Baltic Astronomy, vol. 6, 499-572, 1997.
CLASSIFICATION OF POPULATION II STARS IN THE VILNIUS PHOTOMETRIC SYSTEM. II. RESULTS
A. Bartkevicius1 and R. Lazauskaite1 '2 1 Institute of Theoretical Physics and Astronomy, Gostauto 12, Vilnius 2600, Lithuania 2 Department of Theoretical Physics, Vilnius Pedagogical University, Studenty. 39, Vilnius 2340, Lithuania
Received April 20, 1997.
Abstract. The results of photometric classification of 848 true and suspected Population II stars, some of which were found to be- long to Population I, are presented. The stars were classified using a new calibration described in Paper I (Bartkevicius & Lazauskaite 1996). We combine these results with our results from Paper I and discuss in greater detail the following groups of stars: UU Herculis-type stars and other high-galactic-latitude supergiants, field red horizontal-branch stars, metal-deficient visual binaries, metal- deficient subgiants, stars from the Catalogue of Metal-deficient F-M Stars Classified Photometrically (MDPH; Bartkevicius 1993) and stars from one of the HIPPARCOS programs (Bartkevicius 1994a). It is confirmed that high galactic latitude supergiants from the Bartaya (1979) catalog are giants or even dwarfs. Some stars, identified by Rose (1985) and Tautvaisiene (1996a) as field RHB stars, appear to be ordinary giants according to our classification. Some of the visual binaries studied can be considered as physical pairs. Quite a large fraction of stars from the MDPH catalog are found to have solar metallicity. A number of new possible UU Herculis-type stars, RHB stars and metal-deficient subgiants are identified.
Key words: techniques: photometric - stars: fundamental para- meters (classification) - stars: Population II 500 A. Bartkevicius and R. Lazauskaite
1. INTRODUCTION
Although Population II stars are rare in the solar neighborhood, they play an important role in different branches of astronomy due to their unique characteristics - they are the oldest stars in the Galaxy and, consequently, exhibit metal-deficiency, high velocities and spend most of their life in the galactic halo. Despite a long history of investigation of the stellar content of our Galaxy, a generally accepted definition of stellar populations does not exist (Majewski 1993, King 1995). In this paper, as in our previous papers (Bartkevicius 1994b, Bartkevicius & Lazauskaite 1996, hereafter Paper I) we use the term Population II for stars with metallicity [Fe/H]< —0.5 and a total space velocity (or its radial or tangential components) >100 km s-1. It is obvious that we admit to our Population II sample not only extreme Population II (halo) stars, but also intermediate Population II (thick disk, partly old disk) stars. In this paper we present the results of three-dimensional classifi- cation in the Vilnius photometric system of 848 known or suspected Population II stars and some Population I stars (visual binaries, su- pergiants, etc.) necessary for comparison with Population II stars. For the classification we use the methods described in Paper I of this series. Combining the results of classification from this paper and the results of the reclassification of 809 standard stars from Pa- per I (this brings to 1657 the number of stars classified in a unique scheme), we discuss the following groups of Population II stars: UU Herculis-type stars, field RHB stars, visual binaries, metal-deficient subgiants, stars from the MDPH catalog (Bartkevicius 1993) and the HIPPARCOS program stars (Bartkevicius 1994a).
2. PREVIOUS RESULTS OF CLASSIFICATION
The development of methods for identification and classification of Population II stars in the Vilnius photometric system is briefly described in Paper I. Here we discuss applications of these methods for the determination of the main astrophysical parameters of Pop- ulation II stars. Bartkevicius & Sperauskas (1983) have classified 312 stars, among which a number of new giants and subdwarfs with high metal deficiency were identified. Twelve stars were suspected of being metal-deficient subgiants. It was estimated that about 20 % of high proper motion {¡JL > 0. 26 yr-1) stars are giants or subgiants. Classification of Population II stars 501
Bartkevicius & Tautvaisiene (1987) have made a three-dimen- sional classification of 78 known metal-deficient giants. Bartasiute (1989) has presented the results of classification of 343 stars in an area of 900 square degrees near the South Galactic Pole. Among the stars studied, 35 subdwarfs were identified. Also, the amount of interstellar reddening in this region was investigated. Bartasiute (1993) in her thesis has presented the results of clas- sification of 1189 stars. A majority of these stars are metal-deficient. The results of classification were combined with proper motion and radial velocity data, and space velocities and galactic orbits were calculated for these stars. On the basis of these data, a detailed analysis of stellar populations was carried out. Straizys et al. (1981) detected eight stars suspected of belonging to the red horizontal-branch stars. Recently, Tautvaisiene (1996a) has investigated 13 red horizontal-branch candidates identified by Rose (1985). She determined their spectral types, metallicities, abso- lute magnitudes, eifective temperatures and surface gravities. From a comparison of the observational HR diagram with isochrones, an age of 10-12 Gyr was obtained for these stars. Tautvaisiene (1987) also has calculated Te and log g for 110 metal-deficient giants from color indices in the Vilnius system and compared Te, log g plots with evolutionary tracks and isochrones. Bartkevicius et al. (1992) have classified in the Vilnius system 117 known and suspected Population II supergiants and related stars. Sperauskas (1987) has presented the photometric classification of 32 B and A stars suspected to belong to the blue horizontal- branch on the grounds of intermediate and low dispersion spectra or photometric color indices of various photometric systems. And, at last, in Paper I we presented the classification of 809 standard stars used for establishing new classification methods for Population II stars in the Vilnius photometric system.
3. OBSERVATIONS AND SELECTION OF STARS
According to sources of the observed color indices, the stars in- vestigated in this paper can be divided into two groups: (1) stars observed within several special programs of investiga- tion of Population II stars (see Subsection 3.1), (2) stars selected according to some criteria (see Subsection 3.3) from the General Photometric Catalog of Stars Observed in the Vil- nius Photometric System (Straizys & Kazlauskas 1993). 502 A. Bartkevicius and R. Lazauskaite
3.1. Programs of investigation of Population II stars
Since 1986, several long-term programs of the photometric in- vestigation of Population II stars in the Vilnius system have been started. Some of the investigations described in Section 2 have also been continued. Some stars are included in two or more programs. Below we list the programs and the groups of stars included: 1. Stars with known trigonometric parallaxes, absolute magni- tudes My and metallicities [Fe/H]; 2. HIPPARCOS program stars (Bartkevicius 1994a); 3. Eggen's halo and old disk moving group members (see Eggen 1996): stars from the Arcturus, a Puppis, Kapteyn and Groom- bridge 1830 moving groups; 4. Known and suspected UU Herculis-type stars, supergiants at high galactic latitudes, supergiants of normal chemical composition; 5. Field red horizontal-branch (RHB) candidates; 6. Metal-deficient subgiants; 7. Metal-deficient F-M stars classified spectroscopically from the MDSP catalog (Bartkevicius 1980) and its supplement MDSPS1 (Bartkevicius 1984) and stars from the Catalog of Metal-deficient F-M Stars Classified Photometrically (MDPH; Bartkevicius 1993); 8. Population II visual and spectral binaries; 9. Population II radial velocity program stars (Bartkevicius & Sperauskas 1990); 10. Some peculiar and astrophysically interesting stars. Not all of these programs have been completed at the present time. A detailed description of the programs related directly to the subject of the present study and a discussion of the results obtained will be presented in Section 6.
3.2. Observations
Photoelectric observations in the Vilnius photometric system were done with the 63 cm telescope of the Moletai Observatory (Lithuania), the 48 cm telescope of the Vilnius University and 1 m telescope of the Institute of Theoretical Physics and Astronomy, the two latter telescopes being located at the Maidanak Observa- tory in Uzbekistan. At our request, 10 stars were observed by K. Zdanavicius with the 61 cm telescope of the Mount John Obser- vatory, New Zealand. The time of observations, the telescopes used Classification of Population II stars 503
Table 1. Observing runs and references to the published results. No. Run Observatory, Publication telescope 1. March-May 1986 Moletai, 63 cm Tautvaisiene (1996a) 2. July 1986 Maidanak, 48 cm Lazauskaite & Tautvaisiene (1990) 3. April-May 1987 Moletai, 63 cm This paper 4. August 1987 Maidanak, 48 cm Lazauskaite & Tautvaisiene (1990) 5. August 1988 Maidanak, 1 m Lazauskaite & Tautvaisiene (1990) 6. October 1988 Maidanak, 1 m Lazauskaite & Tautvaisiene (1990) 7. May 1991 Maidanak, 1 m Lazauskaite (1992) 8. October 1991 Maidanak, 1 m Lazauskaite (1992) 9. October-December 1991 Mt. John, 63 cm Zdanavicius et al. (1995) and references to the published observational data are presented in Table 1. The Moletai Observatory measurements were made with the eight-channel automated photometer with a permanently rotating filter wheel for quasi-simultaneous measurements (Paskevicius et al. 1987). The reductions were performed by a differential method. The instrumental color indices were transformed to the standard system by color equations obtained from observations of the stars of various spectral and luminosity classes in the vicinity of the North Celestial Pole (Cernis et al. 1989). In all the Maidanak observing runs, one-channel photometers operating in the photon-counting mode and equipped with a stan- dard set of glass filters of the Vilnius system were used. For the trans- formation of observations to outside the atmosphere, the Nikonov (1953) method as modified by Zdanavicius (1975) was used. The ins- trumental magnitudes V and color indices were transformed to the standard system .with color equations obtained from observations of stars of various spectral and luminosity classes in the Cygnus Stan- dard Region (Zdanavicius & Cerniene 1985). To estimate the external accuracy, the observations done at Maidanak were compared with observations done by other observers and taken from the General Photometric Catalog of Stars Observed in the Vilnius Photometric System (Straizys & Kazlauskas 1993). The mean differences are given in Table 2. The accuracy of the color indices is of the order of ±0.01 mag. However, for U — P and P — X, the standard deviations reach ±0.02 mag. The accuracy of the 3-6 observing runs is, in general, 504 A. Bartkevicius and R. Lazauskaitè
Table 2. Mean differences between our magnitudes and color indices and those from the General Catalog (Straizys & Kazlauskas 1993). As are our values minus Catalog values. Magnitude or Observing runs and color index the number of common stars 3-6 (n=37) 7-8 (n=15) A V —0.003±0.027 —0.007±0.014 A (U-P) —0.008±0.024 +0.007±0.021 A (P-X) +0.006±0.025 —0.002±0.019 A(X-Y) -0.001±0.016 +0.004±0.012 A (Y-Z) —0.003±0.017 +0.000±0.012 A (Z-V) +0.002±0.013 -0.000i0.011 A (V-S) +0.000±0.019 +0.002±0.013
lower than that of the 7-8 runs. This is probably due to the obser- vations made with a smaller aperture telescope (48 cm). The unpublished magnitudes and color indices of stars are pre- sented in Table 3.
3.3. Selection of stars from the General Catalog of Vilnius photometry
The second source of data for our program was the General Pho- tometric Catalog of Stars Observed in the Vilnius System (Straizys & Kazlauskas 1993). It contains observational data published un- til 1992 as well as those which were prepared for publication while the catalog was in compilation. Having in mind that applying new methods described in Paper I gives more accurate classification of stars, we decided to reclassify all metal-deficient stars from this cat- alog. Stars, which are either metal-deficient or belong to Popula- tion II, are marked in this catalog by special symbols attached to their spectral types, as it is explained in Table 1 of the catalog (see Straizys & Kazlauskas 1993). These stars were selected for reclas- sification primarily. It is also expected that some of the stars in the Vilnius photometric catalog have not been recognized as metal- deficient. Therefore, we have classified all stars from the catalog by the method of color index comparison (Paper I) and picked out the stars with [Fe/H]< —0.50. We found over 150 stars which, according to our preliminary classification, show metal deficiency but have not Classification of Population II stars 505
Table 3. Unpublished measurements of Population II stars in the Vilnius photometric system.
Name «(1950) ¿(1950) V U-P P-X X-Y Y-Z Z-V V-S n G 8-50 04 38 20 +22 49.1 12.61 0.46 0.88 1.29 0.33 0.42 0.82 3 HD 36702 05 30 11 -38 35.5 8.72 0.97 0.83 1.24 0.67 0.30 0.85 1 G 99-31 05 42 12 +09 13.7 11.31 0.41 0.50 0.75 0.37 0.23 0.56 1 BD+53°979 05 57 42 +53 18.3 10.00 1.63 0.71 0.44 1.05 2 HD 73759 08 38 21 +45 02.4 7.94 0.65 0.70 0.64 0.27 0.16 0.45 8 HD 74132 08 40 29 +45 38.1 8.26 0.52 0.63 0.58 0.26 0.14 0.40 6 HD 74327 08 41 40 +44 22.0 8.84 0.59 0.64 0.60 0.27 0.13 0.43 8 HD 75555 08 48 59 +45 05.2 8.11 0.61 0.63 0.68 0.28 0.16 0.47 8 HD 77912 09 00 10 +38 51.1 4.62 0.64 0.94 1.32 0.50 0.30 0.76 5 HD 79452 09 12 10 +34 50.5 5.99 0.58 0.75 1.00 0.44 0.25 0.65 2 HD 81774 09 25 50 +43 26.2 8.41 0.61 0.70 0.54 0.22 0.13 0.35 6 BD+29°2055 09 26 37 +29 04.4 10.73 0.48 0.52 0.79 0.39 0.23 0.62 1 HD 84123 09 41 00 +42 16.3 6.78 0.59 0.67 0.48 0.26 0.13 0.37 2 HD 84800 09 45 36 +43 53.9 7.72 0.60 0.83 0.40 0.13 0.08 0.18 4 HD 85015 09 47 10 +44 14.2 8.36 0.51 0.58 0.56 0.25 0.16 0.42 6 HD 88923 10 13 24 +45 42.3 7.70 0.67 0.65 0.53 0.27 0.16 0.45 8 BD+30°2018 10 25 50 +29 45.1 10.20 0.58 0.98 1.28 0.47 0.27 0.75 1 BD+30°2022 10 26 36 +29 56.3 8.78 0.66 1.02 1.38 0.48 0.34 0.81 1 BD+30°2026 10 27 47 +30 04.0 9.97 0.60 0.92 1.24 0.45 0.30 0.72 1 BD+30°2027 10 28 10 +30 09.2 10.36 0.52 0.70 1.01 0.39 0.28 0.65 1 BD+30°2034 10 29 48 +29 49.8 10.32 0.71 0.98 1.48 0.59 0.32 0.82 2 ASW 1-56* 10 33 06 +29 11 10.41 0.46 0.55 0.74 0.34 0.19 0.54 1 HD 99829 11 26 43 +44 37.9 9.15 0.49 0.57 0.62 0.26 0.15 0.43 6 HD 101841 11 40 46 +28 19.9 7.69 0.63 0.67 0.57 0.26 0.15 0.42 4 HD 102102 11 42 38 +43 29.0 8.03 0.62 0.78 0.57 0.19 0.12 0.28 2 HD 102570 11 45 57 +46 24.5 8.28 0.51 0.61 0.60 0.25 0.14 0.41 4 HD 104425 11 58 58 +43 19.2 8.99 0.44 0.52 0.62 0.28 0.19 0.55 7 BD+28°2079 12 04 26 +28 04.5 10.05 0.66 0.84 1.16 0.50 0.28 0.75 5 BD+25°2502 12 21 45 +24 34.5 9.95 0.58 0.75 0.90 0.44 0.22 0.64 2 HD 108100 12 22 34 +43 08.3 7.06 0.49 0.64 0.53 0.22 0.15 0.44 8 HD 108464 12 25 04 +41 38.4 6.47 0.59 0.79 0.67 0.30 0.20 0.58 4 BD+30°2436 13 39 16 +29 54.7 9.90 0.79 0.86 1.22 0.53 0.30 0.78 1 HD 122052 13 56 36 +24 56.1 7.29 0.96: 0.95 1.35 0.62 0.34 0.88 4 HD 140385 15 40 14 +29 47.0 8.56 0.43 0.63 0.86 0.34 0.23 0.56 1 HD 148743 16 27 48 -07 24.4 6.46 1.32 0.81 0.48 0.28 0.16 0.41 1 HD 196866 20 37 12 +25 53.5 7.00 0.72 1.20 1.62 0.53 0.43 0.89 3 HD 223065 23 43 54 -41 50.9 7.25 0.58 0.73 0.41 0.29 0.00 0.25 1
* ASW 1-56: number from Ardeberg A., Sarg K., Wramdemark S. 1973, A&AS, 9, 163 506 A. Bartkevicius and R. Lazauskaite been marked in the catalog as metal-deficient stars. We added these stars to our list of stars to analyze them in more detail.
4. METHODS OF CLASSIFICATION
A detailed description of the methods of three-dimensional clas- sification of metal-deficient stars is presented in Paper I. Here we give only a short key-point description. For classification, three groups of methods have been used: (1) Method of a comparison of the observed color indices, in- trinsic color indices or reddening-free Q-parameters of the program stars and the standard stars. This method is based on the assump- tion that stars with coinciding color indices or Q-parameters have the same astrophysical parameters, in our case, spectral type, intrin- sic color index (Y — V)o, metallicity [Fe/H] and absolute magnitude My. This method is similar to the method of "star boxes" used in the Geneva system (Golay et al. 1977). For a comparison of the observed photometric quantities of stars under investigation, a set of 809 standard stars with known physical parameters has been used. (2) Determination of [Fe/H] from two-color diagrams and metal- licity indices 6 (CI) calibrated in terms of metallicity (Bartkevicius Sz Sperauskas 1983); this method has been used in a computerized version. (3) Determination of absolute magnitude from empirical rela- tions between absolute magnitude and some intrinsic color indices, separately for giants and dwarfs of different metallicities. For the stars of normal chemical composition or with small metal-deficiency, the two-dimensional classification program CLASS for single or binary stars (Vansevicius &; Bridzius 1994) was also used. If the determined color excess was negative or the distance to a star was < 50 pc, zero reddening was adopted. The observed color indices of stars were taken from the General Catalog of Straizys & Kazlauskas (1993), from Table 3 of the present paper, also from the papers of Lazauskaite & Tautvaisiene (1990, variable stars from Table 3), Tautvaisiene (1996a), Zdanavicius et al. (1995) and Bartasiute (1993) which were not included into the General Catalog. Color excess ratios, needed for the calculation of the intrinsic color indices and reddening-free Q-parameters, were taken from the following sources. For the extremely metal-deficient stars, they are from Lazauskaite (1997). For the stars of normal chemical composi- Classification of Population II stars 507 tion and stars with small to medium metal-deficiency, they are from Kuriliene & Sudzius (1974). Q-parameters were calculated by a pro- gram of Kazlauskas (1993).
5. RESULTS OF CLASSIFICATION
The classification methods described in Section 4 were applied to 848 program stars. The results of the classification are presented in Table Al (in the Appendix), in which the columns give the star name, photometric spectral type, intrinsic color index (F—F)o, color excess Ey-v» metallicity [Fe/H] and absolute magnitude My. In the last column the note codes are given: C is for notes concerning the classification (Table A2) and L is for notes from the literature on identification, membership in moving groups, visual and spectral binarity and variability (Table A3). Some remarks concerning the results of classification: (1) The spectral type, which was explained in more detail in Paper I, is estimated only from the photometric data. (2) In our spectral classification we identify some stars as be- longing to the RR Lyr, UU Her or RV Tau types. This does not mean that we assign the star to the corresponding type according to its variability. It just means that color indices and Q-parameters of the program star are close to those of the variable standard star. (3) Part of stars has the discrepant classification. In this case we present two alternative spectral types, the first being more reliable. The given astrophysical parameters correspond to the first spectral type.
6. DISCUSSION
6.1. Some general remarks
In this section, a longer discussion follows on certain groups of stars: high galactic latitude supergiants, field RHB stars, Popu- lation II visual binaries, metal-deficient subgiants, stars from the Catalogue of Metal-deficient F-M Stars Classified Photometrically (MDPH; Bartkevicius 1993) and stars included into one of the HIPPARCOS programs (Bartkevicius 1994a). Some of these stars are from the list of standard stars, others are the so-called program stars. Hereafter, we analyze these two groups of stars together. 508 A. Bartkevicius and R. Lazauskaite
In Figs. 1 and 2 we present the HR diagrams plotted using our classification of the standard and program stars, i.e. for all stars classified in Paper I and in this paper. The distribution of these stars by metallicity is shown in Fig. 3.
