wavelength image available in the IUE archive
HD  15137   (SWP 26978; JD...6363.82) is structured, but not straightforwardly
HD  15137   interpreted in terms of an SB2. The line-width reported in the Table
HD  15137   may reflect both rotation and orbital splitting.
HD  17505A  : The only available high-resolution SWP image (no. 8336;
HD  17505A  JD...4322.09), taken in the IUE small aperture (diameter 2.8"),
HD  17505A  gives a triple-peaked cross-correlation function. The system is an
HD  17505A  optical multiple (ADS 2161AB, IDS 02434+6000; Jeffers et al. 1963),
HD  17505A  with as many as 16 components within a radius of an arc minute
HD  17505A  (Sharpless 1954ApJ...119..334S), but only the B component
HD  17505A  (separation 2.1", Delta(m)=1.9) could possibly contaminate the IUE
HD  17505A  spectrum; the projection of the spatial separation in the dispersion
HD  17505A  direction would correspond to a velocity shift of 9 km/s between the
HD  17505A  IDS AB components. HD 17505 is previously known as a double-lined
HD  17505A  system (e.g., Conti & Ebbets 1977ApJ...213..438C). The `ABC'
HD  17505A  designations in the Table reflect the relative strengths of the
HD  17505A  cross-correlation function peaks, and may not correspond to the IDS
HD  17505A  designations.
HD  19820   (CC Cas): SB2 system, but with a large magnitude difference between
HD  19820   the components (DeltaB=1.6m, Petrie 1950PDAO....8..319P; 2.4m, Hill
HD  19820   et al. 1994A&A...282..455H). The cross-correlation function peak is
HD  19820   symmetrical and unstructured.
HD  35921Aa (LY Aur): SB2, orbit given by Stickland et al. (1994). Tabulated
HD  35921Aa values are means of concordant results from SWPs 6386, 9653, and
HD  35921Aa 9670 (spectroscopic phases 0.48, 0.08, and 0.53). In the notation
HD  35921Aa used in the Table, the binary system is Aab; component B is a visual
HD  35921Aa companion at a distance of 0.6" (Jeffers et al. 1963).
HD  36371   (chi/25 Aur): SB1 system (no. 231 in the catalogue of Batten,
HD  36371   Fletcher & Mann 1978PDAO...15..121B), but no recent orbit is
HD  36371   available. The cross-correlation function is asymmetric.
HD  36486   (delta Ori): SB1, orbit given by Harvey et al.
HD  36486   (1987Obs...107..205H). The tabulated value is the mean of concordant
HD  36486   measures from SWPs 13471, 13499, and 24208 (spectroscopic phases
HD  36486   0.172, 0.641, 0.795).
HD  37041   (theta2 Ori A): SB1, orbit given by Aikman & Goldberg (1976), who
HD  37041   make a possible detection of the secondary. The cross-correlation
HD  37041   function is single-peaked.
HD  37043A  (iota Ori): SB2, orbit given by Stickland (1987Obs...107....5S).
HD  37043A  Tabulated values are the averages of concordant measures from SWPs
HD  37043A  26567, 26573, and 26577, all taken near maximum orbital velocity
HD  37043A  separation in the system's eccentric orbit (spectroscopic phases
HD  37043A  0.00, 0.04, and 0.07).
HD  37468   (sigma/48 Ori A): SB2 (Bolton 1974ApJ...192L...7B); only one
HD  37468   cross-correlation function peak is apparent in SWP 7617
HD  37468   (JD...4247.82). The only other high-resolution SWP image, 14846, is
HD  37468   not available from the IUE archive.
HD  39680   : The structured cross-correlation function calculated from the only
HD  39680   high-resolution, short-wavelength image available in the IUE archive
HD  39680   (SWP 16236; JD...5002.39) strongly suggests an SB2 system, but Gies
HD  39680   & Bolton (1986ApJS...61..419G) found no evidence of radial-velocity
HD  39680   variations. The cross-correlation function structure may therefore
HD  39680   be a consequence of the star's peculiar spectrum.
HD  41161   : The cross-correlation function calculated from the only
HD  41161   high-resolution SWP image available in the IUE archive (no. 4078;
HD  41161   JD...3902.79) is structured. The system is an optical double
HD  41161   (IDS05582+4815; Jeffers et al. 1963), but with a large magnitude
HD  41161   difference (4.4m), and no evidence for orbital radial-velocity
HD  41161   variability was found by Garmany et al. (1980ApJ...242.1063G).
