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## (from tabmap V6.0 (2016-08-18)) 2024-05-19T07:41:52
#---------------------------------------------------------------------------
#-- J/MNRAS/284/265 Rotational Velocities of 373 OB stars (Howarth+ 1997)
#--------------------------------------------------------------------------
#---Table: J/MNRAS/284/265/./notes.dat Individual Notes (346 records)
# Name A11 --- Name of star (repeated if several lines)
# Text A68 --- Text of note
--------------------------------------------------------------------------------
Name |Text
-----------|--------------------------------------------------------------------
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.
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