6.2. Comparison with previous results
We have made an analysis of the differences between the astro- physical parameters derived using the new calibrations and those estimated earlier in the Vilnius photometric system (Bartkevicius & Sperauskas 1983, Bartkevicius & Tautvaisiene 1987, Bartasiute 1989). The results of comparison are presented in Table 4. Table 4. Comparison of new and old astrophysical parameters. new values - old values
Source A(Y-V)0 A[Fe/H] A Mv Bartkevicius & -0.004±0.021 (274) +0.02±0.18 (275) +0.23±0.59 (256) Sperauskas (1983) Bartkevicius & -0.006±0.024 (67) +0.22±0.18 (62) +0.14±0.70 (69) Tautvaisiene (1987) Bartasiute (1989) -0.004±0.015 (217) +0.03±0.17 (192) +0.02±0.55 (224)
The most significant difference is found between the present metallicities and the values from Bartkevicius & Tautvaisiene (1987). The reason of such large difference is a correction of —0.23 dex which was introduced wrongfully in the latter paper. The new and old val- ues of (Y-V)o and My agree within the error bars.
6.3. High-galactic-latitude supergiants
F-type supergiants at high galactic latitudes were first detected by Bidelman (1951). Similar to Population II stars, these stars can be distinguished by their low metallicity, high space velocity or the location at high galactic latitudes. Hereafter we discuss UU Herculis- type stars, the supergiants located higher or lower than 400 pc from the galactic plane and the stars classified as supergiants by Bartaya (1979). Some of the Bartaya "supergiants" were classified photomet- rically by Bartkevicius et al. (1992) and found to be giants or main sequence stars. Here we reclassify all these stars by the method of comparison using a new set of standard stars described in Paper I and in Section 4 of the present paper. Classification of Population II stars 509
-10r ' All stars
B) 0 3
> 5
..«VJ 10
15 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4
(Y-V)0
Fig. 1. HR diagram for all standard and program stars classified in the Vilnius system.
-ior [Fe/H]<—0.5
-5
w 0 3 .g •«. -y**-'' « V'" •H C rH •H > 5 4
10
15 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 (Y-V)o Fig. 2. HR diagram for the standard and program stars classified in the Vilnius system. Only metal-deficient stars ([Fe/H]< -0.5) are pre- sented. 510 A. Bartkevicius and R. Lazauskaite
100
Fig. 3. Distribution of the standard and program stars by metallicity.
6.3.1. UU Herculis-type stars
The F-supergiants at high galactic latitudes, which show a low- amplitude variability, were attributed to the UU Herculis-type group by Sasselov (1983a, 1983b, 1984). Earlier these stars were studied by several authors (see in more detail Bartkevicius et al. 1992). The fact, that UU Herculis-type stars are located at high galactic latitudes and show the chemical composition of Population I, has caused durable discussions about their evolutionary stage. Sasselov (1984) has suggested three possible explanations: (1) UU Herculis- type stars are old and low-mass objects which just "mimic" luminous massive supergiants; (2) these stars originate in the galactic plane and only later reach high galactic latitudes; (3) these stars have been formed far from the galactic plane from the material enriched in metals. Later on, Luck et al. (1983) and Luck & Bond (1984) from a detailed spectroscopic analysis have estimated that some UU Herculis-type stars are moderately metal-deficient and suggested to consider these stars as being in the post-AGB stage. This interpreta- tion seems to be supported by the presence of large infrared excesses detected for some of them (Parthasarathy & Pottash 1986, Trams et al. 1991, Parthasarathy 1994). Now this view is generally accepted (see the discussion by van Winckel et al. 1996). However, the obser- vational results and their interpretation show that either the nature of UU Herculis-type stars is not finally understood, or this group is not uniform. For example, Zsoldos et al. (1993), analyzing the Classification of Population II stars 511 period of light variability of the UU Her itself, concluded that the prototype of the whole group is a normal F-supergiant of high mass (14 MQ). Waters et al. (1993) showed that 89 Her (HD 163506) can be interpreted as a binary system. They also noted that many of high latitude supergiants can be members of binary systems in which one component is in a late stage of evolution, but not necessarily in the post-AGB phase. The properties of UU Herculis-type stars were summarized by one of the authors (Bartkevicius 1992). He included into the "Cat- alogue of Population II A-F Supergiants: UU Herculis and Related Stars" those supergiants which satisfy one or more of the following criteria: (1) metal deficiency; (2) relatively high galactic latitudes; (3) high spatial velocities; (4) very specific variability with relatively small amplitudes and with two or three altering periods from about 20 to 120 days; (5) large infrared excesses due to circumstellar dust shells. On the basis of these criteria, 18 UU Herculis-type stars were iden- tified. Also, six stars were found as ambiguous stars of this group. Twelve of the UU Herculis-type stars have been observed in the Vilnius photometric system. The results of their photometric classi- fication are presented in Table 5. Among other stars observed in the Vilnius system we have found four stars suspected to belong to the UU Herculis type (Table 6). Sometimes the photometric classification of UU Herculis-type stars and suspected candidates is not definite. For some of such stars Table 7 gives an alternative classification. Most of the classified stars are moderately metal-deficient (-0.9 to -1.9 dex). Some stars show low reddening (0.02-0.07 mag), but most stars are moderately reddened (0.1-0.3 mag). The absolute magnitudes of UU Herculis-type stars are often conflicting. A disagreement between the absolute magnitudes de- rived from the strength of the OI 7774 triplet and those from pho- tometry is well known. In Table 8 we present our results for three UU Herculis-type stars, together with My derived from uvbyfl pho- tometry and from the 01 7774 line photometric index A(9), both taken from Arellano Ferro & Parrao (1990). The absolute magni- tudes from Vilnius photometry place UU Herculis-type stars closer to the galactic plane than My from uvbyfl photometry but farther than Mv from the 01 7774 line. Mendoza L Arellano Ferro (1993) 512 A. Bartkevicius and R. Lazauskaite
Table 5. Classification of UU Herculis-type stars.
No. Name Sp(Vilnius) (y-v)o EY-V [Fe/H] MV -s(pc) 1.* BD+14°3061 UU Her-F7 Ib 0.45 0.03 -1.9 -4.5 3350 2.* BD+38°2803 UU Her-(F2 Ib) 0.44 0.09 -1.2 -5.0 3422 3. BD+39°4926 UU Her-(A7 Ia) 0.24 0.09 -2.9 -5.0 -1718 4. BD—30°15602 UU Her? -A0 lab 0.24 0.11 -6.4 -4628 5. HD 34250 A6 II-III/UU Her-F3: 0.37 0.32 -1.5 -3.0 -42 6. HD 46703 UU Her-F0 Ib 0.44 0.08 -1.9 -4.0 1146 7. HD 137569 AOIb, UU Her? 0.20 0.00 -1.0 -5.5 2937 8.* HD 148743 UU Her-F3 Iab/A9 lab 0.35 0.09 -0.8 -6.8 1656 9. HD 161796 UU Her:, A9 lab 0.35 0.11 -0.3 -7.4 3123 10.* HD 163506 UU Her?, A9 Ia 0.35 0.06 -0.4 -7.5 1328 11.* HD 190390 UU Her-A9 Ib 0.46 0.11 -1.9 -4.5 -415 12. PU Vul UU Her?-A3 Ia 0.25 0.28 -0.5 -6.3 -815
Notes: I,8. Ambiguous or insufficiently analyzed UU Herculis-type stars as noted by Bartkevicius (1992). 2. Var: UU Her. The table gives the average astrophysical parameters and the average distance. 10. Var: V441 Her. II. VB?
Table 6. Classification of the suspected UU Herculis-type stars.
No. Name Sp(Vilnius) (Y-V)0 EY-V MV 2 (pc) 1. BD+42°4189 UU Her?-B9 II 0.19 0.18 -3.8 -453 2. HD 172594 UU Her-Fl Ia 0.35 0.40 -7.4 -198 3. HD 194951 UU Her?-F0 I 0.40 0.11 -3.4 -30 4. HD 215684A UU Her?-F5 Ib 0.36 0.02 -5.0 -314
Table 7. The alternative classification of UU Herculis-type and suspected stars.
No. Name Sp(Vilnius) (y-v)o EY-V Mv ¿(pc) 1. BD+14°3061 A5 Ib 0.18 0.30 -5.7 3443 2. BD+42°4189 B9 II 0.16 0.21 -3.7 -417 3. HD 148743 A9 lab 0.21 0.23 -7.0 1385 4. HD 194951 A9 II 0.27 0.24 -2.7 -16 5. HD 215684A Fl lab 0.29 0.09 -7.0 -688 Classification of Population II stars 513
Table 8. Comparison of My for UU Herculis-type stars derived by different methods.
Name Mv(uvbyß) Mv( A) Mv (Vilnius) BD+38°2803 (UU Her) -8.1 -0.4 -4.4* HD 161796 -9.0 -5.2 -6.4 HD 163506 (89 Her) -8.3 -3.9 -5.3
*the average value also find a difference between the absolute magnitudes from uvbyfi photometry and those from the 01 7774 line. They try to explain this difference either by an oxygen deficiency in the atmospheres of these stars or by an extended atmosphere.
6.3.2. Supergiants with \z\> 400 pc
We have looked through the list of stars classified by us in the Vilnius photometric system (Table Al) and isolated some super- giants with | z |> 400 pc (Table 9) which earlier were not classified as UU Herculis-type stars. For their exact identification, a detailed analysis of high dispersion spectra is required. In Fig. 4 we present the HR diagram for all supergiant stars classified here.
6.3.3. High-galactic-latitude supergiants from the Bartaya catalog
Sasselov (1984) has suggested that a large number of UU Herculis-type stars may be among the stars located at high galac- tic latitudes and classified by Bartaya (1979) as F-supergiants. To verify this suggestion, we have classified 26 F stars with |6|> 16°.5 and some other high luminosity stars from the Bartaya catalog. The same stars were classified earlier by Bartkevicius et al. (1992). For some stars, our classification (Table 10) is a little different from the previous one due to an other set of standards. In general, however, the same results were obtained. According to our classification, these stars are giants or even dwarfs. In attempting to explain the discrepancy between our and Bar- taya's classification, we tried to find for the stars from Table 10 their MK classification. However, the MK type for only one star was found. HD 152905 was classified by Sato &: Kuji (1990) from spectrograms of dispersion 73 A/mm at H7. They derived the spec- 514 A. Bartkevicius and R. Lazauskaitè
-10 + AGfi • o o * CH-RV 0 0 0 supergiant • UU Her -8 • • RV TAu 0 o © SRd CO - % -6 « •o 3 •S -4 .H o*o •H > o Ì "2 *+ ++o 0 t + 2
0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 1.6 (Y-V)o Fig. 4. HR diagram for all classified supergiant stars.
Table 9. Supergiants with \z\> 400 pc.
Name Sp(Vilnius) (Y-V)o Ey-v Mv z( pc) BD+8°4122 B3 la, (sdB) 0.16 0.27 -7.6 -1447 BD+20°3004 B6 II-III 0.11 0.03 -3.1 3767 BD+32°2188 Al II 0.19 0.00 -3.5 6846 HD 2207 F9 lb 0.51 0.10 -4.3 -448 HD 161695 A2 lb 0.18 0.03 -5.2 818 HD 204293 A3 lab 0.23 0.09 -5.8 -1393
trai class K0 III, while our photometric spectral type is MD-Ba-G9 III. Also, in Bartkevicius et al. (1992), Bartaya's classification of some other supergiants was compared with MK classifications for the same stars from Jaschek (1978). Only 5 stars from 27 Bartaya's G-K supergiants are of luminosity class I. The remaining stars are of other luminosity classes: 2 are of luminosity class II, 11 stars are of luminosity classes III or IV and 10 are of luminosity class V. Classification of Population II stars 515
Table 10. Results of classification of stars from Bartaya's catalog.
No. Name Sp(Vilnius) (Y-V)o EY-V [Fe/H] MV Sp (Bartaya) 1. BD+44°367 MD-A9 V, BS? 0.37 0.05 -0.1 0.8 F0 I 2. BD+44°2763 F2 III-IV 0.36 0.04 -0.1 1.8 F2 I 3. BD+45°2798 MD?-K0 III, Ba 0.81 0.00 -0.2 1.1 G8 I 4. BD+45°4352 MD?-K5 II-III 1.01 0.11 -0.3 0.3 K5 I 5. BD+46° 186 F9 IVpec/B9 IV+ 0.51 0.00 0.2 2.0 F0 I Gl II/F9 III-IV: 6. BD+46°2573 MD-K5 II-III 1.02 0.06 -0.4 0.1 K4 I 7. HD 9549 A9 IV 0.30 0.09 0.2 1.8 F0 I 8. HD 9861 MD-F3 IV 0.43 0.05 -0.4 3.1 F5 I 9. HD 46276 A7 III 0.33 0.06 2.1 F0 I 10. HD 46528 F0 IV 0.32 0.12 1.9 F5 I 11. HD 49709 F0 IV 0.34 0.07 -0.2 1.9 F2 I 12. HD 50103 MD-G8 III-IV, Ba? 0.72 0.03 -0.9 2.0 K0 I 13. HD 51832 F2 III-IV 0.36 0.08 0.1 1.6 F2 I 14. HD 56243 MD?-K5 III 1.04 0.00 -0.2 -0.1 K4 I 15. HD 58807 F3 IV-V 0.41 0.00 -0.1 3.1: F3 I 16. HD 58965 MD-F5 V 0.45 0.00 -0.2 3.2 F5 I 17. HD 58966 F5 V 0.43 0.00 -0.1 3.3 F5 I 18. HD 73759 F2 III 0.36 0.07 0.0 1.5 F3 I 19. HD 74132 F3 IV-V 0.40 0.00 -0.1 3.3 F5 I 20. HD 74327 Fl IV, RHB? 0.40 0.00 0.0 1.9 F3 I 21. HD 75555 F5:III-IV, RHB 0.44 0.00 -0.1 1.2 F5 I 22. HD 84800 A Boo?-A3 V 0.21 0.00 1.3 A2 II 23. HD 85015 MD-F3 V, BS? 0.41 0.00 -0.5 3.0 F3 III 24. HD 99829 F5 V 0.41 0.00 -0.1 3.4 F5 I 25. HD 102102 A7 IV 0.25 0.06 0.0 2.2 F0 I 26. HD 102570 F3 IV-V 0.39 0.00 -0.1 3.4 F2 I 27. HD 141021 MD?-F3 IV-V 0.42 0.05 -0.2 2.9 F5 I 28. HD 142438 MD-Ba-G5 III 0.71 0.01 -0.2 -0.3 G5 I 29. HD 152905 MD-Ba-G9 III 0.76 0.01 -0.2 0.7 K0 Ib 30. HD 162036 F2 III-IV 0.37 0.04 -0.1 1.4 F2 I 31. HD 173666 Fl III 0.35 0.07 -0.2 1.6 F2 I 32. HD 183098 K0 III 0.79 0.00 -0.2 1.1 Kl I 33. HD 183968 K3 III 0.89 0.00 -0.0 0.7 K3 I 34. HD 185732 F3 III, MD? 0.39 0.04 -0.1 F0 I 35. HD 186253 MD-F0 IV 0.37 0.04 -0.5 1.9 F0 I 36. HD 194130 MD-F3 IV 0.43 0.03 -0.3 3.1 F3 I 37. HD 222717 MD-F2 IV 0.41 0.00 -0.3 2.9 F0 I 38. HD 223153 MD-K2 III 0.86 0.05 -0.3 0.7 Kl I 39. HD 224507 K3 III 0.85 0.07 0.1 1.0 K2 I 516 A. Bartkevicius and R. Lazauskaite
It seems likely that the dispersion used by Bartaya (166 A/mm at H7) is too low to recognize supergiant stars reliably. A similar conclusion was made by Arellano Ferro et al. (1989). They classi- fied Bartaya's stars in the Stromgren system and found that their gravities are much higher than those expected for supergiants. How- ever, the absolute magnitudes from 01 7774 A line photometry are more negative than those from uvby/3 photometry. They consider the reason for this discrepancy can be the abnormal strength of the 01 7774 A absorption due to extended atmosphere or to contamina- tion of this line by other nearby lines.
6.4. Field RHB stars
Red horizontal-branch (RHB) stars are well known in globular clusters. It seems likely that these stars should be present also in the galactic field where halo stars having the same age and metal- licity range as globular clusters are located. However, until now the presence of RHB stars in the galactic field is a matter of discussion. The investigations of RHB stars in various photometric sys- tems recently were reviewed by Tautvaisiene (1996b). In the Vil- nius photometric system these stars were investigated by Straizys et al. (1981) and Tautvaisiene (1996a). In the first of these papers, eight stars were suspected as belonging to the red horizontal branch. In the second paper, 13 red horizontal-branch stars from the Rose (1985) list were investigated. However Norris (1987), using the ob- servations in the DDO and BV systems, showed that Rose's RHB candidates have characteristics of the clump stars in the old open cluster NGC 2243 and of metal-poor giants. So, the identification of field RHB stars still remains a problem. We tried to identify and classify the field RHB stars in the Vil- nius photometric system using the method of comparison of their color indices and Q-parameters with those of the standard stars. The identified RHB stars were selected from the general list of stars under investigation (Table Al). According to spectral type and astrophysi- cal parameters and bearing in mind their reliability, these stars were subdivided into RHB stars (Table 11) and probable RHB stars (Ta- ble 12). This subdivision only means that stars from the first group are photometrically more similar to RHB stars than stars from the second group. All eight stars identified by Straizys et al. (1981) were con- firmed by our classification as RHB stars. However, in the list pre- Classification of Population II stars 517
Table 11. Results of classification of RHB stars in the Vilnius photometric system.
No. Name Sp(Vilnius) (B-V)o (V-V)o Ey-v [Fe/H] Mv 1. BD+09°2860 RHB:-G2 0.68* 0.61 0.00 -1.5 -0.0 2. BD+25°2502 RHB-G5 0.79* 0.65 0.01 -0.7 0.8 3. BD+31°1588 RHB-G2 III 0.80* 0.66 0.07 -0.7 0.7 4. BD+65°111 RHB-G0 III 0.71* 0.60 0.28 -0.6 0.9 5. BD+76°524 RHB-Gl 0.65* 0.58 0.00 -1.2 0.5 6. BD—03°5215 RHB-Gl 0.65* 0.59 0.00 -1.4 0.4 7. HD 3179 RHB-G5 0.67* 0.60 0.00 -1.5 0.7 8. HD 6229 RHB-G5 0.69 0.61 0.04 -1.4 0.6 9. HD 6461 RHB-G3 0.76 0.66 0.00 -0.6 0.7 10. HD 6903 RHB-G3 0.69 0.62 0.00 -0.8 0.9 11. HD 13359 RHB-G4 0.69 0.59 0.06 -1.5 0.3 12. HD 21581 MDGE-G5, RHB? 0.73 0.64 0.07 -1.8 0.2 13. HD 25532 RHB-G0 0.61 0.57 0.08 -1.4 0.8 14. HD 44517 RHB-G1:/F7 IV 0.54 0.51 0.00 -1.3 0.8 15. HD 79452 MD-G5 III, RHB? 0.84 0.67 0.02 -0.6 0.7 16. HD 88923 RHB-F3 0.41* 0.43 0.00 -1.2 0.7 17. HD 104783 RHB-G3 0.78 0.66 0.02 -0.6 0.5 18. HD 105546 RHB-G3 0.67* 0.60 0.02 -1.5 0.3 19. HD 119516 RHB-F9 0.55* 0.54 0.01 -1.9: 0.7 20. HD 145293 RHB/RR-F3 0.47 0.48 0.15 -1.1 0.8 21. HD 166161 RHB-G0 0.73 0.62 0.20 -1.5 0.5 22. HD 167768 RHB?-G7 0.83 0.69 0.02 -0.4 1.3 23. HD 173920 RHB-G6 0.80 0.67 0.00 -0.4 0.9 24. HD 176203 RHB-GO 0.62 0.59 0.09 -1.3 0.7 25. HD 177249 G7 III 0.84 0.68 0.00 -0.2 0.8 26. HD 183418 MD-G7 III, RHB 0.88 0.71 0.05 -0.2 1.1 27. HD 184266 RHB-F8 0.53 0.53 0.05 -1.6 0.7 28. HD 191814 RHB-G7 III 0.86 0.68 0.03 -0.4 1.1 29. HD 195636 MDGE-G0, RHB 0.54 0.55 0.06 -2.1 0.0 30. HD 199854 RR-F5: 0.36 0.44 0.05 -1.4 0.8 31. HD 202573 RHB:-G7 0.87 0.68 0.03 -0.4 1.1 32. HD 208110 RHB-G3 0.80 0.65 0.04 -1.2 1.1 33. HD 213487- RHB-G3 0.79 0.65 0.07 -0.8 0.7 34. HD 214362 RHB-Gl 0.50 0.53 0.00 -2.6: 0.5 35. HD 223460 RHB-G3 III 0.73 0.65 0.05 -0.7 0.8 36. HD 224342 RHB-G5 0.62 0.55 0.10 -0.9 0.6 37. HDE 229274 RHB-GO 0.56 0.57 0.03 -1.5 0.5 38. SA 57-33** RHB-G2: 0.71* 0.63 0.11 -1.5 0.6
* (B-V)0 is calculated from (Y-V)0. ** Number from Becker W. & Fenkart R. 1976, Photometric Catalogue for Stars in Selected Areas and other Fields in the RGU system. Part I, Basle. 518 A. Bartkevicius and R. Lazauskaite
Table 12. Results of classification of probable RHB stars in the Vilnius photometric system.