HD  41997   : The cross-correlation function calculated from the only
HD  41997   high-resolution, short-wavelength image available in the IUE archive
HD  41997   (SWP 30163; JD...6821.26) is structured.
HD  46056   : The tabulated value is the mean of concordant measures from SWPs
HD  46056   6949 and 8846 (JDs...4168.95, 4358.22). Given Walborn's
HD  46056   identification of a secondary spectrum in his classification
HD  46056   spectrogram (Walborn 1973AJ.....78.1067W), with DeltaB=0 (personal
HD  46056   communication), and the breadth of the cross-correlation function
HD  46056   peak, it is possible that the observed cross-correlation function
HD  46056   width represents a combination of rotational broadening and orbital
HD  46056   splitting.
HD  47129A  (Plaskett's star): SB2, orbit given by Stickland
HD  47129A  (1987Obs...107...68S). Tabulated values are averages of measures
HD  47129A  from SWPs 3347, 4819, and 8868 (spectroscopic phases 0.01, 0.10, and
HD  47129A  0.98). The B component difficult to measure reliably in SWP 4819 (as
HD  47129A  well as in several images taken near phase 0.5 which we examined),
HD  47129A  and the measures from the other two images are in poor mutual
HD  47129A  agreement: 111 and 147 km/s. The system shows a strong
HD  47129A  `Struve-Sahade effect' (e.g., Struve 1948).
HD  48099A  : SB2, orbit given by Stickland (1996Obs...116..294S). Tabulated
HD  48099A  results are the mean of concordant measures from six images (SWPs
HD  48099A  3345, 6423, 8143, 8340, 9952, and 52844; spectroscopic phases 0.50,
HD  48099A  0.01, 0.58, 0.45, 0.03, and 0.06).
HD  57060A  (UW CMa): SB2, orbit given by Stickland (1989Obs...109...74S). The
HD  57060A  rotation velocity for component A is the average of concordant
HD  57060A  results from 6 images (SWPs 2145, 2972, 4772, 46919, 49902, 53188;
HD  57060A  spectroscopic phases 0.93, 0.41, 0.81, 0.48, 0.91, 0.75). The B
HD  57060A  component shows a very wide spread of values (and is unmeasurable in
HD  57060A  SWPs 2145, 53188): 118-256 km/s. The system shows a strong
HD  57060A  `Struve-Sahade effect'.
HD  69106   : The asymmetric, broad cross-correlation function peak suggests a
HD  69106   possible SB2; only one short-wavelength, high-resolution image is
HD  69106   available (SWP 28158; JD...6533.32).
HD  72754   : SB1, orbit given by Levato et al. (1988ApJS...68..319L); Thackeray
HD  72754   (1971MNRAS.154..103T) describes the peculiar spectrum of this
HD  72754   system, concluding that the undetected secondary is probably the
HD  72754   more massive component. Five high-resolution SWP images are
HD  72754   available, and give highly variable and complex cross-correlation
HD  72754   function; for SWPs 6505 and 9077 the cross-correlation function is
HD  72754   double, but the measured velocities show that the secondary peak
HD  72754   does not correspond to the secondary star's spectrum. The v.sin(i)
HD  72754   value reported in the Table is derived from SWP 5837, which gives
HD  72754   the cleanest, narrowest, and most symmetric cross-correlation
HD  72754   function peak of the available images.
HD  75759A  : SB2, orbit given by Thackeray (1966MNRAS.134...97T).
