(1) Classified only on low-dispersion (2 Å) spectrograms that were over-exposed in the 4500-4800 Å region. For these stars no barium index could be assigned.
(2) Classified also on spectrograms with a resolution of about 0.3 Å. For these stars barium indices ranging from 0.2 to 0.9 could be assigned. On these spectrograms the intensities of SrI 4607, ZrI, and a number of rare-earth ions could be estimated.
(3) Classified also on spectrograms which had a resolution of about 0.3 Å, but were too dark in the 4500-4600 Å regions to allow the Ba II and Sr I lines to be observed. Rare-earth lines at shorter wavelengths allowed the barium index to be estimated.
(4) Classified only on low-resolution spectrograms which because of the steep spectral gradients did not permit estimation of features below about 4400 Å.
(5) Classified only from spectrograms covering the yellow and red regions. When CH and SiC2 indices are given for such stars they are based on the intensities published by other observers.
Notes indicated by an asterisk in the table:
VX And = HD 1546. An SRa variable intermediate between the semi-regular variables and the Miras. The SRa variables show only moderate Balmer emission near maximum light. In the spectrum of VX And both the isotopic carbon bands and the SiC2 (MS) bands are very strong, as in T Mus.
DL Cas = BD +59 65. Cepheid variable (P = 8.00 days) generally accepted as a member of the cluster NGC 129.
BD +59 70. The star is Kraft AB (1958) in the field of the galactic cluster NGC 129. It is a foreground star.
BD +59 73. The star is Kraft AA in the field of NGC 129. It is a foreground star.
HD 2901. Vr = -107 km/sec. This is a moderately metal-poor star that happens to lie at a low galactic latitude (b = -9).
Eta Cas B = HD 4614 B. All the normally strong lines in the blue region are shallow, but the lines in the red appear normal.
Eta And = HD 5516. This is a two-line spectroscopic binary, but the spectrum looks normal at low dispersion. The secondary is only slighter fainter than the primary.
V 487 Cas = BS 316. Vr = -94.5 km/sec.
HD 6833. A typical metal-deficient star of the halo population. Vr = -248 km/sec.
Psi3 Psc = BS 339 = HD 6903. V sin i = 91. Active chromosphere (Strickland, Williams, 1983).
39 Cet = AY Cet = BS 373. Variable by about 0.2 mag. (Olsen, 1974). H, K em.
V 466 Cas = BD +57 258 = HD 236697. The star is a well-established member of NGC 457.
BD +60 265. Possible member of association Cas OB 8.
BD +59 274. Probable member of NGC 581.
61 Cet = BS 610 = HD 12641. The spectrum, recognized as composite by Appenzeller in 1967, was classified by Markowitz in his OSU MS thesis of 1969 as G2 III + F2 V. The spectrum appears similar on our spectrograms to BS 1176, which was classified here as G2 III + F6: V:. R. Griffin(1995) had established that the star is a spectroscopic binary, and determined an orbit.
67 Cet = BS 666 = HD 14129. At higher resolution a slight enhancement of s-process lines appears to be present, but not enough for the star to be called a marginal barium star.
V Ari = HD 13826. The published Vr = -176 km/sec.
HD 16068. The star is #1 in the cluster Trumpler 2. Membership doubtful.
HD 16115. Yamashita (1975) called this a CH-like star because it had the spectrum of a CH star, but a low velocity relative to the sun.
BS 885 = HD 18774. Bidelman called attention to this peculiar star and pointed out that the near absence of both CN and CH implies a deficiency of carbon in its atmosphere.
BS 965 = HD 20084. This star is more luminous than most of the early G-type CH stars observed by Bond. It most nearly resembles BS 8626 (see Plate 9 of the Atlas of the Spectra of the Cooler Stars, by Keenan and McNeil). It is probably a halo star near the top of the Population II giant branch.
TW Hor = BS 917 = HD 20234. This is Herschel's red star.
BS 1112 = HD 22764. The weakness of the metal lines, plus slight strengthening of H delta and slight filling in of H and K, suggest a composite spectrum.
HD 24035. This southern barium star has such strong CH and CN bands that it might be considered a marginal CH star, or a barium-carbon star (MacConnell et al., 1972).