No. BD/HD Sp(Vilnius) (s-v)o(y-v)o Ey-v [Fe/H] Mv 1. BD+04°4557 MD-G5 III, RHB? 0.80* 0.65 0.08 -0.3 0.9 2. BD+10°6 MDGE-G5, RHB 0.76* 0.66 0.07 -1.5 -0.1 3. BD+11°2998 HB-GO pec 0.54* 0.51 0.11 -1.2: 1.8: 4. BD+17°3248 MDGE-G1 0.54 0.54 0.12 -1.8 0.5 5. BD+18°2890 MDGE-G3 0.67* 0.61 0.06 -1.6 0.3 6. BD+25°2497 RHB7-G7 III 0.84 0.67 0.05 -0.4 1.1 7. BD+27°2057 RHB-G7 III/G3II 0.82 0.68 0.07 -0.4 1.0 8. BD+29°2231 MD7-G6 III,RHB? 0.90 0.68 0.00 -0.1 1.0 9. BD+29°2321 MD-G6 III, RHB 0.84* 0.67 0.05 -0.3 1.0 10. BD—10°548 RHB-G5 0.77 0.63 0.02 -1.6 0.1 11. BD—15°560 A Boo-Fl: 0.33 0.41 0.04 -0.6 0.8 12. BD—20°170 RHB.-G5 0.71* 0.62 0.04 -1.3 0.8 13. CD—23°72 RHB-G3 0.69* 0.61 0.00 -1.4 0.5 14. HD 97 RHB:-G3, MDS6? 0.74* 0.65 0.04 -1.6 0.5 15. HD 21018AB RHB:-G6 0.81 0.68 0.03 -0.4 0.6 16. HD 47147 RR Lyr-F7/B8 II 0.39 0.48 0.01 -1.8 0.7 17. HD 81192 MD-G8 III, RHB? 0.91 0.71 0.04 -0.5 0.6 18. HD 111812 RHB-G3:/G1 III-IV 0.58 0.61 0.01: -1.1: 0.8 19. HD 121135 MDGE-G5 0.75* 0.66 0.00 -1.7:: -0.2 20. HD 185737 MD-G7 III, RHB 0.85* 0.68 0.03 -0.3 1.0
21. HD 210585 MDGE-G5 0.76* 0.67 0.04 -1.9 -0.3 22. HD 214714A RHB:-G5 0.76 0.66 0.06 -0.8 0.9 23. CI Stock 7 144** RHB-G2 III/G1(III) 0.77* 0.64 0.11 -0.7 0.8 24. [J 92] 24*** RHB-G3 III/F9(III-IV) 0.75* 0.62 0.06 -0.5 1.0
* (B-V)o is calculated from (Y-K)0. ** Number from Sanders W.L. 1973, A&AS, 9, 221 (open cluster NGC 6913). *** Number from Janulis R. 1992, Baltic Astronomy, 1, 25 (M 15 area). sented by Tautvaisiene (1996a) we find only three RHB stars (HD 104783, HD 79452 and BD+25°2502) and three stars are probable RHB stars (BD+25°2497, BD+27°2057 and BD+29°2231). Most of other stars are classified as giants with small metal deficiency (Ta- ble 13). This difference between the two classifications can be due to different values of estimated reddening. Tautvaisiene (1996a) con- siders the reddening to be zero. Although these stars are located in Classification of Population II stars 519
the direction of the North Galactic Pole, we derive the mean value of Ey-v ~ 0.04 mag. A possibility of such reddening in the direc- tion of NGP is recently confirmed by Knude (1996). Due to different reddenings accepted, our intrinsic color indices are also somewhat different from those of Tautavaisiene (1996a). As a consequence of larger reddening, our [Fe/H] are a little more positive than those derived by Tautvaisiene. However, the absolute magnitudes of these stars in both investigations are quite similar, with the mean value around +1.2 mag.
Table 13. Stars from the Tautvaisiene (1996a) list, which in the present work were classified as non-RHB stars.
No. Name Sp(Vilnius) (Y-V)0 Ey-V [Fe/H] Mv
1. BD+25°2436 G8 IV, MD? 0.69 0.01 -0.2 2.7 2. BD+25°2459 G9 III 0.70 0.03 0.0 -0.3 3. BD+26°2387 MD-G7 III 0.69 0.01 -0.5 1.0 4. BD+29° 2294 MD-G5 III 0.65 0.04 -0.4 1.1 5. BD+29° 2321 MD-G6 III, RHB 0.67 0.05 -0.3 1.0 6. BD+33° 2280 MD-G8 III-IV 0.68 0.00 -0.3 1.4 7. BD+34° 2371 MD-G6 III-IV 0.70 0.04 -0.3 1.6 8. BD+36° 2303 MD-Ba?-G7 III 0.71 0.08 -0.5 0.7 9. HD 105944 MD7-G5 III 0.64 0.06 -0.1 1.5
The HR diagram for RHB and probable RHB stars is plotted in Fig. 5. The accuracy of the My from Vilnius photometry is not better than ±1.0 mag. The distribution of these stars by [Fe/H] is given in Fig. 6. For the same stars we have also plotted their distribution by (B — V)o (Fig. 7), color indices B — V being taken from Mermilliod & Mermilliod (1994). When no UB V photometry was available, the (B—V)o was calculated from (Y—V)o by the relations between these color indices derived for giants by Bartkevicius & Lazauskaite (1992). The interval of (B — V)o for the field RHB stars is similar to that for globular cluster RHB stars (Straizys et al. 1981, Straizys 1982). For the extreme metal-deficient RHB stars (B—V)o are between 0.4 and 0.6, as in the globular clusters M 3 and M 15. The red limit for the stars with metallicity between -1.0 and -1.5 extends to 0.7-0.8, as in 47 Tuc and M71. For the stars with mild metal deficiency ([Fe/H]> —1), (B—V)o reaches 0.9-1.0, where the horizontal branch merges with the red giant clump observed in open clusters. 520 A. Bartkevicius and R. Lazauskaite
-1.0 • RHB O RHB prob. O ~ 0.0 • O
2.0 0.4 0.6 0.8 (Y-V) o
Fig. 5. HR diagram of RHB stars and probable RHB stars.
Fig. 6. Distribution of RHB and probable RHB stars by metallicity.
The two-color diagram (U—P)o, (Y—V)o for RHB and probable RHB stars is presented in Fig. 8. The (X—Y)o, (Y—V)o diagram used by Tautvaisiene (1996a) for the separation of RHB staxs from stars of other types is shown in Fig. 9. It can be noticed, that the last diagram shows a smaller difference between locations of stars of various types than the previous diagram. Thus, the (U—P)q, (Y—V)o diagram, as well as any other diagram in the form of "luminosity-sensitive color Classification of Population II stars 521
1 [Fe/H]>-0.5
1i i -0 . 5>- [Fe/H>--1.C
1 Ii -0.1>[Fe/H]> --0 . 5
1. 1( '1 1i [Fe/H]<-1.5
1 1 i 0.2 0.4 0.6 0.8 1.0
Fig. 7. Distribution for RHB and probable RHB stars by the intrinsic color index (B-V)q.
index vs temperature sensitive color index", e.g. (U-P)0, (F-S')o used by Straizys et al. (1981), are more useful for identification of RHB stars.
6.5. Population II visual binaries
Visual binaries are astrophysically important objects since they allow to test theories of stellar evolution and their fraction among the single stars contains information on the conditions of star formation. Binaries are also used to investigate the accuracy of calibrations of photometric systems. The visual binaries described in this section were selected from our general list of the standard and the Population II program stars. 522 A. Bartkevicius and R. Lazauskaitè
0.3
0.4
0.6
On Lix-i ...- # • • ^ og** 0A D 0.7 X • O A
o8ooAOo°o, 0.8 °o°o 8 • RHB * RHB probable 0.9 + G A MDG O MDGE 1.0 0. 0.5 0.6 0.7 0.8
(Y-V)0
Fig. 8. The (U-P)0, (y~V)o diagram for RHB stars. The location of giants of normal chemical composition (G) and metal-deficient giants (MDG, MDGE) is shown together with the mean sequences of normal supergiants, giants and dwarfs.
Fig. 9. The (X-Y)0, ( Y-V)Q diagram for RHB stars. Symbols are the same as in Fig. 8. Classification of Population II stars 523
Only the stars with the components measured as separate stars were included. The classification of binaries in the Vilnius system is pre- sented in Table 14 which contains the following results: spectral type, intrinsic color index (V —V)o, color excess Ey-v, metallicity [Fe/H], absolute magnitude My and distance to the star with its standard deviation. Although we tried to include into the observing program only Population II visual binaries, the classification shows that some binaries are stars of solar metallicity. The absolute magnitudes determined by various methods were averaged with equal weights. Bearing in mind the results of com- parison of our My with other sources (Bartkevicius &; Lazauskaite 1996, Vansevicius & Bridzius 1994), the following standard errors for individual My were adopted when calculating the standard deviation of the mean absolute magnitude of each component: (1) For My of dwarfs and subdwarfs determined by the empirical relations (1) and (2) of Paper I, a — ±0.5. (2) For My of giants determined by the empirical relations (4) and (5) of Paper I, a = ±0.6. (The comparisons with various sources give an error similar to that for dwarfs and subdwarfs. However, absolute magnitudes of the standard giants are less accurate than those of dwarfs and subdwarfs.) (3) For My for all types of stars derived using the methods of comparison of intrinsic color indices and Q-parameters, a — ±0.8. (4) For My for the stars of solar chemical composition, derived using the CLASS program (Vansevicius h Bridzius 1994), o = ±0.8. The distances to the stars were calculated using the usual equa- tion:
. , V - My + 5 - RY-V • EY-V log d= (1) where V is the magnitude of Vilnius system and My is the mean absolute magnitude given in Table 14. The ratio RY-V =4.15 (Kaz- lauskas 1996) was used. The standard deviation of the distance was calculated by the equation:
Based on the analysis of accuracy of the observations and on comparison of our astrophysical parameters with those from other sources, the following typical values of errors were used: ay = 0.02 mag, CTEY-V — 0-02 mag and OMv calculated as described above. 524 A. Bartkevicius and R. Lazauskaite Table 14. Results of classification of visual binaries in the Vilnius system. No. Name Sp(Vilnius) (Y-V)o Ey-v [Fe/H] Mv d± We have made an attempt to evaluate the physical or optical nature of the visual binaries. A strong argument for the physical reality of a system is the parallel motion of the components. For this we have compiled from literature the proper motions and radial velocities for the components of binaries investigated (Table 15). The proper motions were taken mainly from the PPM catalog (Roser & Bastian 1991, Bastian & Roser 1993). PMA and SPMA are proper motion in right ascention with its standard error while PMD and SPMD are proper motion in declination and its standard error. PMA is given in milliseconds per year, other quantities in milliarcseconds per year. Proper motions, not found in the PPM, were taken from the NLTT catalog (Luyten 1979). In that case the total proper motion in arcseconds per year is given. The radial velocities, given in km/s, are taken from various lit- erature sources, most of which are listed in the Bibliographic Cata- logue of Stellar Radial Velocities (Barbier-Brossat et al. 1994). The first evaluation of nature of binaries was made solely on the basis of proper motions and radial velocities. The stars with similar proper motions and radial velocities are the physical pairs and are marked by PH! in the last column of Table 15. The stars which have no radial velocity measurements but show common proper motion are physical binaries with large probability, and they are marked by PH. There are a few stars which have similar but not identical proper motion, and they are considered the probable physical pairs (PH?). The stars with clearly different proper motions are identified as the optical binaries (OPT). The astrophysical parameters derived from photometry add in- formation on the nature of binaries. The metallicities and distances of the binary components divided into groups as described above are compared in Fig. 10. It is expected that the physical binaries must be located approximately at the same distance and have the nearly identical metallicities. However, not all stars confirm this prediction. For example, components of the 11th pair have quite different metal- licities and distances although their motions are parallel. The reason of such disagreement may be in the errors of their photometric clas- sification. One component, BD+31°3025, can be a subgiant which is usually classified with larger uncertainty. If the absolute magnitude of this star would be less by 1 mag, both stars would be located at the same distance. An unresolved close component can also be the reason of wrong classification. 526 A. Bartkevicius and R. Lazauskaite Table 15. Proper motions and radial velocities for the visual binaries. No. Name PMA SPMA PMD SPMD RV Nature 1. HD 919 8.4 4.1 -16 4.5 OPT HD 947 -1.1 2.0 -14 2.2 2. LTT 575 0.276° PH LTT 576 0.276° 3. BD+52°913A 0.106 G 191-B2B 0.088c +22(1) 4. HD 55195A -0.3 3.1 -5 3.2 HD 55195B 5. HD 73394A +4.3 2.2 -90 2.1 HD 73394B HD 73394C 6. HD 73710 -2.8 1.9 -13 2.0 +34.51(2) PH HD 73709 -2.9 3.4 -13 3.4 7. HD 104513 -29.6 4.6 68 4.8 +2.1(3) OPT HD 104425 +5.8 4.2 -24 4.2 8. HD 112413 -19.9 0.4 57 0.5 -1.9(4) PH! HD 112412 -18.3 2.1 44 2.1 -1.9(5) 9. BD+36°2481 10.8 7.0 -30 6.0 BD+36°2482 0.2 8.7 -10 7.1 PH? BD+36°2483 0.4 10.3 -19 10.0 BD+36°2484 10. HD 134439 -70.2 2.9 -3547 3.0 +310.6(6) PH! HD 134440 -70.2 9.9 -3567 9.9 +311.5(6) 11. HD 158226 -28.6 2.4 64 2.4 -73.4(6) PH! BD+31°3025 -29.2 5.9 69 5.7 -73.4(6) 12. HD 172167 17.3 0.3 286 0.3 -12.1(7) OPT BD+38°3231 13.6 4.5 254 4.4 13. G 184-48 0.578° +32.22(8) PH! G 184-49 0.578° +31.90(8) 14. HD 184700 -5.7 2.0 -331 2.0 -19.4(9) OPT HD 184768 -1.1 2.1 -390 2.1 -17.7(9) 15. HD 185657A 3.3 2.9 141 2.9 -92.0(7) HD 185657B HD 185657C HD 185657D 16. HD 190211A -0.1 4.3 -17 4.4 HD 190211B 17. BD+40°4197A +0.3 4.0 +19 4.0 OPT BD+40°4197B -1.2 4.6 -17 4.6 18. HD 196882A +1.4 3.6 3 3.7 HD 196882B 19. HD 219175 +38.0 2.2 -35 2.3 -30.1(11) PH BD-09°6150 +38.5 2.2 -34 2.3 20. HD 219834A 0.305° +13.1(7) PH HD 219834B 0.305° Classification of Population II stars 527 a Total proper motion is given in arcsec per year from NLTT (Luyten 1979) ' Total proper motion is given in arcsec per year from Giclas H. L., Burnham R. Jr., Thomas N. G. 1966, Lowell Obs. Bull., No. 132 c Total proper motion is given in arcsec per year from Routly P. M. 1972, Pub. U. S. Naval Obs., Second Series, 20, Part 6, 1 References of radial velocities given in Table 18: (1) Reid N., Wegner G. 1988, ApJ, 335,953 (2) Mermilliod J.