HD  93161A  : The optical pair AB (IDS 10403-5903; Jeffers et al. 1963) are
HD  93161A  separated by 2", with sensibly identical apparent blue magnitudes
HD  93161A  and spectra (Walborn 1973ApJ...179..517W; Thackeray, Tritton &
HD  93161A  Walker 1973MmRAS..77..199T). The star designated A in the Table has
HD  93161A  the more positive velocity (and the slightly greater area under the
HD  93161A  cross-correlation function peak), and does not necessarily
HD  93161A  correspond to the IDS `A' component. The Radcliffe observers
HD  93161A  considered both components to be possible radial-velocity variables;
HD  93161A  Levato et al. (1991ApJS...75..869L) have published a preliminary SB1
HD  93161A  orbit, but do not identify the component to which it refers. There
HD  93161A  are two high-resolution SWP images in the archive (nos. 14740 and
HD  93161A  14741; JDs...4829.65, 4829.77), both taken through the small (2.8"
HD  93161A  diameter) entrance aperture. Since the IUE psf has fwhm=3" or worse,
HD  93161A  it is likely that the combined AB spectrum was recorded in the two
HD  93161A  images, which were obtained 2h 40m apart. The velocity of our A
HD  93161A  component is approximately constant, but the B component's velocity
HD  93161A  becomes almost 40 km/s more negative between the exposures. Since
HD  93161A  the semi-amplitude reported by Levato et al., 44 km/s, is only about
HD  93161A  20% of the velocity separation found in SWP 14741, 220 km/s, the
HD  93161A  possibility remains that both components are short-period binaries.
HD  93161A  The projection of the spatial separation of the components onto the
HD  93161A  dispersion direction corresponds to a zero-point difference of 7
HD  93161A  km/s between their spectra.
HD  93205A  : SB2, orbit given by Stickland & Lloyd (1993Obs...113..256S).
HD  93205A  Measures are from SWP 6367, taken near maximum orbital velocity
HD  93205A  separation in the system's eccentric orbit (spectroscopic phase
HD  93205A  0.97), and the only image in the archive which shows both components
HD  93205A  well resolved with the tau Sco template. SWP 6611 (phase 0.31) shows
HD  93205A  the secondary only very weakly, suggesting a possible
HD  93205A  `Struve-Sahade' effect.
HD  93206A  : Components A and B are the primaries of two unresolved SB1 systems
HD  93206A  (Leung, Moffat & Seggewiss 1979ApJ...231..742L). Tabulated values
HD  93206A  are averages of measures from SWPs 4707, 9018, 49996, and 50035
HD  93206A  (spectroscopic phases 0.76, 0.34, 0.29, 0.83 in the 6-d `A' orbit,
HD  93206A  and 0.27, 0.00, 0.15, 0.71 in the 21-d `B' orbit; the phases in the
HD  93206A  two orbits are uncertain by 0.18 and 0.14 cycles, respectively, for
HD  93206A  the most recent pair of images). The B-component measures show a
HD  93206A  rather large spread (v.sin(i)=67-125 km/s), but this is probably due
HD  93206A  simply to the difficulty in measuring its weak, often blended
HD  93206A  cross-correlation function peak.
HD  93403A  : SB2, orbit given by Thackeray & Emerson (1969MNRAS.142..429T); the
HD  93403A  secondary is only marginally detected in the optical spectra. Of ten
HD  93403A  spectra available in the IUE archive, only two show well-resolved
HD  93403A  lines (SWP 2625, JD...3762.90; SWP 9075, JD...4382.34; average
HD  93403A  values are reported in the Table), and in neither case is the
HD  93403A  cross-correlation function well-defined with the tau Sco template.
HD  93521   : The terminal velocity is latitude-dependent (Howarth & Reid
HD  93521   1993A&A...279..148H).
HD  93827   : Possible SB2 (Garrison, Hiltner & Schild 1977ApJS...35..111G); the
HD  93827   only high-resolution SWP image available (50536) gives a single
HD  93827   cross-correlation function peak.
HD  96917   : The only high-resolution, short-wavelength image available in the
HD  96917   IUE archive (SWP 7697; JD...4258.21) gives an asymmetric
HD  96917   cross-correlation function.
HD  97484A  : SB2, orbit given by Stickland, Lloyd & Corcoran
HD  97484A  (1994Obs...114..284S). Results are averages of concordant measures
HD  97484A  on SWPs 40517 and 40526 (spectroscopic phases 0.98 and 0.56).
HD 100213A  (T U Mus): SB2, orbit given by Stickland et al.
HD 100213A  (1995Obs...115..317S). Results are the average of measures on six
HD 100213A  images (SWPs 19642, 37906, 54356, 54397, 54407, and 54426; orbital
HD 100213A  phases 0.06, 0.58, 0.04, 0.39, 0.98, and 0.59). The measures are
HD 100213A  reasonably concordant, but the B component shows a larger range of
HD 100213A  values than might be expected (s.d. 25 km/s), and there is good
HD 100213A  evidence for a `Struve-Sahade effect'.