HD 24281. This can be considered a marginal CH star.
HD 27277. The star is Hoag #4 in NGC 1545. HD 27292 is #3.
DG Eri = HD 27598. Vr = -98 km/sec.
HD 28099 = VB 64. The star is Van Bueren #64 in the Hyades. H and K are slightly shallow.
HD 283750 = BD +26 730 = Gl 172A. A BY Dra variable. Fairly strong H, K em.
R Dor = BS 1492 = HD 29712. An SRb variable.
BD +38 955 = KZP 1745 = MSB 10. An LB variable. Photographic range is 11.7 to 12.5.
12 Cam = BS 1623 = HD 32357. A spectroscopic binary with H, K em.
HD 33793 = Gl 191. This is Kapteyn's star (See Yerkes Atlas, Pl. 19). The peculiarity lies in the enhancement of the Ca I and Cr I lines relative to the strength of the TiO bands. The type is assigned from the strength of the latter, placing the star more than one magnitude below the main sequence.
Alpha Aur A = BS 1708 = HD 34029. The type corresponds to the phase when the primary dominates the spectrum. The influence of the secondary (of slightly earlier type) is not entirely absent, but Capella is included in the catalog because of its importance as an early G-type binary with one of the best-determined orbits.
HD 271182 = CPD -65 457. LMC.
TU Tau = HD 38218. Called composite by Richer. We have no blue observations.
BS 2018 = HD 39045. Vr = +105 km/sec.
BS 2028 = HD 39225. Vr = +101 km/sec. BS 2018 and 2028, about 2 degrees apart, have not only similar radial velocities but also similar proper motions.
36 Cam = HD 41927. The luminosity class is a little too faint for the Hipparcos parallax, which corresponds to MV = -0.9. The CH band is slightly weaker than normal.
HD 49068. Probably a member of cluster NGC 2287.
HD 49091. Although in the field of NGC 2287, the star is probably not a member of the cluster.
HD 49105. Probably a member of NGC 2287.
BD -20 1568 = HD 49212. Probably a member of NGC 2287.
HD 49500. The weakness of both CN and CH suggests a deficiency of carbon.
Omicron1 CMa = BS 2580 = HD 50877. Possible member of cluster Cr 121.
HD 52938. In cluster M59 = NGC 2323.
BD -9 1935. Hoag No. 3 in cluster NGC 2353. Probably a member.
145 CMa = BS 2764 = HD 56577. Possible member of Omicron1 CMa group.
BS 2786 = HD 57146. VV Cep system with companion of type B8 III or A0 III (Parsons, 1982)
YY Gem = HD 60179C = Alpha Gem C. BY Dra eclipsing binary. The metallic lines in the blue are all shallow, though Ca 4226 Å is wide.
HD 69898, HD 60899. These giants are in the field of NGC 2422, but have not been considered members because of their proper motions, The luminosity of HD 60898 (MV = -1.25) places it at nearly the distance of the cluster. HD 60899 has a lower luminosity (MV = 0.30) and is thus about 1 magnitude too faint to be a likely cluster member.
R Pup = BS 2974 = HD 62058. Possible member of NGC 2439.
CPD -31 1790. In NGC 2439.
BS 3043 = HD 63660. The apparent weakness of the metal lines may be due to the presence of components from the companion in this spectroscopic binary.
BS 3120 = HD 65662. Close to open cluster NGC 2516. If the star is a member, MV = -2.32.
341 Car = BS 3126 = HD 65750. Probable member of NGC 2516.
BS 3153 = HD 66342. Cox's star No. 110 in NGC 2516. The star is a member of the cluster.
HD 68879. No. 8 in NGC 2548. The weakness of the K line and the 3883 CN band suggest a companion of type F, but this is not certain.
HD 73598. Probable member of Praesepe.
39 Cnc = BS 3427 = HD 73665. Probable member of Praesepe.
BS 3428 = HD 73710. Probable member of Praesepe.
HD 73974. Probable member of Praesepe.
HD 75021. Common proper motion with HD 75022. Hipparcos parallax is negative.
HD 75022. The luminosity class assumes normal solar composition, but if the suspected barium enhancement is real, the luminosity could be lower. The negative Hipparcos parallax would imply a higher luminosity than the spectrum allows.