-C., Mayor M. 1989, A&A, 219, 125 (3) Abt H. A., Levy S. G. 1985, ApJS, 59, 229 (4) Abt H. A., Snowden M. S. 1973, ApJS, 25, 137 (5) Strassmeier K. G., Fekel F.C. 1990, A&A, 230, 389 (6) Carney B. W., Latham D.W., Laird J. B., Aguilar L. A. 1994, AJ, 107, 2240 (7) Beavers W. J., Eittler J.J. 1986, ApJS, 62, 147 (8) Marcy G. W., Lindsay V., Wilson K. 1987, PASP, 99, 490 (9) Fouts G., Sandage A. 1986, AJ, 91, 1189 (10) Abt H. A., Willmarth D. W. 1987, ApJ, 318, 786 Another example is the 17th pair with components of similar metallicities but located at different distances and forming an optical pair, according to their velocities. Similar metallicities do not always mean the physical nature of the system, especially for binaries of solar composition. The presented examples show that physical and optical binaries cannot be distinguished only by their photometric astrophysical parameters. Further we present comments on the nature of individual bina- ries. Attributing the stars to physical or optical binaries, we take into consideration their proper motions and radial velocities, as well as their astrophysical parameters derived from Vilnius photometry; the priority is given to astrometric data. When the proper motions of both components are not known, we name the pair as probable optical or probable physical binary depending on the agreement of distances and metallicities of the components. 1. HD 919 and HD 947 are at the same distance within the errors. However, HD 919 is a M-type star and its classification is uncertain. Proper motions show that stars form an optical pair. 2. LTT 575 and LTT 576. The common proper motion suggests that the pair is a physical binary. The distance difference is < 2ad- 3. The difference of distances of BD+52°913A and G 191-B2B is < 2<7d. However, G 191-B2B probably is a hot subdwarf, and its My can be uncertain. The nature of this binary is indefinite. 528 A. Bartkevicius and R. Lazauskaite Fig. 10. Comparison of metallicities (a) and distances (b) of binary star components. The errors of 0.2 dex in metallicity were assumed for all stars. 4. The classification of HD 55195A and HD 55195B is suffi- ciently accurate. The stars are located at quite different distances and probably form an optical pair. 5. The different distances and metallicities of HD 73394A and of the pair contained HD 73394B and HD 73394C suggest that A and B+C is an optical system. However, HD 73394B and HD 73394C can be physically related. 6. Common proper motion, nearly identical metallicities and distances argue for the physical connection between HD 73710 and HD 73709. 7. HD 104513 and HD 104425 is an optical pair, as is indicated by different proper motions. 8. HD 112413 and HD 112412 have coinciding radial velocities and are located at the same distance but their proper motions are slightly different. The pair is physical. 9. Similar proper motions, metallicities and distances indicate that BD+36°2482 and BD+36°2483 is a physical pair. Other com- ponents are optical. 10. The common proper motion shows that it is a physical pair. Metallicities and distances of the components agree very well. Classification of Population II stars 529 11. HD 158226 and BD+31°3025 form a physical pair as is indi- cated by similar proper motions and radial velocities. Their metallic- ities and distances are a little different probably due to classification errors of BD+31°3025. This star can be a subgiant. If the absolute brightness of BD+31°3025 would be fainter by 1 mag, both compo- nents were located at the same distance. 12. Proper motions and distances are quite different: the pair is optical. 13. Proper motions, radial velocities and distances agree very well: the pair is physical. 14. Although radial velocities are similar, proper motions and distances of the components are different: we assume this binary to be an optical pair. 15. HD 185657A and HD 185657C have nearly equal metallicities and distances and probably form a physical pair. Other components are optical. 16. HD 190211A and HD 190211B are located at different dis- tances. Metallicities of the components are nearly the same. Since the classification of the component B is uncertain, the nature of this pair is indefinite. 17. Different proper motions and distances indicate that the pair is optical. 18. HD 196882A and HD 196882B are located at quite different distances. We assume this binary to be an optical pair. 19. The stars form a physical pair, as is indicated by their com- mon proper motion, nearly identical distances and metallicities. 20. Common proper motion and close distances indicate the physical nature of this pair. Consequently, we have found nine physical and five optical pairs. In many cases, but not always, photometric distances and metallici- ties of components of the physical pairs agree quite well. Two stars are assigned to the probable physical pairs and two stars are con- sidered to be the probable optical pairs. The nature of two pairs remains indefinite. 6.6. Metal-deficient subgiants Metal deficient subgiants were identified by photometric (see e.g. Carney et al. 1994; Schuster & Nissen 1989b; Nissen & Schuster 1991; Schuster et al. 1996) and spectroscopic (Tomkin et al. 1992, Axer et al. 1994, 1995, Fuhrman et al. 1995, Pilachowski et al. 1993, 530 A. Bartkevicius and R. Lazauskaite 1996, etc.) methods. However, up to now the number of metal defi- cient subgiants identified among field staxs is quite small. Frequently, they are photometrically indistinguishable from subdwarfs. For ex- ample, Axer et al. (1994) found that ~ 1/2 of subdwarfs in their spectroscopically investigated sample are subgiants. Such misclas- sification introduces errors to distances, kinematic parameters and ages of stars. We recognize metal-deficient subgiants among other stars stu- died by using the method of comparison of color indices and Q- parameters with those of standard stars and taking into account their position in the HR diagram. The results of classification of metal-deficient subgiants are presented in Table 16. 6.7. Stars from the Catalog of Metal-Deficient F-M Stars (MDPH) The Catalogue of Metal-deficient F-M Stars Classified Photo- metrically (MDPH), compiled by Bartkevicius (1993), contains about 4400 suspected metal-deficient stars. As was emphasized in the de- scription of the MDPH catalog, the photometrically selected stars should be considered just as stars suspected in metal-deficiency, es- pecially if the stars were selected on the basis of UBV photometry. We have classified 471 stars from this catalog. Figs. 11 and 12 show the HR diagrams for the metal-deficient MDPH stars and the MDPH stars of solar chemical composition, respectively. Distribu- tion of the MDPH stars by metallicity (Fig. 13) is quite unexpected. A large fraction of these stars, about 25%, have [Fe/H]=0.0±0.2, i.e. the solar chemical composition. The majority of other stars are only mildly metal-deficient. Such result can be explained as follows: (1) Although the main criterium for including the stars into the catalog was [Fe/H]< —0.4, some stars brighter than 6th mag with —0.4 < [Fe/H]< —0.2, having kinematic parameters of Population II, were also included. (2) When compiling the catalog, zero reddening was adopted in many cases, but, as it is shown in Fig. 14 , the real reddening is larger. In the Vilnius photometric system, for example, underestimation of Ey-v by 0.01 mag gives the metallicity too negative by 0.1 dex. (3) A part of stars are binaries (see Table A2) or show various peculiarities in their spectra. (4) It is possible that some stars of MDPH have uncertain pho- tometry or they are misidentified. Classification of Population II stars 531 Table 16. Metal deficient subgiants classified in the Vilnius system. No. Name Sp(Vilnius) (Y-V) o Ey-V [Fe/H] Mv 1. BD+1°4042 MDSG(sd):-G5 pec 0.60 0.20 -0.9 5.5 2. BD+30°2027 MDSG-G7 0.62 0.05 -0.5 3.7 3. BD--8°3901 MDSG:-G2 0.68 0.10 -1.2 1.5 4. BD--12°81 MDSG-G7: 0.65 0.01 -0.8 1.0 5. HD 4906 MDSG:-G5 0.61 0.05 -0.8 3.7 6. HD 5916 MD-G7 IV pec 0.73 0.00 -0.4 3.2 7. HD 6286 MDSG-G8 0.74 0.06 -0.7 3.0 8. HD 6755 MDSGE-G3 0.56 0.09 -1.9 3.2 9. HD 30229 MDSGE-G3 0.60 0.06 -2.3 2.2 10. HD 31362 MD-F3 IV 0.40 0.00 -0.5 2.9 11. HD 38094 MD7-G6 III-IV 0.67 0.04 -0.3 2.1 12. HD 92787 MD-Fl IV-V 0.37 0.00 -0.4 1.8 13. HD 105791 MDSGE:-G1: 0.56 0.00 -1.9 0.6 14. HD 111721 MDSGE-G3 0.65 0.01 -1.6 2.1 15. HD 112887 MDSG-F2 0.44 0.01 -0.5 2.9 16. HD 126991 MDSG-G5/G3 V 0.65 0.02 -1.1 2.7 17. HD 128279 MDSGE:-G0:pec 0.60 0.00 -2.3 5.5 18. HD 131509 MD-G9 IV 0.68 0.02 -0.4 2.8 19. HD 134475 MD-F5 IV-V 0.44 0.01 -0.5 2.8 20. HD 150875 MD-F2 IV 0.44 0.13 -0.3 2.7 21. HD 168092 MD-Fl IV-V 0.39 0.00 -0.4 1.9 22. HD 170737 MDSG-G5 0.61 0.06 -0.9 3.9 23. HD 170899 MDSG:-G5:/B7 III+G7 Ib 0.74 0.10 -1.0 2.7 24. HD 175305 MDSGE-G3 pec 0.59 0.07 -1.7 2.7 25. HD 181007 MDSG:-G2 0.56 0.14 -1.2 3.7 26. HD 186253 MD-F0 IV 0.37 0.04 -0.5 1.9 27. HD 194130 MD-F3 IV 0.43 0.03 -0.3 3.1 28. HD 194378 MD-Fl IV-V 0.41 0.04 -0.3 2.4 29. HD 219715 MDSGE:G3 pec, sd? 0.58 0.06 -1.1 4.9 30. HD 219877 MD-F3 IV 0.42 0.00 -0.3 3.0 31. HD 222717 MD-F2 IV 0.41 0.00 -0.3 2.9 32. HD 224085 MD-K0 IV: 0.78 0.01 -0.8 33. HD 224844 MDSG?-G8 0.67 0.04 -0.5 2.8 34. LTT 397 (MDSG)-G8:/G4 III: 0.73 0.00 -0.7 2.9 35. [C93] 81* MDSGE-G3, sd? 0.59 0.41 -0.9 4.7 36. [J84] 33** MDSGE-G3 0.66 0.12 -1.5 2.2 * Number from Cernis K., 1993, Baltic Astron., 2, 214 (IC 348, Per OB2 area) ** Number from Janulis R. 1984, Bull. Vilnius Obs., No. 67, 18 (M71 area). 532 A. Bartkevicius and R. Lazauskaite -10 MDPH stars [Fe/H]<=-0.5 -5 « 0 : f 3 •H C rH •H > 5 sf 10 15 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 (Y-V)o Fig. 11. HR diagram for metal-deficient MDPH stars. -10 MDPH stars [Fe/H]>-0.5 m 3 •rH C 2. 5 10 Fig. 12. HR diagram for MDPH stars of normal chemical composi- tion. Classification of Population II stars 533 150 "IBin size - 0.2 dex N 100 50 0 2.5 -2.0 -1.5 -1.0 -0.5 0.0 0.5 [Fe/H] Fig. 13. Distribution of stars from the MDPH catalog by metallicity estimated in the Vilnius photometric system. 100 N [—1 —1 —1 —1 "Tl-n .1.1 n-m . . . _ 0.0 0.05 0.10 0.15 0.20 0. Ey-V Fig. 14. Distribution of stars from the MDPH catalog by reddening. Only stars with [Fe/H]>-0.4 are shown. For the stars with doubtful metallicity, a detailed examination of the literature is necessary. 6.8. Field metal-deficient F-M stars from the HIPPARCOS program The astrometric satellite HIPPARCOS of the European Space Agency was launched on August 8, 1989. During its 37-month mis- sion, the fundamental astrometric parameters for nearly 118 200 pre- selected stars (Turon et al. 1992) have been derived. The accuracy 534 A. Bartkevicius and R. Lazauskaite in parallax is from 1 mas (milliarcsec) for stars of 6th mag to 3 mas for stars of 12th mag (Arenou et al. 1995). The accuracy in proper motions is 1.5 mas yr_1 In 1982 one of us (Bartkevicius 1994a) proposed for HIPPARCOS a program of 455 metal-deficient F-M stars, from which 447 stars have been measured. 247 program stars were measured in the Vilnius photometric system. These stars were classified using the methods and scheme described in Paper I. Using these results and Eq. (1), the distances to the stars and photometric parallaxes (7r(ph) = 2) were calculated. The distribution of photometric parallaxes 7r(ph) is presented in Fig. 15. According to Arenou et al. (1995), the standard error of the HIPPARCOS parallaxes for stars of 9th mag (composing most of the stars discussed here) is 1.5 mas. It gives an accuracy better than 10 % for stars within 67 pc and better than 20 % for stars within 133 pc. The relative parallax error 7. CONCLUSIONS 1. 848 true and suspected Population II stars are classified us- ing the methods described in Paper I. In addition, 809 standard stars were reclassified in Paper I. Thus we have a total of 1657 stars classified by the uniform method. 2. Astrophysical parameters for 12 UU Herculis-type stars from the "Catalogue of Population II A-F Supergiants: UU Herculis and Related Stars" (Bartkevicius 1992) were estimated. Also, among the classified stars we have found four suspected UU Herculis-type stars. We have discovered 8 supergiants with | 2 |> 400 pc. We had a hope to find many UU Herculis-type stars among the stars classi- fied as supergiants by Bartaya (1979). However, none of them was confirmed to be such. Probably, the dispersion used by Bartaya (166 A/mm at H7) was too small for the recognition of supergiants. Classification of Population II stars 535 50 100 150 Parallax (ph, mas) Fig. 15. Distribution by photometric parallaxes of metal-deficient F-M stars from the HIPPARCOS program proposed by Bartkevicius (1994a). 15 N d(ph)<-100 pc bin size - 0.2 dex 10 5 • -3.0 -2.5 -2.0 -1.5 -1.0 -0.5 0.0 0.5 [Fe/H] Fig. 16. Distribution by metallicity of the metal-deficient stars with d(ph)< 100 pc from the HIPPARCOS program proposed by Bartkevicius (1994a). 536 A. Bartkevicius and R. Lazauskaite 3. The other investigated group were the field RHB stars. We selected and classified 38 RHB stars and 24 probable RHB stars. Some stars classified by Tautvaisiene (1996b) as RHB were not con- firmed. The discrepancy between the two classifications can be due to differences in their reddening estimation. Tautvaisiene (1996b) adopted zero reddening because the investigated stars are located near the North Galactic Pole. We found the mean reddening to be about 0.04 mag. 4. 20 pairs of metal-deficient visual binaries with their compo- nents measured as separate stars were investigated. Their proper motions and radial velocities were taken from the literature. Their distances and metallicities were derived from Vilnius photometry. On the base of these data, but giving priority to astrometry, the na- ture of binaries was estimated. We identified nine physical pairs and five optical pairs. In many cases, but not always, the photometric distances and metallicities of components of the physical pairs agree quite well. 5. On the ground of our classification and on the location of stars in the HR diagram, 36 stars were assigned to a class of metal- deficient subgiants. 