HD 101131A  : The cross-correlation function calculated from the only available
HD 101131A  high-resolution SWP image (SWP 7703; JD...4258.51) appears to be a
HD 101131A  blend of a redshifted, relatively narrow peak and a broad,
HD 101131A  blueshifted component, and has been fitted as such, but the fit is
HD 101131A  not well constrained for such severely blended components,
HD 101205   : The tabulated v.sin(i) is the mean of concordant values from SWPs
HD 101205   6142 and 22104 (JDs...4095.13, 5727.59), but the radial velocities
HD 101205   differ by 210 km/s. Radial-velocity variability has previously been
HD 101205   reported by Thackeray & Wesselink (1965MNRAS.131..121T) and by
HD 101205   Ardeberg & Maurice (1977A&AS...28..153A), and EB-type photometric
HD 101205   variations with P=2.08d have been reported by Balona
HD 101205   (1992MNRAS.254..404B; he mistakenly identifies it as HD 101191) and
HD 101205   by Mayer, Lorenz & Drechsel (1992IBVS.3765....1M).
HD 101436   : The tabulated v.sin(i) is the mean of concordant values from SWPs
HD 101436   6938 and 6972.
HD 115071A  : Only one high-resolution, short-wavelength image is available in
HD 115071A  the archive (SWP 10009; JD...4487.47). The cross-correlation
HD 115071A  function is double-peaked, and Conti, Leep & Lorre
HD 115071A  (1977ApJ...214..759C) considered the radial velocity to be variable;
HD 115071A  the system is almost certainly an SB2.
HD 135240A  (delta Cir): SB2, orbit given by Stickland et al.
HD 135240A  (1993Obs...113..139S). The tabulated results are the means of
HD 135240A  measures on SWPs 45682 and 45730 (spectroscopic phases 0.25, 0.75).
HD 148937   : The tabulated v.sin(i) is the mean of concordant values from SWPs
HD 148937   2754, 2893, 2988, and 9717.
HD 149404A  (V918 Sco): SB2, orbit given by Stickland & Koch
HD 149404A  (1996Obs...116..145S). Results are the average of measures on six
HD 149404A  images near quadratures (SWPs 2756, 9631, 9675, 54350, 55252, and
HD 149404A  55303; spectroscopic phases 0.49, 0.09, 0.50, 0.97, 0.43, and 0.94).
HD 149404A  The cross-correlation peaks are blended at all times, and the fits
HD 149404A  were constrained such that the separations were fixed at the values
HD 149404A  calculated from the orbit given by Stickland & Koch (1996). The
HD 149404A  system appears to show a moderately strong `Struve-Sahade effect'.
HD 150136   : SB2 with considerable magnitude difference between components
HD 150136   (Garmany, Conti & Massey 1980ApJ...242.1063G). The tabulated value
HD 150136   is the mean of SWPs 9718 (v.sin(i)=153 km/s) and 13778 (97 km/s).
HD 150136   The cross-correlation function peak in 13778 is very distorted; both
HD 150136   images probably contain unresolved peaks from both components in
HD 150136   this SB2 system, and the tabulated value is therefore of doubtful
HD 150136   interpretation.
HD 152218A  : SB2, orbit given by Hill, Crawford & Barnes (1974AJ.....79.1271H).
HD 152218A  Results are averages of measurements on SWPs 16203 and 45463, which
HD 152218A  show large velocity separations of the components (phases in the
HD 152218A  Hill et al. orbit are uncertain by more than one cycle at the time
HD 152218A  of these observations).
HD 152236   : Very asymmetric cross-correlation function (extended to blue).
HD 152246   : The tabulated v.sin(i) is the mean of concordant values from SWPs
HD 152246   16117 and 16214. The cross-correlation function are asymmetric
HD 152246   (extended to blue).
HD 152248A  : SB2, orbit given by Stickland et al. (1996Obs...116..226S).
HD 152248A  Tabulated results are the mean of measures from six images which
HD 152248A  give concordant widths (SWPs 6393, 9630, 45501, 54359, 54427, and
HD 152248A  55262; spectroscopic phases 0.80, 0.25, 0.77, 0.19, 0.79, and 0.23).
HD 152248A  The system shows the `Struve-Sahade effect'.