6. Till now the numbers of known UU Herculis-type stars, super- giants at high galactic latitudes, field RHB stars and metal-deficient subgiants are quite small. Therefore it seems important to make sure that the stars selected by us do really belong to these groups. More accurate estimations of their astrophysical parameters from high dispersion spectra would be important. 7. We have classified 471 stars from the Catalogue of Metal- Deficient F-M stars (MDPH; Bartkevicius 1993). A quite unex- pected distribution of these stars by metallicity has been found: a large fraction of these stars have solar chemical composition, al- though the criterion of including them into the catalog was [Fe/H]< —0.4. The discrepancy between our present metallicities and the metallicities given in the catalog is probably explainable by the adopted interstellar reddening. Compiling the catalog, zero redden- ing was adopted in many cases. The real reddening can be larger, as it was shown in the present paper. 8. We have classified 247 metal-deficient stars from one of the HIPPARCOS programs. Their photometric parallaxes show that only 79 of them are located nearer than 100 pc. Therefore, even after analyzing the HIPPARCOS results, the number of metal-deficient stars with reliable parallaxes remains small. Classification of Population II stars 537 ACKNOWLEDGMENTS. This work was made using the NASA Astrophysical Data System and the catalogs from the Strasbourg Astronomical Data Center. The authors are grateful to S. Bartasiüte for reading the paper and some useful suggestions. 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Lazauskaitè Waters L.B.F.M., Waelkens C., Mayor M., Trams N.R.1993, A&A, 269, 242 Worley Ch.E., Douglas G.G. 1984, The Washington Visual Double Star Catalogue, 1984, CDS Magnetic Tape S1107, Strasbourg Zdanavicius K. 1975, Bull. Vilnius Obs., No. 41, 3 Zdanavicius K., Cerniené E. 1985, Bull. Vilnius Obs., No. 69, 3 Zdanavicius K., Dodd R. J., Forbes M.C., Sullivan D.J. 1995, Baltic Astronomy, 4, 25 Zsoldos E., Fernie J.D., Arellano Ferro A., Seager S. 1993, A&A, 275, 484 Classification of Population II Stars 541 Table Al. Results of classification in the Vilnius photometric system No. Name Spectrum Ey-V [Fe/H] Mv Note 1. BD+00°32 sdK3pec 0.65 0.00 -0.67 7.07 C 2. BD+01°3070 sdGO: 0.55 0.08 -0.74 5.13: L 3. BD+01°4655 G0 V 0.53 0.01 -0.06 4.36 4. BD+01°4827 G8 V, MD? 0.61 0.02 -0.15 5.38 5. BD+02°202 MD-G9 III 0.74 0.02 -0.46 0.83 6. BD+03°193 sdF9 0.54 0.02 -0.64 4.47 7. BD+04°4557 MD-G5 III, RHB? 0.65 0.08 -0.31 0.88 L 8. BD+05°3858 MD-G5 III, SHd 0.69 0.13 -0.45 1.63 9. BD+06°65 sdG5 0.59 0.02 -0.60 5.45 L 10. BD+08°4122 B3 Ia, (sdB) 0.16 0.27 -7.60 C 11. BD+09°3223 sdF6, MDSG? 0.46 0.17 -0.84: 3.23 12. BD+11°4463 sdGO 0.50 0.00 -1.12 4.58 13. BD+11°4571 MD-K3 V, sd? 0.83 0.00 -0.68: 8.65: C, L 14. BD+12°5016 K3 V 0.72 0.00 0.05 6.84 15. BD+14°3061 UU Her-F7 Ib 0.45 0.03 -1.89 -4.45 C 16. BD+15°3485 MD-G8 III 0.72 0.12 -0.42 0.93 17. BD+17°744 K3 V 0.73 0.00 0.10 6.40 L 18. BD+18°4922 MD-G8 III 0.75 0.03 -0.45 0.83 19. BD+19°4601 MD-G2 V 0.57 0.01 -0.39 5.26 20. BD+20°3004 B6 II-III 0.11 0.03 -3.10 C 21. BD+20°5292 G7 V 0.59 0.07 -0.05: 5.49 22. BD+21°2396 MD-F2 IV-V 0.40 0.01 -0.29 3.16 L 23. BD+23°3130 sdF7:extr, MDSGE? 0.57 0.07 -2.18 5.08 L 24. BD+23°4631 BS-sdF5 0.43 0.04 -0.72 3.34 25. BD+25°2436 G8 IV, MD? 0.69 0.01 -0.24 2.71 26. BD+25°2459 G9 III 0.70 0.03 -0.03 -0.28 27. BD+25°2497 RHB?-G7 III 0.67 0.05 -0.36 1.11 28. BD+25°2502 RHB-G5 0.65 0.01 -0.68 0.82 29. BD+25°2511 MD-K0 V 0.62 0.01 -0.30 5.66 L 30. BD+25°2531 sdGO, MDSGE? 0.55 0.02 -0.98: 3.65: C 31. BD+25°2539 MD-G9 III 0.75 0.03 -0.47 0.93 32. BD+26°2368 MD-G8 III 0.76 0.04 -0.31 0.66 C 33. BD+26°2387 MD-G7 III 0.69 0.01 -0.51 0.99 L 34. BD+27°2057 RHB-G7 III 0.68 0.07 -0.36 0.97 C 35. BD+27°2130 MD-KO V 0.64 0.01 -0.59 6.28 36. BD+27°2773 MD-KO III, Ba 0.84 0.01 -0.30 1.00 37. BD+270 3334 F6 V 0.45 0.00 0.07 3.21 L 38. BD+28°2079 MD-G8 III, RHB? 0.70 0.08 -0.40 0.80 39. BD+28°3357 MD-F8 V 0.50 0.00 -0.30 4.42 40. BD+290 567 sdF8 0.50 0.01 -0.53 3.98 41. BD+290 2055 sdGl 0.54 0.07 -0.77 4.91 C 42. BD+29°2231 MD?-G6 III, RHB? 0.68 0.00 -0.13 0.99 43. BD+290 2294 MD-G5III 0.65 0.04 -0.37 1.14 44. BD+29°2321 MD-G6III, RHB 0.67 0.05 -0.33 0.95 45. BD+30°546 sdF5 0.46 0.06 -0.64 3.43 46. BD+30°559 MD-F8 V 0.50 0.09 -0.47 3.80 C 47. BD+30°2018 MD?-G9 III 0.74 0.00 -0.10: 1.02 48. BD+30°2026 MD-G9 III-IV 0.75 0.00 -0.23 0.88 49. BD+30°2027 MDSG-G7 0.62 0.05 -0.51: 3.68 50. BD+30°2034 Ba-G8 II 0.80 0.11 -0.16 -2.12 L 542 A. Bartkevicius and R. Lazauskaite Table Al (continued) No. Name Spectrum Ey-V [Fe/H] MV Note 51. BD+30°2436 MDG-G8 0.80 0.03 -1.27: -0.61 L 52. BD+31°598 MD-FO V, sg? 0.40 0.06 -0.38 2.89 53. BD+31°602 MDGE-G8 0.79 0.23 -1.84: -0.77 54. BD+31°624 BS-sdF3 0.41 0.13 -1.09 3.38 55. BD+31°645 B3V 0.02 0.71 -1.8 C 56. BD+31°1588 RHB-G2 III 0.66 0.07 -0.73 0.69 57. BD+31°3025 G3V, MDSG? 0.57 0.04 0.01 5.03 L 58. BD+31°3645 AO V, BHB? 0.18 0.00 1.21 59. BD+32°3945 Gl II 0.62 0.06 -2.0 60. BD+33°2280 MD-G8 III-IV 0.68 0.00 -0.28 1.39: 61. BD+34°2371 MD-G6 III-IV 0.70 0.04 -0.26 1.63 62. BD+34°2839 A9 III-IV 0.31 0.05 0.30 1.14 63. BD+35°2449 MD-F5 V, BS? 0.43 0.00 -0.39 3.57 64. BD+35°2450 MD-Gl V 0.55 0.00 -0.27 5.01 L 65. BD+35°2461 MD-F7 V 0.49 0.00 -0.39 3.81 L 66. BD+35°2483 BS7-F3 IV 0.42 0.03 -0.48 3.20 67. BD+35°2552 MD-Gl V 0.55 0.00 -0.46 4.98 68. BD+35°2564 MD-GO V 0.54 0.01 -0.47 4.14 69. BD+36°2303 MD-Ba?-G7 III 0.71 0.08 -0.46 0.73 70. BD+360 2384 MD7-F8 V 0.52 0.04 -0.14 1.02 71. BD+360 2400" sdF8 0.51 0.02 -0.61 4.43 72. BD+360 2403 G6 IV 0.60 0.00 0.22 4.57 73. BD+360 2404 MD7-G9 III 0.79 0.00 -0.15 1.05 74. BD+360 2408 MD-G7 III 0.76 0.00 -0.23 1.03 75. BD+360 2469 GO V 0.54 0.03 -0.04 4.17 76. BD+360 2471 GO V 0.53 0.05 -0.08 4.24 77. BD+360 2479 G8 V 0.61 0.02 0.02 5.38 78. BD+360 2481 MD7-G3: V 0.55 0.00 -0.11: 5.65 L 79. BD+360 2482 MD-K4 III 1.00 0.00 -0.31 0.06 L 80. BD+360 2483 MD-KO III 0.78 0.00 -0.24 0.70 L 81. BD+360 2484 G5 V 0.56 0.00 0.13 4.68 L 82. BD+37°432 MD-G9 III 0.75 0.03 -0.46 0.94 L 83. BD+3702435 G3 V 0.56 0.00 -0.15 5.20 84. BD+3702444 MD-G7 V 0.61 0.04 -0.51 5.82 85. BD+3702449 MD7-G9 III 0.81 0.02 -0.15 1.25 86. BD+37°2503 MD-F8 V 0.51 0.00 -0.29 4.15 L 87. BD+37°2514 sdGO: 0.52 0.02 -0.66 4.90: 88. BD+37°2517 MD-K1 III 0.85 0.00 -0.32 0.56 89. BD+3702518 MD-GO V 0.52 0.00 -0.30: 4.71 90. BD+37°2520 MD-K4 II-III 1.04 0.07 -0.26 -0.04 91. BD+37°2521 G8 V 0.63 0.05 -0.02 5.31 92. BD+37°2522 MD-Kl III 0.86 0.00 -0.39 0.30 93. BD+37°2523 MD-K2 III 0.84 0.02 -0.27 0.62 94. BD+3803231 sdGl: 0.55 0.01 -0.68: 1.90 L 95. BD+40°4197A FO IV 0.33 0.02 -0.08 2.23 L 96. BD+40°4197B MD-G8 III 0.76 0.02 -0.45 1.01 L 97. BD+4102436 MD7-G9 III 0.76 0.00 -0.20 1.23 98. BD+4102441 MD-K2 III 0.87 0.02 -0.24 0.61 99. BD+41°2442" MD-G8 III 0.70 0.04 -0.30 1.06 100. BD+41°2443 F7 V 0.48 0.01 -0.06 3.41 Classification of Population II Stars 543 Table AI (continued) No. Name Spectrum (r-vOo Ey-V [Fe/H] My Note 101. BD+41°2444 MD-F8 V 0.52 0.01 -0.22 3.88 102. BD+41°3776 sdF7 0.46 0.00 -0.67 3.38 103. BD+41°3810 BHB-B9 0.32 0.14 -1.18 1.07 104. BD+41°3903 MD-F3 IV-V 0.43 0.00 -0.44 2.99 105. BD+42°3935 G8 la 0.80 0.83 -8.7 L 106. BD+42°3937 B9 III 0.15 0.38 -1.4 107. BD+42°4189 B9 II, UU Her? 0.16 0.21 -3.7 C 108. BD+43°3638 MD-G8 III 0.75 0.07 -0.40: 0.93 109. BD+44°367 MD-A9V, BS? 0.37 0.05 -0.90: 0.79 L 110. BD+44°2763 F2 III-IV 0.36 0.04 -0.07 1.75 111. BD+44°3738 MD-G6 III, SRd 0.68 0.00 -0.36 1.75 112. BD+45°2798 MD?-K0 III, Ba 0.81 0.00 -0.17 1.13 113. BD+45°4352 MD?-K5 II-III 1.01 0.11 -0.26: 0.31 114. BD+46°186 B9 IV+Gl II 0.51 0.00 0.18 2.00 C 115. BD+46°2573 MD-K5 II-III 1.02 0.06 -0.35 0.11 116. BD+48°2699 G9 IV 0.66 0.03 0.02 3.52: 117. BD+48°2701 MD?-F1 IV-V 0.38 0.03 -0.22 1.60 118. BD+48°3755 MD-KO V 0.65 0.00 -0.51 6.33 119. BD+49°939 BS-sdF5 0.42 0.20 -1.16 3.40 L 120. BD+49°2137 B5 V 0.09 0.03 -0.6 121. BD+52°913A MD-K4 V 0.76 0.00 -0.23 6.93 L 122. BD+53°979 MD-Ba-KO II-III 0.76 0.39 -0.29 -0.08: L 123. BD+54°2461 AO V 0.20 0.20 1.15 124. BD+58°2562 B8 V 0.16 0.21 -0.37 125. BD+59°2407 K2 III 0.84 0.21 0.04 0.77 126. BD+60°2522 09 II, sdOB?, He? 0.00 0.53 -6.10 127. BD+62°2124 MD-F6 V 0.46 0.06 -0.40 3.49 128. BD+65°111 RHB-GO III 0.60 0.28 -0.64 0.92 129. BD+65°125 sdF5 0.45 0.11 -0.78 3.26 130. BD+65°159 sdF7 0.50 0.06 -0.65 3.60 131. BD+65°1572 K3 V, MD? 0.70 0.02 -0.14 6.73 132. BD+66°82A MD-FO V 0.41 0.02 -0.34 3.01 133. BD+66°84 MD-G8 III 0.74 0.24 -0.40 1.05 134. BD+66°92 sdGO 0.54 0.04 -0.72 4.86 135. BD+66°113 BS-sdF3 0.44 0.02 -0.58 3.05 136. BD+75°597 MD-F7 V 0.48 0.05 -0.59 3.56 137. BD-00°65 sdF8 0.53 0.01 -0.76 4.60 138. BD-00°4526 MD-G8 III-IV 0.69 0.00 -0.65: 1.48 139. BD-01°4383 Kl V 0.66 0.00 -0.06 5.72 140. BD-07°133 MD-K2 III 0.84 0.00 -0.24 0.71 141. BD-07°230 AO V 0.20 0.00 0.79 142. BD-070 5988AB G2 V 0.53 0.00 0.12 4.66 143. BD-07°5988B G7: III 0.72 0.03 -0.13 0.22 144. BD-08°279 F7 V 0.48 0.03 0.04 3.51 145. BD-08°280 MD-KO III 0.77 0.01 -0.21 0.95 146. BD-09°176 MD-G9 V 0.60 0.00 -0.02: 5.44 L 147. BD-10°4311 MD-GO V 0.55 0.01 -0.34 4.76 148. BD-10°6092A K5 V 0.78 0.00 6.83 L 149. BD-10°6092AB K9 V 0.78 0.00 6.93 150. BD-10°6092B K6: V 0.75 0.00 8.65 544 A. Bartkevicius and R. Lazauskaite Table Al (continued) No. Name Spectrum (l"-V)o Ey-V [Fe/H] MV Note 151. BD--11° 160 sdF7extr 0.47 0.00 -1.96 4.18 152. BD--12°81 MDSG-G7: 0.65 O.Ol -0.83 0.99 153. BD--13°6438 sdF3 0.39 0.03 -1.14:: 2.57 154. BD--13°6442 MD-F3 IV-V 0.42 0.02 -0.28 2.89 155. BD--13°6443 F6 V 0.48 0.02 -0.13 3.29 156. BD--13°6444 MDGE-KO, CH? 0.99 0.09 -1.50 -1.54 157. BD--13° 6446 MD-F3 V, BS 0.43 0.03 -0.36 3.19 158. BD--13° 6447 MD-F9 V 0.51 0.00 -0.39 3.97 159. BD--13°6465 sdB5 0.08 0.21 3.50 160. BD--14° 184 MD7-K4 V 0.74 0.00 -0.06: 7.62 161. BD--14°6472 G3 V 0.56 0.03 0.10 4.32 162. BD--14°6517 MD-Kl III 0.87 0.03 -0.48 0.32 163. BD--15°98 sdF8 0.47 0.00 -0.75 4.72 164. BD--15°6357 MD7-K0 III 0.79 0.04 -0.16 1.05 165. BD--16°121 MD-F8 IV-V 0.49 0.02 -0.22 2.70 166. BD--16°168 G9 V 0.62 0.04 -0.04 5.18 L 167. BD--16°6253 G9 IV 0.67 0.03 0.17 3.00 168. BD--17°117 G6 V 0.59 0.03 -0.03 5.27 169. BD--17°6850 MD7-G0 V 0.53 0.00 -0.16 4.10 170. BD--18°10 MD-GO V 0.54 0.04 -0.20 4.12 171. BD--18°6261 MD-GO V 0.54 O.Ol -0.55 5.09 172. BD--19°27 MD-Gl V 0.56 0.00 -0.40 5.26 173. BD--19°109 MD-K5 II-III 1.00 0.09 -0.27 1.00 L 174. BD--19°111 Ml V, sd? 1.04 0.00 8.80 L 175. BD--19°129 MD-G7 V 0.58 0.02 -0.19 5.20 L 176. BD--20°95 G8 V 0.61 0.03 -0.11 5.10 177. BD--20° 117 Kl V 0.66 0.03 -0.04 6.30 178. BD--20° 160 K3 V 0.67 0.00 0.02 6.53 179. BD--20°4124 MDG-G3:, WG 0.75 0.06 -1.26 -0.46 180. BD--22°31 MD-KO III 0.80 0.01 -0.30 0.64 181. BD--23°12851 sdKl 0.65 0.02 -1.15:: 6.64 182. BD--27°13815 MD-K3 III 1.05 0.01 -0.43 -0.69 183. BD -38°245 MDGEI-G5 0.66 0.08 -2.53 -0.50 184. HD 87 MD7-G8 III-IV 0.70 0.04 -0.11 1.38 185. HD 316 MD-GO V 0.53 0.00 -0.23 4.47 186. HD 571 (A6 II+F9 II) 0.35 0.09 C 187. HD 603 MD-Gl V 0.53 0.00 -0.34: 4.42 188. HD 748 MD-GO V 0.52 0.00 -0.25 4.26 189. HD 919 M3 III, (MD7-K3III) 1.23 0.09 -0.70 L 190. HD 947 MD-G9 III, Ba 0.75 0.08 -0.47 0.85 L 191. HD 955 B5V: 0.07 0.04 -0.3 192. HD 967 MD-Gl V 0.57 0.00 -0.46 4.98 193. HD 1000 F7 V 0.47 0.00 -0.11 3.60 194. HD 1112 B9 V 0.16 0.00 0.85 195. HD 1256 B6 V, sdB5? 0.10 0.04 -0.20 L 196. HD 1440 MD-G7 III 0.71 0.05 -0.27 0.92 197. HD 1584 MD-G2 V 0.57 0.02 -0.50 4.43 198. HD 1605 KO IV 0.73 0.02 -0.09 2.76 199. HD 1635 K3 II-III 0.93 0.05 -0.05 0.47 L 200. HD 1641 MD-F5 V 0.45 0.03 -0.29 3.42 L Classification of Population II Stars 545 Table AI (continued) No. Name Spectrum (Y-V)o Ey-v [Fe/H] MV Note 201. HD 1654 MD-G7 III 0.75 0.02 -0.19 1.11 202. HD 2084 MD?-Ba-G4 (II-III) 0.71 0.03 -0.20 -0.15: 203. HD 2094 BS-Fl: 0.38 0.04 -0.67 1.16 L 204. HD 2141 Gl V 0.55 0.02 -0.01 4.50 205. HD 2170AB MD-G5 III 0.65 0.05 -0.31 1.12 L 206. HD 2207 F9Ib 0.51 0.10 -4.30 L 207. HD 2221 MD?-G8 V 0.65 0.00 -0.36: 5.77 208. HD 2233 MD7-K1 III 0.82 0.04 -0.18 0.81 209. HD 2329 B3 V 0.07 0.21 -0.30 L 210. HD 2343 G8 III-IV 0.75 0.07 -0.17 0.88 L 211. HD 2437 G5 V 0.58 0.04 0.08 4.65 L 212. HD 2469 MD-G6: III 0.70 0.00 -0.29 0.65 213. HD 2506 MD-G8 III-IV 0.72 0.05 -0.45 0.93 214. HD 2670 MD-GO V 0.55 0.02 -0.45 4.61 215. HD 2694 MD-F7 V 0.47 0.00 -0.28 3.76 216. HD 2719A MD-F7 IV-V 0.49 0.01 -0.25 3.40 L 217. HD 2796 MDGE-G3, RHB? 0.63 0.07 -2.27 0.01 218. HD 3042 MD-G2 V 0.57 0.00 -0.42 5.47 219. HD 3415 MD-F8 V 0.50 0.04 -0.25 3.64 220. HD 3556 GO V 0.53 0.00 0.08 4.44 221. HD 3951 MD-G8 III 0.72 0.01 -0.25 0.80 222. HD 4008 Kl III-IV 0.82 0.05 -0.02 0.95 223. HD 4098 MD-G5: V 0.56 0.00 -0.43 5.03 224. HD 4271A F8 V 0.51 0.00 -0.06 4.03 L 225. HD 4353 K0 IV 0.73 0.01 -0.07 1.80: 226. HD 4615D (A9 IV+Kl III-IV) 0.46 0.28 C, L 227. HD 4775 Fl V+G7 V 0.36 0.17 L 228. HD 4822 MD-F9 V 0.53 0.01 -0.42 4.54 229. HD 4915 G5: V, MD? 0.58 0.00 -0.26 4.90 230. HD 4928 MD-G9 III 0.80 0.00 -0.23 0.87 L 231. HD 5319 KO III-IV 0.75 0.00 0.14 2.33 232. HD 5352 BHB-A9: 0.31 0.10 -1.39 0.95 233. HD 5362 MD?-K3 III 0.93 0.04 -0.16 0.67 234. HD 5575 MD?-K0 III 0.77 0.05 -0.15 0.96 235. HD 5588 MD-Kl III 0.87 0.04 -0.39 0.45 236. HD 5744 B9 V 0.16 0.02 0.76 237. HD 5911 Gl IV 0.54 0.05 0.25 3.21: 238. HD 6286 MDSG-G8 0.74 0.06 -0.73 2.97: L 239. HD 6628 sd(MDSG)G8extr 0.69 0.00 -1.46 6.94 C 240. HD 7351 (M3 II) 1.11 0.17 -2.5 L 241. HD 7671 MD-K5 II-III 1.04 0.03 -0.26 -0.09 242. HD 7732 MD-G6 III-IV 0.74 0.00 -0.65: 1.00 243. HD 8065 B9 Ib 0.23 0.32 -5.80 244. HD 8082 MD-K4 III 1.03 0.01 -0.34 -0.31 245. HD 8323 B7 V 0.12 0.03 -0.20 246. HD 9270AB MD-G8 III 0.77 0.00 -0.33 0.93 L 247. HD 9746 MD-KO III 0.84 0.06 -0.44 0.57 248. HD 9754 MD-F3 V 0.43 0.02 -0.54 3.19 249. HD 9861 MD-F3 IV 0.43 0.05 -0.40 3.05 250. HD 9864 sdF8 0.50 0.00 -0.60 4.55 546 A. Bartkevicius and R. Lazauskaitè Table Al (continued) No. Name Spectrum (Y~V)o Ey-V [Fe/H] Mv Note 251. HD 9922 MD-F5 IV-V 0.45 0.00 -0.27 3.09 252. HD 9996 AO V 0.17 0.01 1.08 L 253. HD 10059 AO V 0.22 0.07 0.91 254. HD 10060 K3 III 0.85 0.08 0.08 1.00 255. HD 11037 MD-G8 III 0.76 0.00 -0.32 0.92 L 256. HD 12402 MD-KO III 0.77 0.01 -0.15 0.99 L 257. HD 12533ABC Kl Ia 1.03 0.00 -7.4 L 258. HD 13421 MD-F9 V 0.63 0.00 -0.40: 5.06: c, L 259. HD 13474 Al V+Gl III 0.44 0.17 L 260. HD 15176 MD-K2 III 0.83 0.01 -0.16 0.82 L 261. HD 15833 MD-Ba-G9 III 0.75 0.11 -0.26 0.89 262. HD 15910 B9 V 0.16 0.02 0.30 0.84 263. HD 16257 BS-sdF3 0.42 0.03 -0.52 2.99 264. HD 16901 Gl lab 0.62 0.12 -7.0 L 265. HD 20654 G 7 III-IV 0.65 0.16 -0.05 2.53 266. HD 21267 B8 V 0.14 0.08 0.50 267. HD 21269 Gl lab 0.61 0.26 -6.0 c, L 268. HD 21755 MD-G9 III 0.73 0.01 -0.33 0.87 269. HD 22360 MD-G8 II-III 0.77 0.04 -0.32 0.88 270. HD 23065 MD-G7 V 0.61 0.00 -0.37 5.70 271. HD 23439AB sdKO 0.64 0.00 -1.10 6.70 L 272. HD 23605B AOV 0.21 0.18 0.77 L 273. HD 27348 MD-G8 III 0.73 0.00 -0.34: 0.97 L 274. HD 27887 MD-F6 V 0.46 0.02 -0.45 3.13 275. HD 28782 A2: V 0.22 0.12 1.04 276. HD 29907 sdG5extr 0.57 0.02 -1.46 6.01 277. HD 30229 MDSGE-G3: 0.60 0.06 -2.32 2.15 L 278. HD 30240 MD-Ba-G8 III 0.72 0.00 -0.29 1.71 279. HD 31362 MD-F3 IV 0.40 0.00 -0.50 2.89 L 280. HD 32008 MD-G5 III-IV 0.64 0.00 -0.40 1.35 L 281. HD 34043 MD7-K3 II-III 0.94 0.05 -0.18 0.19 L 282. HD 36335 MD-F9 IV 0.41 0.04 -0.53 3.06 283. HD 36702 MDGE-K2 0.97 0.00 -2.29 -2.33 284. HD 38094 MD?-G6 III-IV 0.67 0.04 -0.26 2.07 285. HD 38558 A9 II-III 0.24 0.11 -0.50 286. HD 42633 MD7-K3 III, Ba? 0.93 0.05 -0.16 0.22 L 287. HD 44517 RHB-Gl: 0.51 0.00 -1.29 0.82 c, L 288. HD 45282 sdG5:extr 0.64 0.00 -2.34 6.99 289. HD 46276 A7 III 0.33 0.06 2.12 290. HD 46528 FO IV 0.32 0.12 1.88 291. HD 47147 RR Lyr-F7 0.48 0.01 -1.82 0.68 C 292. HD 48660 KO III 0.74 0.07 -0.08: 0.88 293. HD 50082 MD-Ba-G8 III 0.75 0.03 -0.40 1.00 294. HD 50103 MD-G8 III-IV, Ba? 0.72 0.03 -0.86 1.95 295. HD 51832 F2 III-IV 0.36 0.08 0.06 1.58 296. HD 52497 MD-G8 III 0.72 0.02 -0.33 0.72 L 297. HD 55195A A Boo-F3(III) 0.42 0.01 -0.63 0.90 c, L 298. HD 55195B MD-K2 III 0.85 0.03 -0.21 0.97 L 299. HD 56167 C3,0CH: 0.86 0.02 -0.73 L 300. HD 58425 MD-KO III 0.80 0.05 -0.38 0.71 Classification of Population II Stars 547 Table AI (continued) No. Name Spectrum EY-V [Fe/H] MV Note 301. HD 58965 MD-F5 V 0.45 0.00 -0.19 3.20 302. HD 58966 F5 V 0.43 0.00 -0.09 3.33 303. HD 60986 MD-G8 III-IV 0.70 0.00 -0.29: 0.93 L 304. HD 64144 K5 II 1.04 0.00 -2.5 305. HD 66498 sd(MDSG)G7pec 0.63 0.00 -0.75 5.86 C 306. HD 71703 K0 III-IV 0.76 0.00 0.05 2.62: 307. HD 72779 G2 III-IV 0.55 0.06 0.13 2.02: L 308. HD 73017 MD-G8 III-IV 0.73 0.00 -0.41 0.91 L 309. HD 73171 MD-Kl III 0.85 0.02 -0.26 0.60 L 310. HD 73394B F6 V 0.48 0.03 0.05 3.35 L 311. HD 73394C F6 V 0.48 0.02 0.05 3.25 L 312. HD 73709 A5 IV-V 0.25 0.02 0.10 1.51 L 313. HD 73710 G9 III 0.78 0.00 -0.11 0.80 L 314. HD 73759 F2 III 0.36 0.07 0.01 1.47 315. HD 74132 F3 IV-V 0.40 0.00 -0.11 3.34 L 316. HD 74327 F1 IV, RHB? 0.40 0.00 0.00: 1.86: 317. HD 75555 F5: III-IV, RHB 0.44 0.00 -0.05 1.15 318. HD 76351 K3 la 1.04 0.00 -9.0 L 319. HD 77912 MD7-G8 II 0.75 0.05 -0.20 -1.29: 320. HD 79554 K3 III 0.88 0.07 -0.14 0.42 L 321. HD 80290AB MD-F7 IV-V 0.45 0.00 -0.41 3.43 L 322. HD 81539 BS-sdF5 0.43 0.03 -0.67 3.19 323. HD 81774 F1 IV 0.35 0.00 -0.15 1.75 L 324. HD 83189 MD-K2 III 0.89 0.02 -0.34 0.04 L 325. HD 83287 A7 IV-V 0.28 0.00 0.13 2.09 326. HD 83489 MD-Kl III 0.84 0.00 -0.30 0.52 L 327. HD 84123 A Boo-F0:(III) 0.38 0.01 -0.79 0.31 328. HD 84800 A Boo?-A3V 0.21 0.00 1.27 329. HD 84903 MDGE-G8 0.78 0.21 -2.18 -1.59 330. HD 85015 MD-F3 V, BS? 0.41 0.00 -0.47 3.00 L 331. HD 88923 RHB-F3 0.43 0.00 -1.23 0.73 L 332. HD 89414 MD-Kl III 0.83 0.00 -0.31 0.50 333. HD 90040 MD-Kl III 0.86 0.00 -0.39 0.45 L 334. HD 90089 sdF3, BS? 0.45 0.00 -0.81 3.47 L 335. HD 90164 MD-GO V 0.53 0.00 -0.40 4.38 336. HD 91190 MD-G7 III 0.75 0.00 -0.41 0.82 337. HD 91480 MD-F3 V, BS, VB? 0.38 0.00 -0.41 3.20 L 338. HD 92787 MD-Fl IV-V 0.37 0.00 -0.44 1.79 L 339. HD 99747 MD-F5 V 0.42 0.00 -0.68 3.42 L 340. HD 99829 F5 V 0.41 0.00 -0.05 3.39 341. HD 101841 F3 III 0.39 0.02 -0.15 1.57 342. HD 101906AB MD-G7 III 0.67 0.04 -0.46 2.41: L 343. HD 102102 A7 IV 0.25 0.06 0.03 2.15 344. HD 102570 F3 IV-V 0.39 0.00 -0.05 3.41 345. HD 104425 sdF8 0.47 0.00 -0.70 4.40 L 346. HD 104513 A7 IV-V 0.30 0.00 2.06 L 347. HD 104783 RHB-G3 0.66 0.02 -0.59 0.50 348. HD 105944 MD7-G5 III 0.64 0.06 -0.14 1.49: 349. HD 106574 MD-Kl III 0.86 0.00 -0.35 0.57 L 350. HD 106677 MD7-K0 III 0.79 0.07 -0.26 0.88 L 548 A. Bartkevicius and R. Lazauskaitè Table Al (continued) No. Name Spectrum (Y-V) o Ey-V [Fe/H] MV Note 351. HD 107054 Fl III, VB? 0.35 0.03 1.68 L 352. HD 107346 (sdKOpec) 0.62 0.07 -0.96: 6.49 c, L 353. HD 107465 MD-K4 II-III 1.04 0.01 -0.30 -0.19 354. HD 107700 A6 V+G9 III-IV 0.46 0.02 L 355. HD 108100 MD-F2 V 0.37 0.00 -0.38 2.86 356. HD 108317 sdGlextr, MDSGE? 0.59 0.00 -2.01 4.73 C 357. HD 108464 (A9 IV-V+G9 III-IV) 0.47 0.03 L 358. HD 108467 MD7-G9 III 0.79 0.01 -0.17 1.03 359. HD 108834 MD-K2 III 0.84 0.04 -0.34 0.75 360. HD 108976 MD-F6 IV-V 0.47 0.00 -0.28 3.79 361. HD 109282 M3 II-III 1.20 0.08 -2.1 362. HD 109484 MD?-G9 III, Ba 0.74 0.02 -0.15 1.75 363. HD 110326 A8 III 0.31 0.05 0.30 1.62 L 364. HD 110679 G6 IV 0.63 0.08 0.09 3.35: 365. HD 111285 MD-G9 III, Ba? 0.73 0.02 -0.19 1.56 L 366. HD 111348 MD-F9 V 0.52 0.00 -0.38 4.39 367. HD 111456 MD-F8 V 0.48 0.00 -0.25 3.59 L 368. HD 111721 MDSGE-G3 0.65 0.01 -1.58 2.05 369. HD 111765 MD-K3 III 0.92 0.01 -0.21 0.34 370. HD 111812 RHB-G3:, Gl III-IV 0.61 0.01: -1.09: 0.75 L 371. HD 112257 G3 V 0.58 0.00 -0.13 4.94 372. HD 112412 sdF3 0.38 0.00 -0.66 3.24 L 373. HD 112413 B9 V 0.09 0.00 0.30 1.05 L 374. HD 112887 MDSG-F2 0.44 0.01 -0.46 2.92: 375. HD 112989AB MD-KO III 0.80 0.07 -0.28 0.53 L 376. HD 113001AB sdOB? 0.05 0.25 4.20 L 377. HD 113049 MD-KO III 0.78 0.01 -0.23 0.92 378. HD 113994 MD-G8 III 0.74 0.02 -0.37 0.99 L 379. HD 117555C MD-G6(III:), sg? 0.70 0.03 -0.61 3.55:: c,L 380. HD 117555C MD-G5(III-IV) 0.66 0.03 -0.59 3.29: 381. HD 117555C MD-G5 III-IV 0.65 0.03 -0.55 1.66: 382. HD 117555C MD-G5 III 0.67 0.03 -0.44 0.86 383. HD 117567 F5 V 0.43 0.00 0.13 3.56 L 384. HD 118245 MD-F3 IV 0.41 0.02 -0.52 3.20 385. HD 118904 MD-K2 III 0.86 0.05 -0.28 0.65 386. HD 119425AB MD?-K2 III 0.83 0.00 -0.18 0.69 L 387. HD 120164A MD?-G9 III 0.79 0.01 -0.16 1.08 L 388. HD 120182 MD-F9 V 0.53 0.02 -0.37 4.49 389. HD 120566 MD-F9 V 0.54 0.00 -0.51 3.75 390. HD 121147 BHB-AO 0.18 0.00 -0.76 1.09 391. HD 121211 MD-K2 III 0.85 0.00 -0.26 0.68 392. HD 122052 MDGE-KO 0.96 0.00 -1.77 -1.96 L 393. HD 124243 MD-Gl V 0.55 0.00 -0.28 5.25 394. HD 124953 FO IV 0.30 0.00 -0.09 2.10 L 395. HD 124969 G2 V 0.56 0.04 -0.12 4.43 396. HD 125230 MD-F9 V 0.53 0.02 -0.26 4.59 397. HD 126029 G2 V 0.53 0.00 -0.12 4.78 398. HD 126991 MDSG-G5?, G3 V 0.65 0.02 -1.13: 2.69 399. HD 127243 MD-G5 III 0.65 0.05 -0.37 0.90 400. HD 127337 K3 II-III 0.94 0.09 -0.08 0.38 L Classification of Population II Stars 549 Table AI (continued) No. Name Spectrum (Y-V)o Ey-v [Fe/H] MV Note 401. HD 127413 MD-GO V 0.52 0.00 -0.36: 4.57 402. HD 127505 MD-GO V 0.54 0.01 -0.31 4.46 403. HD 127825 MD-GO V 0.52 0.00 -0.56 4.44 404. HD 128220 (sdOB), VB? 0.40 0.00 L 405. HD 128902 MD-K5 II-III 1.03 0.06 -0.33 -0.25 L 406. HD 129336 G9 III 0.73 0.00 -0.12 1.57 L 407. HD 129846 MD-K5 II-III 0.99 0.02 -0.32 0.06 L 408. HD 130952 MD-G9 III 0.74 0.02 -0.41: 1.05 409. HD 131509 MD-G9 IV 0.68 0.02 -0.39: 2.77 410. HD 132142 KO V 0.62 0.00 -0.08 5.68 411. HD 132564 MD-F6 V 0.50 0.03 -0.32 3.62 412. HD 132678 MD-K3 III 0.93 0.04 -0.26 0.37 413. HD 132772 BS-FO: 0.37 0.01 -0.66 1.36 414. HD 133208 MD-G6 III 0.74 0.00 -0.39: 0.97 415. HD 134246 MD-G8 III 0.70 0.02 -0.23 1.02 416. HD 134320 MD-K2 III 0.87 0.06 -0.37 0.39 L 417. HD 134323 MD-G9 III 0.73 0.02 -0.42: 0.88 L 418. HD 134335 MD-K2 III 0.86 0.04 -0.22 0.70 L 419. HD 134475 MD-F5 IV-V 0.44 0.01 -0.45 2.78 420. HD 135482 F3 III+K3 II-III, MD-KO III-IV 0.80 0.05 421. HD 137071 K6 Ib 1.16 0.02 -5.0 422. HD 138085 MD-Ba-G6 III 0.71 0.04 -0.27 0.14: 423. HD 138265 MD-K4 III 1.04 0.01 -0.40 -0.41 424. HD 138852 MD-G9 III 0.74 0.02 -0.43: 0.99 L 425. HD 139074 MD-Ba-G8 III 0.74 0.01 -0.47: 0.91 L 426. HD 139087 G9 II-III+K7 III 0.81 0.04 L 427. HD 139497 MD-F8 V 0.51 0.07 -0.53 3.74 428. HD 139761 MD-G8 III 0.76 0.04 -0.21 1.00 429. HD 139778 MD-KO III 0.81 0.02 -0.27 0.68 430. HD 140385 G3 V 0.57 0.00 -0.03 5.11 L 431. HD 140458 G5 V 0.58 0.01 0.06 4.89 432. HD 140716 MD-KO III 0.80 0.02 -0.19 0.86 L 433. HD 141021 MD?-F3 IV-V 0.42 0.05 -0.15 2.90 434. HD 141353 K3 III 0.87 0.06 -0.04 0.52 435. HD 141472 MD-K4 III 0.99 0.02 -0.30 0.01 436. HD 141531 MD-G6:III 0.73 0.19 -0.25 0.18 C 437. HD 142438 MD-Ba-G5 III 0.71 0.01 -0.17 -0.31: 438. HD 142980 K2 III-IV 0.83 0.01 0.09 1.24 439. HD 144204 K4 II 1.04 0.07 -3.0 L 440. HD 146813 B3 II-III 0.04 0.05 -3.9 C 441. HD 147352 MD7-K4 II-III 0.95 0.03 -0.12 0.32 442. HD 148211 MD-F7 IV-V 0.50 0.02 -0.54 3.97: 443. HD 148349 M2 III 1.15 0.14 -0.11 -0.58 L 444. HD 148642 MD-F8 V 0.52 0.01 -0.52 4.24 445. HD 148743 UU Her-F3 lab 0.35 0.09 -0.79 -6.78 C, L 446. HD 149161 MD?-K5:III 1.06 0.00 -0.15 -0.34 L 447. HD 150010 MD7-K3 III 0.88 0.06 -0.08 0.90 448. HD 150030 MD-Ba-G8 II-III 0.76 0.04 -0.20 0.94 449. HD 151101 MD-Kl III 0.86 0.06 -0.33 0.23 450. HD 151388 MD-K5 II-III 0.99 0.03 -0.31 0.07 L 550 A. Bartkevicius and R. Lazauskaite Table Al (continued) No. Name Spectrum (Y-V) 0 Ey-V [Fe/H] MV Note 451. HD 151937 MD-Kl III 0.87 0.04 -0.38 0.15 452. HD 152224 K0 III-IV 0.76 0.03 -0.11 1.63 L 453. HD 152905 MD?-Ba-G9 III 0.76 0.01 -0.22 0.72 454. HD 153344 G5 V 0.57 0.00 0.10 4.65 L 455. HD 153751 MD-G8 III 0.73 0.00 -0.52 0.92 L 456. HD 153956 MD-Kl III 0.84 0.02 -0.23 0.67 457. HD 155524 G9 III-IV 0.73 0.00 -0.11 2.14: 458. HD 155675 MD-GO V 0.52 0.01 -0.57 4.55 L 459. HD 156826 MD?-G8(IV-V:) 0.69 0.00 -0.52: 4.12: C 460. HD 156947 MD7-K0 III 0.81 0.01 -0.13 0.78 L 461. HD 157466 MD-GO V 0.51 0.00 -0.53 4.42 462. HD 157617 MD-Kl III 0.86 0.09 -0.27 0.38 463. HD 159501 MD-KO III 0.79 0.04 -0.23 1.00 L 464. HD 160290 MD-KO III 0.82 0.04 -0.23 0.83 L 465. HD 160823 MDGE-G6 0.75 0.04 -1.37 -0.20 L 466. HD 160885 MD-K3 V 0.73 0.00 -0.42 7.18 467. HD 161695 A2 Ib 0.18 0.03 -5.20 468. HD 161815 G9 III-IV 0.73 0.04 -0.10 2.01 469. HD 162036 F2 III-IV 0.37 0.04 -0.07 1.44 470. HD 162076 MD7-G9 III-IV 0.73 0.00 -0.09 1.50 471. HD 162667 MD7-G8 II-III 0.75 0.04 -0.12 0.66 L 472. HD 162714 MDGE-KO 0.89 0.28 -1.45: -1.23 L 473. HD 163547 K3 III 0.89 0.02 -0.06 0.52 474. HD 164136 B6 IV+F3 II 0.30 0.13 C, L 475. HD 165462 MD-G8 III 0.72 0.14 -0.33 0.46 476. HD 165683 MD-Kl III 0.86 0.01 -0.24 0.42 477. HD 165803 MD:-G5 V 0.58 0.00 -0.32 5.20 478. HD 165872 09 V 0.08 0.43 -3.10 L 479. HD 166460 MD-K2 III 0.85 0.05 -0.21 1.04: 480. HD 166479/80 A9 IV+G9 III-IV 0.52 0.06 L 481. HD 167944 FO III: 0.37 0.26 1.29: L 482. HD 168092 MD-Fl IV-V 0.39 0.00 -0.36 1.87 L 483. HD 169060 G9 III 0.76 0.02 -0.15 1.05 484. HD 169191 K2 III 0.86 0.06 0.05 0.93 L 485. HD 169223 MD-Kl III 0.85 0.06 -0.22 0.69 L 486. HD 169413 G8 III-IV 0.73 0.03 -0.15 0.97 487. HD 169689 B9 III+G7II, G5 IV 0.60 0.16 L 488. HD 169885 A6 IV 0.23 0.03 1.77: 489. HD 170174 MD-G8 III 0.76 0.09 -0.29 0.88 490. HD 170899 MDSG:-G5: 0.74 0.10: -0.96: 2.68: L 491. HD 171245 MD-K5 II-III 1.03 0.05 -0.29 0.06 L 492. HD 171496 MD-G5 II-III,WG 0.66 0.21 -0.32 0.71 493. HD 172365 F9 Ib 0.52 0.14 -4.30 494. HD 173029 KO III 0.79 0.05 -0.18 1.43 495. HD 173294 MD-Ba-G5: III 0.68 0.14 -0.24 1.84 496. HD 173416 MD-KO III 0.78 0.02 -0.19 0.94 497. HD 173423 Kl III 0.84 0.03 -0.11 0.87 498. HD 173475 MD-Kl III 0.84 0.11 -0.28 0.94 499. HD 173567 F7 V 0.52 0.10 -0.14 3.87 500. HD 173666 Fl III 0.35 0.07 -0.19 1.62 Classification of Population II Stars 551 Table AI (continued) No. Name Spectrum (K-Klo Ey-v [Fe/H] MV Note 501. HD 173764 MD-G8 III 0.81 0.05 -0.53 0.44 L 502. HD 173883 MD-F9 V 0.53 0.03 -0.44 4.55 503. HD 174205 MD-K2 III 0.87 0.04 -0.26 0.52 504. HD 174817 BHB-A2 0.30 0.02 -1.21 0.93 505. HD 175021 sdF5 0.45 0.05 -0.67 3.39 506. HD 175443 MD-K5 II-III 0.98 0.00 -0.26 0.25 507. HD 175679 MD-Ba-G8 III-IV 0.73 0.03 -0.59 1.65 L 508. HD 176155AB Kl III 0.81 0.00 -0.06 0.98 L 509. HD 176408 K2 III 0.84 0.04 0.12 0.90 L 510. HD 176704 K3 III 0.88 0.01 0.04 0.62 L 511. HD 176707 MD-G8 III 0.76 0.02 -0.38 0.95 L 512. HD 178020 MD-F6 V 0.49 0.04 -0.44 3.62 513. HD 179094 MD-KO III 0.78 0.04 -0.20 1.04 L 514. HD 180583 F7 I-IIb 0.48 0.07 -3.7 L 515. HD 180584 K0 III-IV, VB? 0.77 0.03 -0.22 0.74 516. HD 180928 K4 III 0.94 0.09 -0.12 0.16 L 517. HD 181053 MD?