HD 152249   : SB2 according to Conti & Ebbets (1977ApJ...213..438C); possible
HD 152249   radial-velocity variable according to Bolton & Rogers
HD 152249   (1978ApJ...222..234B); photometric variable (Delta{V}=0.16)
HD 152249   according to Feinstein & Ferrer (1968PASP...80..410F). The three
HD 152249   high-resolution, SWP images available in the IUE archive (9720,
HD 152249   54571, and 55822; a fourth image, SWP 6847, was not accessible) all
HD 152249   show single cross-correlation function peaks, which agree in radial
HD 152249   velocity and line width, to within the errors; the mean v.sin(i) is
HD 152249   reported here.
HD 152667   : SB1 system (orbit given by Stickland & Howarth
HD 152667   1991Obs...111...23S), with no sign of the secondary component in the
HD 152667   cross-correlation function. The value reported here is the average
HD 152667   of two concordant values obtained at either quadrature (SWPs 2982
HD 152667   and 7833; spectroscopic phases 0.93 and 0.34).
HD 155775   : The cross-correlation function peak generated from SWP 7830
HD 155775   (JD...4270.47) shows a redwards `shoulder' which is absent in the
HD 155775   other two images available (SWPs 7838, 7861; JDs...4271.29,
HD 155775   4273.60). The tabulated v.sin(i) value is the mean of the concordant
HD 155775   measures derived from all three images. Garrison et al.
HD 155775   (1977ApJS...35..111G) report the system as SB2, but without giving a
HD 155775   magnitude difference; Garmany et al. (1980ApJ...242.1063G) find SB1.
HD 156359   : The tabulated value is the mean of concordant measures from SWPs
HD 156359   4733, 35646, and 35650.
HD 159176A  : SB2, orbit given by Stickland et al. (1993Obs...113..204S). The
HD 159176A  tabulated values are the means of measures from SWPs 9735, 45686,
HD 159176A  and 45727 (spectroscopic phases 0.56, 0.00, and 0.50) which give
HD 159176A  concordant line-widths but variable line strengths (the
HD 159176A  `Struve-Sahade effect').
HD 163181   : Asymmetric cross-correlation function (extended to blue).
HD 164816   : The cross-correlation function from SWP 15308 (JD...4899.21) is
HD 164816   `notched', giving the appearance of a partially resolved SB2 system;
HD 164816   when fit with a single Gaussian, v.sin(i)=190 km/s is inferred. The
HD 164816   only other high-resolution SWP image available in the archive, SWP
HD 164816   2814 (JD...3782.34), shows a symmetrical cross-correlation function
HD 164816   peak which is clearly narrower; it is the value from this image that
HD 164816   is entered in the Table. The system is almost certainly SB2.
HD 165052A  : SB2, orbit given by Morrison & Conti (1978ApJ...224..558M). The
HD 165052A  tabulated values are the averages of concordant measures from SWPs
HD 165052A  6392, 50034, 54352, and 54377 (orbital phases 0.55, 0.1, 0.2, 0.4;
HD 165052A  the phase uncertainty is 0.3 in the most recent images).
HD 167771A  : SB2, orbit given by Morrison & Conti (1978ApJ...224..558M). The
HD 167771A  tabulated values are the averages of concordant measures from SWPs
HD 167771A  2832, 6363, 54385, and 54414 (orbital phases 0.77, 0.31, 0.19, 0.62;
HD 167771A  the phase uncertainty is 0.09 in the most recent images).
HD 167971A  : The system comprises component A accompanied by a spectroscopic
HD 167971A  and eclipsing binary, Ba+Bb (Leitherer et al. 1987A&A...185..121L).
HD 167971A  The cross-correlation function peak in SWP 28297 (photometric phase
HD 167971A  0.63) shows a bluewards `shoulder' which is absent in the only other
HD 167971A  high-resolution short-wavelength image in the archive, SWP 28287
HD 167971A  (0.03). The widths of the main peaks are in good agreement, and the
HD 167971A  mean value is given in the Table. Leitherer et al. estimate the
HD 167971A  continuum intensity difference from optical line ratios
HD 167971A  (Ba=Bb=0.25A) and eclipse depths (Ba=Bb=0.48A), but the latter
HD 167971A  estimate appears to be based on the full amplitude of the
HD 167971A  light-curve (Delta(m)=0.3), and does not allow for the substantial
HD 167971A  `ellipsoidal' variations. Adopting a more realistic Delta(m)=0.2
HD 167971A  brings the photometric value into perfect accord with the
HD 167971A  spectroscopic estimate, and implies that Ba and Bb are each 1.5m
HD 167971A  fainter than A, in agreement with the relatively weak signature of
HD 167971A  the secondaries in the cross-correlation function.
HD 190603   : Asymmetric cross-correlation function (extended to blue).
HD 191201   : SB2, orbit given by Plaskett (1926). Only one high-resolution SWP
HD 191201   image is available in the archive.
HD 191423   : v(infty), which is probably latitude-dependent, has been corrected
HD 191423   for a stellar radial velocity of -90 km/s.
HD 192660   : Asymmetric cross-correlation function (extended to blue).
HD 206267Aa : The brightest member of an optical quadruple system. Component Aa
HD 206267Aa (=star A3 in Stickland 1995Obs...115..180S) is stationary and gives
HD 206267Aa the stronger cross-correlation function peak (with the tau Sco
HD 206267Aa template), while Ab (=star A1) orbits an undetected (or only
HD 206267Aa marginally detected) Ac. The cross-correlation function peaks of Aa
HD 206267Aa and Ab are strongly blended at all phases, and we fixed the
HD 206267Aa separations at the values calculated from the orbit given by
HD 206267Aa Stickland (1995) in order better to constrain the line widths.
HD 209481A  (LZ Cep): SB2, orbit given by Howarth et al. (1991Obs...111..167H).
HD 209481A  Tabulated results are the means of concordant measures from SWPs
HD 209481A  38911, 38939, 38977, and 39010 (spectroscopic phases 0.55, 0.00,
HD 209481A  0.06, and 0.49).
HD 215835A  (DH Cep): SB2, orbit given by Sturm & Simon (1994A&A...282...93S).
HD 215835A  Measures are from SWP 45503 (photometric phase 0.76); other images
HD 215835A  are available in the archive, but yield uncertain results with the
HD 215835A  tau Sco template.
HD 224151A  (V373 Cas): SB2, orbit given by Hill & Fisher (1987A&A...171..123H).
HD 224151A  Four high-resolution images are available; tabulated values are
HD 224151A  means of SWPs 20973 and 22446 (JDs...5586.28, 5769.27), which give
HD 224151A  double-lined cross-correlation function.
HD 242908   : The double-peaked cross-correlation function calculated from the
HD 242908   only available short-wavelength, high-resolution image (SWP 16092;
HD 242908   JD...4992.27) suggests that this may be a previously unrecognized
HD 242908   SB2 system, with nearly equal components separated by 150 km/s and
HD 242908   each with v.sin(i)=90-100 km/s (Gaussian FWHM 130-140 km/s); an
HD 242908   acceptable fit is possible with a single peak, however.
HD 332407   : Probable eclipsing binary (Lipunova & Putilina
HD 332407   1985IBVS.2766....1L).
CPD-59 2603 (Tr16-104): The cross-correlation function shows 3 peaks. Only two
CPD-59 2603 high-resolution SWP spectra are available in the IUE archive; these
CPD-59 2603 show no significant difference in the velocity separation of the BC
CPD-59 2603 components, but a large change in the velocity of component A. The
CPD-59 2603 simplest interpretation is that there are at least 4 components,
CPD-59 2603 with component A the SB1 system for which preliminary orbital
CPD-59 2603 elements are given by Levato et al. (1991ApJS...75..869L).
CPD-59 2603 Spectroscopic multiplicity had already been strongly suspected by
CPD-59 2603 Walborn (1973AJ.....78.1067W), and also by Levato & Malaroda
CPD-59 2603 (1991ApJS...75..869L), who classified the spectrum as `O7: V: +
CPD-59 2603 Companion?' (cp. Walborn's O7 V ((f)), with the comment `secondary
CPD-59 2603 spectrum visible?'). The components must be close together; there is
CPD-59 2603 no significant spatial extension evident in the IUE echellograms,
CPD-59 2603 and Walborn's careful observing notes, made in connection with his
CPD-59 2603 classification spectrogram, make no mention of a visual companion
CPD-59 2603 (personal communication). Massey & Johnson (1993AJ....105..980M;
CPD-59 2603 their star 408) obtain a distance modulus, based on spectroscopic
CPD-59 2603 parallax, of V(0)-M(V)=12.2, which is less than the mean cluster
CPD-59 2603 value of 12.55, but not significantly so.