-Ba-G9 III 0.75 0.05 -0.25 -0.37 L 518. HD 181182A A8 III-IV 0.31 0.07 1.66 L 519. HD 181182A B8 IV-V 0.15 0.07 -0.21: L 520. HD 181182A B8 V 0.14 0.07 0.16 L 521. HD 181276 G8 III 0.74 0.00 -0.10 1.17 L 522. HD 182274 MD-F9 V 0.49 0.00 -0.31 3.45 523. HD 182440 MD-K3 III 0.94 0.02 -0.30 0.31 524. HD 183085 FO III 0.32 0.10 0.89 525. HD 183098 KO III 0.79 0.00 -0.17 1.06 L 526. HD 183344AB Gl lab 0.69 0.29 -7.5 C, L 527. HD 183439 MD-K5: III 1.08 0.02 -0.24 -0.75 L 528. HD 183536 MD-GO V 0.51 0.00 -0.50 4.41 529. HD 183864AB Gl Ib 0.64 0.36 -4.6 L 530. HD 184293 K3 III 0.85 0.08 0.04 0.85 L 531. HD 184409 MD-F5 V 0.46 0.03 -0.51 3.13 532. HD 184958 MD-K4 III 1.03 0.00 -0.34 -0.31 533. HD 185016 A5: III: 0.24 0.12 0.27 534. HD 185018A MD-G5 II-III, WG? 0.68 0.03 -0.41 -1.06 L 535. HD 185353 MD-G7 III, RHB 0.68 0.03 -0.28 0.98 L 536. HD 185657B MD-Ba-G8 III-IV 0.73 0.00 -0.78 1.59 L 537. HD 185657C MD-F8 V 0.52 0.04 -0.30 4.56 L 538. HD 185657D MD-G9 III 0.76 0.04 -0.28 0.87 L 539. HD 185732 F3 III 0.39 0.04 -0.1 L 540. HD 185982 MD-Ba-G8: III 0.70 0.08 -0.21 -0.85 541. HD 186253 MD-FO IV 0.37 0.04 -0.47 1.92: L 542. HD 186621 MD-G9 III 0.73 0.10 -0.43: 0.81 543. HD 186675 MD-G9 III 0.75 0.00 -0.43 0.96 C 544. HD 186776 M3 III, MDGE? 1.23 0.05 -1.00 L 545. HD 187193 MD-G8 III 0.76 0.01 -0.31 0.95 546. HD 187982 A2 Ia 0.26 0.49 -7.0 L 547. HD 188149 MD-Ba-K3 II-III 0.96 0.07 -0.19 0.34 548. HD 189108 MD?-Ba-G5 II 0.70 0.02 -0.21 -0.97 549. HD 189410 MD-Fl V, A Boo?, BS? 0.39 0.01 -0.56 1.13 L 550. HD 189943 MD7-G8 III-IV, RHB? 0.65 0.05 -0.05 2.13: 552 A. Bartkevicius and R. Lazauskaite Table Al (continued) No. Name Spectrum Ey-V [Fe/H] MV Note 551. HD 190211A MD7-K4 II-III 0.96 0.05 -0.15 0.13 L 552. HD 190211B MD-Ba?-G6 III 0.74 0.05 -0.61 1.01 L 553. HD 190327 MD-Ba-G8 II 0.77 0.05 -0.25 -1.65: 554. HD 190630 MD-Kl III 0.86 0.05 -0.28 0.63 555. HD 190771 G3 V 0.57 0.00 0.07 4.74 L 556. HD 191010 MD-G8 III 0.71 0.08 -0.21 0.92 L 557. HD 191264 F8 IV-V 0.51 0.11 0.19 3.38: 558. HD 191494 B9 IV+(F1 III) 0.18 0.02 559. HD 191546 F2 II-III 0.42 0.14 0.53 L 560. HD 191814 EHB-G7 III 0.68 0.03 -0.43 1.05 561. HD 192876 MD-G8 II-III, AGB? 0.75 0.08 -0.46 0.54 L 562. HD 193410 F3: IV-V 0.46 0.16 -0.13 3.54 L 563. HD 193632 MD-F7 V 0.47 0.00 -0.49 3.40 564. HD 194097 K3 II-III 0.93 0.05 -0.10 -0.24 565. HD 194130 MD-F3 IV 0.43 0.03 -0.29 3.06 566. HD 194378 MD-Fl IV-V 0.41 0.04 -0.33 2.41 L 567. HD 194951 A9 II, UU Her? 0.27 0.24 -2.7 C 568. HD 195506 MD-K2 III 0.84 0.01 -0.28 0.77 569. HD 195564AB G3: V 0.60 0.00 -0.15: 4.99 L 570. HD 196360 MD-Ba?-G8 III 0.74 0.00 -0.56 1.29 571. HD 196741AB MD-G6 III-IV 0.69 0.05 -0.35 1.78 L 572. HD 196821 AO III 0.16 0.00 -0.60 L 573. HD 196866 K2 III,MD? 0.84 0.12 0.03 0.98 L 574. HD 196882B AO V 0.18 0.04 0.86 C, L 575. HD 196925 G9 III-IV 0.72 0.02 -0.02 1.66 L 576. HD 196944 sdF8, MDSG? 0.52 0.09 -1.01 3.11: 577. HD 197121 K2 III 0.86 0.06 -0.04 0.70 L 578. HD 197139 MD-K2 III 0.85 0.02 -0.25 0.73 579. HD 197249 MD-G8 III 0.70 0.04 -0.40 0.65 580. HD 197433 Kl V+K9 V 0.66 0.02 L 581. HD 197433 Kl V+K9 V 0.70 0.00 L 582. HD 197433 G9V+K7 V 0.66 0.02 L 583. HD 197941 sdF8 0.51 0.00 -0.52 4.26 L 584. HD 198181 MD-K2 III 0.83 0.02 -0.24 0.76 585. HD 198364 MD-G9 III 0.75 0.01 -0.43 0.90 L 586. HD 198390 MD-F6 V 0.47 0.00 -0.53 3.21 L 587. HD 198456AB G8 III 0.79 0.05 -0.16 1.16 L 588. HD 199178 G2 III-IV 0.57 0.10 0.02 2.49: L 589. HD 199697 MD-K5 II-III 1.01 0.01 —0.29: 0.17 590. HD 199876 MD-F3 IV 0.42 0.20 -0.33 3.46 591. HD 200205 MD-K4 III 0.96 0.07 -0.17 0.16 L 592. HD 200466 G5 V 0.60 0.00 -0.14 5.39 L 593. HD 200661 MD7-K0 III 0.78 0.04 -0.21 1.06 594. HD 200663 MD-Ba-G9 III 0.71 0.05 -0.26 1.06: 595. HD 201078 F3 Ib-II 0.40 0.09 -3.80 L 596. HD 201251 MD-K5 III 1.08 0.07 -0.24 -0.27 L 597. HD 201924 K0 V 0.63 0.00 -0.03 5.39 598. HD 202144 MD-G8 III 0.75 0.01 -0.31 0.78 L 599. HD 202720 K2 III 0.86 0.06 0.01 0.76 600. HD 202908AB Gl V 0.54 0.00 -0.05 4.52 L Classification of Population II Stars 553 Table AI (continued) No. Name Spectrum (K-V)o Ey-v [Fe/H] MV Note 601. HD 203156AB B9 III+F7 II 0.39 0.10 L 602. HD 203156AB B7 II-III+F7Ib 0.34 0.15 L 603. HD 204293 A3 lab 0.23 0.09 -5.80 604. HD 205539 MD7-F3 IV-V 0.42 0.00 -0.25 3.11 L 605. HD 206301 G2 V, MD? 0.59 0.00 -0.26 5.12 L 606. HD 206445 MD-Ba?-K3 II-III, K2 Ia 1.01 0.06 -0.28 0.37 L 607. HD 206842 MD7-K3 III 0.94 0.04 -0.29 0.32 608. HD 206843 sdF8 0.52 0.01 -1.08 4.68 609. HD 207222 A Boo?-Al V 0.22 0.00 -0.10 1.22 610. HD 207356 MD-G6 III 0.69 0.07 -0.47 1.09 611. HD 207673 A2 lab 0.22 0.30 -6.10 L 612. HD 207739 sdG5extrpec, MDSGE? 0.65 0.03 -2.45 3.83 L 613. HD 207933 MD-G9 III 0.74 0.06 -0.25 1.75 614. HD 208501 B8 lab 0.15 0.59 -6.50 L 615. HD 208728 MD7-G9 III-IV 0.74 0.20 -0.20 2.01 L 616. HD 209258 MD-K5 III 1.04 0.13 -0.56 -0.09 617. HD 209663 MD-K5 II-III 1.03 0.02 -0.26 0.13 618. HD 209761 MD-K3 III 0.93 0.00 -0.31 0.42 L 619. HD 210221 A7 lab 0.28 0.24 -6.7 620. HD 210354 MD-G8 III 0.76 0.01 -0.31 0.83 L 621. HD 210752 sdF8 0.53 0.00 -0.73 4.32 L 622. HD 210905 K2 III 0.82 0.00 -0.06 0.89 L 623. HD 210985 sdF8 0.50 0.00 -0.62 4.39 624. HD 211275 F9 IV-V 0.52 0.02 0.16 3.16 625. HD 211998AB sdG2, MDSGE7-G3 0.61 0.00 -1.58: 4.50 c, L 626. HD 212071 KO II, MD? 0.79 0.13 -0.22 0.79 627. HD 212430 MD-G9 III 0.75 0.00 -0.40 0.97 L 628. HD 212943 G9 III-IV, MD? 0.82 0.00 -0.27 0.97 L 629. HD 212988 MD-K3 II-III 1.02 0.03 -0.35 0.08 630. HD 213022 K2 III 0.84 0.05 0.02 0.94 L 631. HD 213389 MD-K2 III, K2 IV 0.85 0.01 -0.39 0.65 c, L 632. HD 213781 B6 III 0.12 0.03 -1.40 633. HD 214313 MD-K4 II-III 0.98 0.03 -0.23 0.28 634. HD 214547 BS-sdF3 0.45 0.05 -0.58 3.16 635. HD 214558 Fl V+G9 III-IV 0.57 0.07 L 636. HD 214850AB G5 V, MD? 0.61 0.00 -0.31 5.33 L 637. HD 214995 MD-G9 III 0.80 0.04 -0.22 0.87 L 638. HD 215242 B7 III+Kl II 0.41 0.11 L 639. HD 215510 MD?-K0 II-III 0.79 0.01 -0.21 0.88 L 640. HD 215684A Fl lab, UU Her? 0.29 0.09 -7.0 c, L 641. HD 215943 MD-G9 III 0.76 0.02 -0.20 0.91 L 642. HD 216102 MD-Kl III 0.86 0.01 -0.31 0.58 643. HD 216131 MD-G8 III 0.72 0.00 -0.30: 1.06 644. HD 216478 MD-G9 III 0.75 0.10 -0.26 0.87 645. HD 216635 MD-G9 III-IV 0.75 0.04 -0.27 1.00 646. HD 216944 MD-G8 III 0.71 0.04 -0.41 1.05 647. HD 217314 K3 II-III 0.93 0.10 -0.06 0.35 648. HD 217459 K3 III 0.93 0.05 -0.09 0.45 L 649. HD 217476 F9 Ia 0.63 0.36 -8.7 c, L 650. HD 217782AB AO V 0.21 0.00 1.24 L 554 A. Bartkevicius and R. Lazauskaite Table Al (continued) No. Name Spectrum (Y-V) o Ey-V [Fe/H] MV Note 651. HD 217833A B5 III 0.09 0.07 -1.90 L 652. HD 217906 M3 II-III 1.19 0.10 -2.1 L 653. HD 217984 G9 IV 0.66 0.05 0.03 2.93 654. HD 218059 MD-F6 V 0.48 0.00 -0.35 3.89 655. HD 218209 MD-G3 V 0.58 0.00 -0.52 5.37 656. HD 218396 MD7-F0 V, BS? 0.35 0.01 -0.60 1.99: L 657. HD 218560 MD-KO III 0.77 0.07 -0.22 0.73 658. HD 218568 G5 V 0.57 0.01 -0.13 5.31 L 659. HD 218703 MD-G7 III 0.75 0.01 -0.24 1.44 660. HD 218790AB G3 IV-V 0.58 0.00 0.08 4.60 L 661. HD 218792 K3 III 0.93 0.04 -0.09 0.40 L 662. HD 218970 B3(V) 0.08 0.02 -0.5 C 663. HD 219018AB G2 V 0.55 0.00 0.10 4.36 L 664. HD 219139 MD-G9 III 0.75 0.04 -0.30 1.01 L 665. HD 219150A MD-F5V, MDSG? 0.43 0.00 -0.55 3.20 L 666. HD 219215 MD-K5 II-III 1.09 0.07 -0.24 -0.67 L 667. HD 219646 G5 IV 0.60 0.10 0.07 3.00 668. HD 219657AB G3 IV-V 0.57 0.00 0.06 4.75 L 669. HD 219678 MD-F6 V 0.48 0.01 -0.38 3.71 670. HD 219834AB G8 IV-V 0.63 0.00 0.05 4.23: L 671. HD 219834B K2 V 0.67 0.00 -0.01 5.59 L 672. HD 220140 Kl V 0.68 0.00 -0.33 6.36 L 673. HD 220172 B2 V, He? 0.08 0.03 -1.93 674. HD 220293 MD-G7 V 0.59 0.00 -0.41 5.44 675. HD 220386 F9 V 0.51 0.00 -0.02 4.08 676. HD 220465 G9 III 0.75 0.01 -0.08 1.20 677. HD 220957 MD-G8 III-IV 0.71 0.01 -0.38 0.81 678. HD 221091 Kl III 0.82 0.05 -0.03 0.83 679. HD 221661 MD-G9 III 0.77 0.00 -0.35 0.81 680. HD 222092 G9 III-IV 0.73 0.05 -0.10 1.05 681. HD 222093 K0 III 0.76 0.02 -0.12 1.34 L 682. HD 222369 sdF7:extr 0.48 0.02 -1.80 4.93 683. HD 222582 G2 V 0.56 0.00 0.01 4.78 L 684. HD 222721 G8 V 0.60 0.00 -0.16 5.39 685. HD 223024AB A9 IV-V 0.36 0.00 1.90 L 686. HD 223047 MD-Ba-G8 II 0.75 0.10 -0.39 -1.42 L 687. HD 223061 F9 V, MD? 0.54 0.00 -0.22 4.46 688. HD 223084 MD-F8 V 0.52 0.00 -0.37 4.53 689. HD 223153 MD-K2 III 0.86 0.05 -0.30 0.69 690. HD 223323 MD-F4 V 0.46 0.01 -0.35 3.48 691. HD 223364 G6 V 0.59 0.03 -0.04 4.99 692. HD 223460 RHB-G3 III 0.65 0.05 -0.67 0.82 693. HD 223586 MD-Ba?-K0 III 0.85 0.00 -0.31 0.99 694. HD 223737 (M5: II:), MDGE? 1.38 0.00 -2.00 C, L 695. HD 223746 MD-G2 V 0.56 0.00 -0.35 4.86 696. HD 223860 MD?-G8 III-IV 0.73 0.03 -0.19 1.76 697. HD 224133 MD?-F9 V 0.50 0.00 -0.14 4.25 698. HD 224165 K0 II 0.81 0.08 -0.15 -0.43: 699. HD 224253AB G9 V 0.63 0.00 -0.19 5.61 L 700. HD 224383 Gl V 0.57 0.00 -0.09 4.76 Classification of Population II Stars 555 Table AI (continued) No. Name Spectrum Ey-V [Fe/H] MV Note 701. HD 224507 K3 III 0.85 0.07 0.12 1.02 702. HD 224762 G5 V 0.58 0.00 -0.02: 5.13 703. HD 224763 MD-F3 V 0.42 0.03 -0.29 3.13 L 704. HD 224817 sdGO 0.53 0.01 -0.63 4.15 705. HD 224844 MDSG7-G8 0.67 0.04 -0.48 2.84 706. HD 225015AB MD-F8 V 0.49 0.00 -0.27 4.07 L 707. HD 225085 MD-F8 V 0.52 0.00 -0.24 4.10 708. HDE 227504 MD-G0 V 0.52 0.00 -0.37 4.30 709. HDE 229281 sdF3 0.40 0.08 -0.78 2.66 710. HDE 232121A (B8 II+K1II) 0.48 0.21 L 711. HDE 232121A (B7 II+K5 II) 0.23 0.43 L 712. HDE 232121A (B6 II-III+Kl II) 0.50 0.20 L 713. HDE 232121A (B9 II+G9 Ib) 0.41 0.24 L 714. HDE 232227 A0 V 0.22 0.06 1.07 715. HDE 236429 F9 Ib 0.53 0.47 -5.0 L 716. HDE 236433 F3 II 0.38 0.47 -3.10 L 717. HDE 283705 MDGE-G7 0.77 0.08 -1.52 -0.67 C 718. HDE 283706A MDGE-G7 0.76 0.10 -1.97 -1.17 C 719. HDE 283707 MD-F8 V 0.50 0.04 -0.58 4.10 720. HDE 283716 sdK3 0.73 0.00 -1.30 7.70 721. HDE 283807 MD-Gl V 0.55 0.00 -0.42 4.64 722. HDE 284347 MD-G8 III 0.76 0.23 -0.40 0.98 723. HDE 285838 sdGl 0.56 0.04 -0.59 5.28 724. HDE 285840 MD-K0 V 0.62 0.06 -0.37 5.91 725. HDE 285845 sdG7 0.62 0.04 -0.85 6.20 726. HDE 333252 MD-G8 III 0.75 0.05 -0.37 0.75 727. HDE 335471 MD-G0 V 0.55 0.01 -0.42 5.18 728. HDE 337281 MD-K0 III 0.78 0.08 -0.22 0.94 729. HDE 340730 G2 V 0.56 0.02 -0.05 4.81 L 730. HDE 341191 MD-G7 III 0.70 0.03 -0.37 1.00 731. HDE 345011 MD-G5 III 0.65 0.07 -0.49 0.87 732. HDE 345408 MD-G8 III-IV 0.71 0.03 -0.34 0.99 733. HDE 346933 MD7-G0 V 0.54 0.01 -0.18 4.37 734. HDE 350802 MD-F5 V 0.46 0.03 -0.42 2.50 735. NGC 752 66 MD-F4 V 0.45 0.03 -0.55 3.03 736. NGC 752 139 BS-sdF3: 0.42 0.11 -1.35 3.49 737. NGC 752 520 sdF5, BS? 0.41 0.02 -0.71 3.25 738. NGC 752 533 MD-F8 V 0.49 0.02 -0.46 3.86 739. NGC 6811 36 MD-F5 V, sg? 0.45 0.05 -0.61 3.36 740. NGC 6811 81 sdF4, MDSGE?, VB? 0.44 0.03 -0.58 3.22 741. NGC 6811 85 BS?-sdFl: 0.37 0.07 -0.85 0.99 742. Cl Stock 7 51 sdF7 0.50 0.08 -0.65 4.33 743. Cl Stock 7 67 sdF8, MDSG? 0.48 0.05 -0.60 3.41 744. Cl Stock 7 86 sdF8 0.51 0.02 -0.82 4.05 745. Cl Stock 7 88 MD-G0 V 0.56 0.01 -0.58 5.27 746. Cl Stock 7 144 RHB-G2 III, Gl (III) 0.64 0.11 -0.71 0.82 747. Cl Stock 7 169 BS?-sdF4:, MDSG? 0.45 0.05 -0.54 3.25 748. Cl Stock 7 194 BS-sdF5 0.41 0.15 -1.28 3.30 749. Cl Stock 7 228 MD-G5 V 0.58 0.02 -0.40 5.09 750. [DP89] 180 MD-G0 V 0.54 0.01 -0.56 4.61 556 A. Bartkevicius and R. Lazauskaite Table Al (continued) No. Name Spectrum (y-V)0 Ey-v [Fe/H] MV 751. [DP89] 332 MD-F7: V, VB? 0.49 0.01 -0.31 3.80 752. CI Melotte 22 1282 sdF5 0.45 0.31 -0.90 3.36 753. LTT 31 MD-KO V 0.61 0.00 -0.38 5.96 754. LTT 36 MD-GO V 0.55 0.03 -0.19 4.62 755. LTT 146 MD-GO V 0.56 0.00 -0.62 5.17 756. LTT 168 sdKO 0.63 0.00 -0.75 6.28 757. LTT 175 sdG3 0.60 0.05 -1.11 6.43 758. LTT 204 K2 V 0.68 0.01 -0.07 6.36 759. LTT 209 sdK9 0.99 0.00 -0.90 8.59 760. LTT 234 MD-K3 V 0.70 0.00 -0.24: 7.24 761. LTT 289 MD-K2 V 0.63 0.00 -0.50: 6.44 762. LTT 334 sdG8 0.67 0.03 -1.25 7.19 763. LTT 335 MD-K4 Vpec 0.73 0.00 -0.37 7.68 764. LTT 338 M3V, sd? 1.14 0.00 9.00 765. LTT 349 sdM2, M3 V 1.15 0.00 10.49 766. LTT 397 (MDSG)-G8: 0.73 0.00 -0.67 2.88: 767. LTT 478 MD?-K3 V 0.72 0.04 -0.05 7.34 768. LTT 527 sdMl, Ml V 1.01 0.04 8.39 769. LTT 531 MD-K3 V 0.74 0.10 -0.37 7.95 770. LTT 558 MD-K4 V 0.73 0.00 -0.47 7.45 771. LTT 569 (M3 V) 1.28 0.00 11.32 772. LTT 575 sdM2 1.14 0.00 10.51 773. LTT 576 M2 V, sdM2 1.12 0.06 9.87 774. LTT 1244 sdK4 0.70 0.00 -0.90: 8.06 775. LTT 2402 sdG2 0.53 0.00 -1.30 5.24 776. LTT 8414 sdG3extr 0.58 0.00 -1.63: 6.49 777. LTT 8920 MD-G9 V 0.65 0.05 -0.61 6.14 778. LTT 10169 sdK5 0.75 0.00 -0.57 8.48 779. LTT 10325 sdK9 1.02 0.00 -0.81 8.75 780. LTT 16892 sdMl, Ml V 1.03 0.00 -1.20 8.82 781. LTT 16948 sdK7, Ml V 0.90 0.00 -1.09 8.08 782. LTT 16961 M2 V, sdM2 0.96 0.00 -1.01 8.52 783. LTT 17007 K9 V 0.78 0.03 -0.07 7.19 784. LTT 17012 K7 V 0.88 0.00 0.09 8.15 785. BMP 70430 MD-KO V 0.62 0.09 -0.19 5.56 786. BMP 70506 MD-GO V 0.52 0.00 -0.49 4.50 787. C* 2252 (C2,2CH) 1.02 0.28 -1.14 -1.24 788. C* 2509 C2,2CH 1.07 0.30 -1.62 -1.42 789. [J86] 33 sdF8 0.53 0.06 -0.60 4.33 790. [J86] 89 sdF8 0.53 0.06 -0.77 4.40 791. [C93 12 sdF5 0.45 0.15 -1.00 3.68 792. [C93 27 MDGE-G5 0.70 0.24 -1.70: -9.32 793. [C93 49 MD-G3 V 0.56 0.10 -0.60 5.78 794. [C93 58 sdKl 0.63 0.32 -0.86 6.55 795. [C93 81 MDSGE-G3, sd? 0.59 0.41 -0.94: 4.66: 796. [JS92] 30 MD-Ba-G8 III-IV 0.73 0.18 -0.37: 1.60 797. [Ph84] 37 BHB-A9 III 0.29 0.06 -1.22 0.89 798. [Ph84] 38 BHB-A9 III, A3 II-III 0.30 0.03 -1.22 0.92 799. [Ph84] 39 A3 IV 0.24 0.05 1.01 800. [Ph84] 50 BHB-AO V 0.22 0.02 -0.85 1.25 Classification of Population II Stars 557 Table AI (continued) No. Name Spectrum i^-vjo Ey-V [Fe/H] MV Note 801. [KJ86] 3 BS?-sdF3 0.41 0.03 -0.66 3.15 802. [KJ86] 19 sdF7extr 0.49 0.15 -2.05: 5.32 803. [SKV93 1-59 sdF9 0.51 0.07 -0.55 4.24 804. [SKV93 1-163 MD-G6 V 0.59 0.00 -0.37 5.73 805. [SKV93 1-204 MD-F9 V 0.53 0.03 -0.50 4.31 806. SKV93 1-226 MD-F9 V 0.50 0.02 -0.51 4.46 807. [CS92] 13 (MDSG)-G5 0.59 0.14 -0.46 5.52 808. [HRR77] 12 MD-F7 IV-V 0.48 0.06 -0.37 3.33 809. NGC 7023 4 MD-GO V 0.49 0.00 -0.45 4.50 810. BSNSN 1 sdGO 0.51 0.16 -0.79 4.59 811. BSNSN 54 MDG-G5, F9 III 0.71 0.20 -1.31: -0.13 812. BSNSN 97 (sdKl) 0.69 0.29 -0.63: 6.45: C 813. BSNSS9 BS-sdF5 0.42 0.23 -1.14 3.59 814. BSNSS18 MD-F9 V 0.53 0.14 -0.63 3.91 815. BSNSS 25 sdGO 0.58 0.15 -1.08: 4.88 816. BSNSS 50 (MD-GO V:) 0.53 0.20 -0.87: 4.01: C 817. BSNSS 58 sdF8: 0.52 0.23 -0.82: 4.35 818. BSNSS 94 sdF8 0.53 0.12 -0.89 4.74 819. BSNSS 108 sdF5 0.44 0.22 -0.72 3.48 820. BSNS 38 MDGE-G5 0.74 0.10 -1.69 -0.10 821. BSNS 58 MD-G6 III 0.68 0.11 -0.43 0.91 822. BSNS 75 MD-KO V 0.65 0.10 -0.47 5.65 823. BSNS 121 MD-K3 V 0.69 0.00 -0.37 6.70 824. BSD 74-2396 GO III 0.52 0.08 1.3 825. BF76] 33 RHB-G2: 0.63 0.11 -1.49 0.60 826. BF76] 1462 MD-GO V, MDSG? 0.54 0.05 -0.50 3.97 827. BF76] 1545 sdF4 0.46 0.08 -0.82 3.70 828. BF76] 1692 MD-G6 III 0.65 0.14 -0.53 0.93 829. M60] +42 329 sdFöextr, MDSGE? 0.46 0.41 -1.89: 4.10 830. M60] +43 276 sdF8, F7 V 0.51 0.03 -0.59 3.99 831. M60] +43 327 BS-sdF3, MDSG? 0.44 0.05 -0.65 3.19 832. M60] +43 331 MD-GO V 0.52 0.02 -0.44 4.36 833. T73] 36-47 MD-F9 V 0.49 0.00 -0.33 3.87 834. T73] 35-74 F9 V 0.51 0.00 -0.11 3.96 835. T73] 35-94 G5 V 0.58 0.03 0.04 4.68 836. JS84 33 MDSGE-G3 0.66 0.12 -1.53 2.24: 837. JS84 45 MD-G5 III 0.68 0.12 -0.34 1.07 838. JS84 58 MD-F3 IV 0.42 0.12 -0.50 3.24 839. J92] 24 RHB-G3 III 0.62 0.06 -0.52 1.02 840. G 8-50 MD-K3 V 0.70 0.05 -0.34 7.18 841. G 28-34 MD-K3 V 0.70 0.06 -0.37 7.13 842. G 86-39 sdG9 0.65 0.05 -0.64 6.15 843. G 99-31 sdG3extr 0.56 0.04 -1.22 5.63 844. G 153-63 sdG5 0.58 0.26 -0.60 6.33 845. G 158-77 M2 V 1.01 0.00 8.4 846. G 185-30 sdK3 0.69 0.11 -0.97 7.19 847. G 266-69 sdG5extr 0.59 0.00 -1.92 6.38 848. G 266-85 MD-KO V 0.64 0.02 -0.44 5.99 L 849. G 268-61 sdG9: 0.59 0.00 -0.73: 7.73 C 850. G 268-95 sdK3 0.66 0.00 -0.90: 6.90 558 A. Bartkevicius and R. Lazauskaité Table Al (continued) No. Name Spectrum EY-V [Fe/H] MV Note 851. G 270-7 sdG5 0.59 0.05 -0.48 5.78 852. G 270-68 sdK3: 0.64 0.00 -0.67: 6.57 853. G 270-103 sd:K3: 0.64 0.00 -0.65 7.45: 854. G 270-114 K7 V 0.84 0.00 7.32 855. ASW 1-56 MD-GO V 0.53 0.00 -0.45 4.61 856. MAL 2-5 MD-F6 V 0.49 0.05 -0.35 3.75 857. MAL 4-11 G2V.CH? 0.56 0.03 -0.07: 5.24 858. MAL 4-24 (G5 IV), MD? 0.58 0.03 -0.27 4.93 Notes: 735-736 Open cluster NGC 752. Number from Heinemann K., 1926, Astron. Nachr., 227, 193. 737-738 Open cluster NGC 752. Number from Lavdovsky V. V. 1961, Trudy Astr. Obs. Pulkovo, 73, 5. 739-741 Open cluster NGC 6811. Number from Lindoff U. 1972, A&AS, 16, 315. 742-749 Open cluster NGC 6913. Number from Sanders W.L. 1973, A&AS, 9, 221. 750-751 Open cluster NGC 7039. Number from Dzervitis U., Paupers O. 1989, Investig. of the Sun and Red Stars, Riga, No. 30, 5. 752 Open cluster Pleiades. Number from Hertzsprung E. 1947, Ann. Ster- rewacht Leiden, 19, 3. 787-788 Number from Stephenson C.B. 1973, Publ. Warner and Swasey Obs., Vol.1, No. 4, 1. 789-790 M56 area. Number from Janulis R. 1986, Bull. Vilnius Obs., No. 75, 8. 791-795 Number from Cernis K. 1993, Baltic Astronomy, 2, 214. 796 NGC 6712 area. Number from Janulis R., Smriglio F. 1992, Baltic Astronomy, 1, 430. 797-800 Number from Philip A.G.D. 1984, Contr. van Vleck Obs., No. 2, 1. 801-802 M29 area. Number from Kazlauskas A., Jasevicius V. 1986, Bull. Vilnius Obs., No. 75, 18. 803-806 Number from Straizys, Kazlauskas A., Vansevicius V., Cernis K. 1993, Baltic Astronomy, 2, 171 (Table 1). 807 Number from Cernis K., Straizys V. 1992, Baltic Astronomy, 1, 163. 808 Number from Herbst W., Racine R., Richer H.B. 1977, PASP, 89, 663. 809 NGC 7023 area. Number from Straizys V., Cernis K., Kazlauskas A., Meistas E. 1992, Baltic Astronomy, 1, 149. Classification of Population II Stars 559 810-812 M56 area. Number from Boyle R.P., Smriglio F., Nandy K., Straizys V. 1990, A&AS, 84, 1 (Table III). 813-819 M56 area. Number from Boyle R.P., Smriglio F., Nandy K., Straizys V. 1990, A&AS, 84, 1 (Table IV). 820-823 M71 area. Number from Boyle R.P., Smriglio F., Nandy K., Straizys V. 1990, A&AS, 86, 395. 824 Number from Schwassmann A., van Rhijn P. J. 1951, Bergedorfer Spec- tral Durchmusterung, Vol. 4. 825-828 Number from Becker W., Fenkart R. 1976, Photometric Catalogue for Stars in Selected Areas and Other Fields in the RGU System. Part I, Basle. 829-832 Number from Metik L.P. 1960, Izvestia Crimean Obs., 23, 60 (SA 40 area). 833-835 Number from Tchipashvili D.G. 1973, Bull. Abastumani Obs., No. 44, 3 (NGP). 836-838 M 71 area. Number from Janulis R., Straizys V., 1984, A&SS, 100, 95; Janulis R. 1984, Bull. Vilnius Obs., No.67, 18. 839 M 15 area. Number from Janulis R. 1992, Baltic Astronomy, 1, 25. 855 Number from Ardeberg A., Sarg K., Wramdemark S. 1973, A&AS, 9, 163 856-858 Number from Bartasiûtè S., Ph. D. Thesis, 1993, Vilnius University (Table 7A). 560 A. Bartkevicius and R. Lazauskaite Table A2. Notes on classification in the Vilnius photometric system. 1. BD+0°32 Peculiar star. Negative color excess, Ey-v = -0.06, is obtained by the comparison method described in the text (hereafter MD-comparison) and by the CLASS program (hereafter CLASS). 10. BD+8°4122 A supergiant B3 la at z — -1450 pc. 13. BD+11°4571 MD-comparison gives Ey-v — 0.10 and d = 40 pc; zero reddening is adopted. 15. BD+14°3061 All similar standard stars found by MD-comparison are UU Herculis-type stars. CLASS gives A5 lb in halo (z = 3440 pc). 20. BD+20°3004 B6 II-III giant in halo (z = 3770 pc). 30. BD+25°2531 May be metal-deficient subgiant or giant if zero reddening is adopted. 32. BD+26°2368 CLASS gives G7 II and EY-v = 0.10 at 2 = 2170 pc: this reddening is too large for b = 86°. 34. BD+27°2057 CLASS gives G3 II at 2 = 1710 pc. 41. BD+29°2055 Uncertain reddening: Ey~v = 0.07 from MD-comparison, Ey-v = 0.23 from CLASS and Ey-v - 0.00 from reddening maps of D.Burstein and C. Heiles, AJ, 87, 1165, 1982, hereafter BH. 46. BD+30°559 In K.Cernis, Baltic Astron., 2, 214, 1993 and V.Straizys, A. Kazlauskas, Baltic Astron., 2, 1, 1993, BD number of this star is in error: instead of BD+30°557 should be BD+30°559. 55. BD+31°645 CLASS gives Ey-v — 0.71 and MD-comparison gives Ey-v = 0.10 and sdF7extr; the BH method gives Ey-v = 0.19. 107. BD+42°4189 CLASS and MD-comparison give z > 400 pc. 114. BD+46°186 Very uncertain classification. Both MD-comparison and CLASS give Ey.v = 0.00. 120. BD+49°2137 CLASS gives B5 V at 2 = 1540 pc. 186. HD 571 Very uncertain classification. 226. HD 4615AB Uncertain classification. 239. HD 6628 MD-comparison gives Ey-v = 0.08 at d = 20 pc; CLASS gives Ey^v — 0.11 at d = 28 pc; zero reddening is adopted. 258. HD 13421 MD-comparison gives Ey-v — 0.08 at d = 17 pc; zero red- dening is adopted. 267. HD 21269 CLASS gives G1 lab at z = -650 pc. 287. HD 44517 MD-comparison gives a negative value of color excess, Ey-v = -0.06; zero reddening is adopted. Classification of Population II Stars 561 Table A2 (continued) 291. HD 47147 CLASS gives B8 II and Ey-v = 0.41; this reddening is too large for b = -22°. The BH method gives ES-v = 0.05. 297. HD 55195A CLASS gives B7 V and Ey-v = 0.37; this reddening is too large for 6 = -18°. The BH method gives EB-v = 0.04. 305. HD 66498 MD-comparison gives Ey-v = 0.06 at d = 24 pc; CLASS gives Ey-v = 0.06 at d = 24 pc; zero reddening is adopted. 318. HD 76351 CLASS gives K3 la at z = 4140 pc. 352. HD 107346 Very uncertain classification. 356. HD 108317 CLASS gives Ey-v — 0.13; this reddening is too large for 6 = 67°; the BH method gives zero reddening. 379. HD 117555 For all observations of this star (379-382) MD-comparison gives very uncertain My- 436. HD 141531 MD-comparison gives £y_v = 0.19 and CLASS gives Ey-v = 0.27; both values are too large for b = 45°; the BH method gives EB-v = 0.02. 440. HD 146813 CLASS gives B3 II-III at z = 2440 pc. 445. HD 148743 Uncertain classification from MD-comparison and CLASS: in both cases z « 1500 pc; the BH method gives EB-V = 0.19. 459. HD 156826 MD-comparison gives Ey-v = 0.08 at d = 15 pc; zero red- dening is adopted; luminosity claws uncertain. 474. HD 164136 The BH method gives EB-v = 0.05 at 6 = 24°. 526. HD 183344AB CLASS gives G1 lb at z = - 750 pc. In V. Jasevicius et al., Bull. Vilnius Obs., 85, 50, 1990 and 543. HD 186675 V. Straizys V., A. Kazlauskas, Baltic Astronomy, 2, 1, 1993, HD number is in error: instead of HD 186648 should be HD 186675. 567. HD 194951 In R. Lazauskaite, G. Tautvaisiene, Bull. Vilnius Obs., No. 85, 30, 1990, Table 2), HD number is in error: instead of HD 196866 should be HD 194951. 574. HD 196882B In V. Straizys, A. Kazlauskas, Baltic Astronomy, 2, 1, 1993, spectral type is in error: instead of K3 III should be B9. 625. HD 211998 MD-comparison gives Ey-v = 0.07 at d = 10 pc; the BH method gives EB-v — 0.01; zero reddening is adopted; b = -41° 631. HD 213389 Uncertain classification. 640. HD 215684A Very uncertain classification; a high luminosity star in halo? 649. HD 217476 MD-comparison gives uncertain classification. 562 A. Bartkevicius and R. Lazauskaite Table A2 (continued) 662. HD 218970 CLASS gives B3 at z = -960 pc, uncertain luminosity class. 694. HD 223737 The star is too red ((y-V)o = 1.38) for precise classifica- tion; z sa 1700 pc. 717. HDE 283705 The BH method gives EB-v = 0.24. 718. HDE 283706A The BH method gives EB-v = 0.24. 759. LTT 209 Both MD-comparison and CLASS give very uncertain classification. 798. [Ph84] 38 The BH method gives EB-v = 0.08. 812. BSNSN 97 Very uncertain classification. 816. BSNSS 50 Very uncertain classification, very peculiar star. 849. G 268-61 Very uncertain classification. Classification of Population II Stars 563 Table A3. Notes from the literature 2. BD+01°3070 SB. 7. BD+04°4557 SB: long period. 9. BD+06°65 VB: IDS00272N0624B, CCDM00324+0657B, 27.1, 4.0. 13. BD+11°4571 VBP-MD. Vfi: IDS21243N1145ABC, CCDM21291+1211ABC, AB: 0.7, 4.5, AC: 1.0, 1.5. 17. BD+17°744 Hyades member. 22. BD+21°2396 VB: IDS12068N2057A, 26.8, 0.9. 23. BD+23°3130 Var RV. 29. BD+25°2511 VAR: Am 0.1. 33. BD+26°2387 VBP-MD. VB: IDS12399N2603AB, CCDM12448+2530AB, 2.9, 2.1. 37. BD+27°3334 VAR: EP Lyr, RVB, P 83.34 d, V 9.96-10.90:. 50. BD+30°2034 SB: P 122.5 d. 51. BD+30°2436 VB?: ¿10. 57. BD+31°3025 PUP, VB-MD. VB: IDS17230N3109B, CCDM17267+3104B, 67.8, 1.1. 64. BD+35°2450 VBP-MD. VB: IDS13216N3540AB, CCDM13261+3509AB, 3.0, 1.2. 65. BD+35°2461 VB: IDS13283N3525C, CCDM13328+3455C, AB: orbit:a 0.18, P 54.8 yr, Am 0.5, AC: 122.5, 2.0. 78. BD+36°2481 VB-MD. VB: IDS14188N3643C, CCDM14228+3615C, AB: 137.1, 3.3, AC: 128.4, 3.8, AD: 153,8, 3.6, AE: 136.4, 3.3, AF: 126.8, 3.3. 79. BD+36°2482 VB-MD. VB: IDS14188N3643D, CCDM14228+3615D. 80. BD+36°2483 VB-MD. VB: IDS14188N3643E, CCDM14228+3615E. 81. BD+36°2484 VB-MD. VB: IDS14188N3643F, CCDM14228+3615F. 82. BD+37°432 VB?: IDS01518N3710AB, 0.2, 0.3. 86. BD+37°2503 VBP-MD. VB: IDS14069N3656AB, CCDM14111+3628AB, 1.2, 1.5. 94. BD+38°3231 VB-MD. CPM with Vega (HD172167). 95. BD+40°4197A VB-MD. VB: IDS20259N4040A, 14.0, 0.3. 96. BD+40°4197B VB-MD. VB: IDS20259N4040B. 105. BD+42°3935 VAR: TX Cyg, DCEP, P 14.7098 d, V 8.59-10.02. 109. BD+44°367 VB? 119. BD+49°939 VAR? 121. BD+52°913A VB-MD. VB: i 73. 122. BD+53°979 VAR: Z Aur, SRD, P 110-136 d, V 9.2-11.7. 146. BD-09°176 VB: IDS00479S0888A, 80, 5.3, B: CPM. 148. BD-10°6092A VB: IDS23133S0950A, 22, 1.1. 166. BD-16°168 VB: IDS00571S1547A, 27, 4.9, B: CPM. 173. BD-19°109 VB: IDS00396S1889A, AB: 90, 1.2, AC: 34, 6.0. 174. BD-19°111 VB: 34, 4.3, B: CPM. 175. BD-19°129 VB: IDS00447S1913AB, CCDM00497-1841AB, 7.0, 4.4. 189. HD 919 VB-MD. VB: IDS00085N7528A, CCDM00142+7601A, 72.6, 0.3. 564 A. Bartkevicius and R. Lazauskaite Table A3 (continued) 190. HD 947 VB-MD. VB: IDS00085N7528B, CCDM00142+7601B, 72.6, 0.3. 195. HD 1256 VAR?: V 6.47-6.52. 199. HD 1635 VAR? 200. HD 1641 VBP-MD. VB: IDS00157N3226AB, CCDM00209+3259AB, 1.6, 0.5. 203. HD 2094 VBP-MD. VB: IDS00200N3157AB, CCDM00253+3230AB, 5.2, 0.2. 205. HD 2170AB VBP-MD. VB: IDS00208N5614AB, CCDM00262+5647AB, AB: 1.8, 3.2, AC: 22.9, 3.0. 206. HD 2207 Var RV. VAR: TU Cas, CEP(B), P 2.139298 d, V6.88-S.03. 209. HD 2329 PUP. 210. HD 2343 SB: P 936 d, K 12.6 km/s. 211. HD 2437 VB: IDS00230S0035A, 25.9, 2.0. 216. HD 2719A VB: 145, 3.66, B: CPM. 224. HD 4271A VB: IDS00401S0018A, CCDM00452+0015A, 59.0, 7.3, B: CPM. 226. HD 4615D VBP. VB: Composite spectra. 227. HD 4775 VBP. VB: IDS00446N6342AB, i 0.1. SB. VAR?: V 5.33-5.39. 230. HD 4928 W630 group. 238. HD 6286 VBP-MD. VB: IDS00587N2603AB, CCDM01041+2635AB, 0.6, 1.7. SB. 240. HD 7351 PUP. VAR?: SRB, A V 0.15. 246. HD 9270AB VB: IDS01261N1450AB, CCDM01315+1521AB, 1.0, 7.0, CPM. VAR?: V 3.59-3.65. 252. HD 9996 SB: P 273.2 d. VAR: GY And, ACV, V 6.27-6.41. 255. HD 11037 Var RV? 256. HD 12402 Hyades group. 257. HD 12533ABC VBP-MD. VB: IDS01578N4151ABC, CCDM02039+4220ABC, AB: 9.8, 2.8, A: CPM with HD12534, Pleiades group. BC: orbit: a 0.296, P 61.1 yr, Am 1.2, AD: 27.9, 12.7, possibly CPM with BD+41°408. A: SB. BC: SB: P 2.67d, K1 141 km/s, K2 112.5 km/s. 258. HD 13421 Var RV? 259. HD 13474 VBP-MD. Var RV? VAR?: CST. 260. HD 15176 Var RV. 264. HD 16901 Var RV? 267. HD 21269 SB: P 3837 d. 271. HD 23439AB VBP-MD. VB: IDS03401N4110AB, CCDM03470+4126AB, AB: 8.0, 0.61, AC: 86.4, 2.4, CD: 4.4, 2.7. 272. HD 23605B VB: IDS03414N3802A, 28.9, 1.2. 273. HD 27348 VB: IDS04140N3420A, CCDM04204+3435A, 110.0, 7.9. VAR? 277. HD 30229 VB: IDS04407S6530A, CCDM04412-6519A, AB: 20.9, 3.3, BC; 3.6, 0.5. 279. HD 31362 Var RV? 280. HD 32008 Var RV? 281. HD 34043 VAR?: V 5.48-5.51. Classification of Population II Stars 565 Table A3 (continued) 286. HD 42633 Var RV? VB: IDS06067N6002A, CCDM06157+6000A, 102.7, 5.1. 287. HD 44517 SB. 296. HD 52497 VAR: CEP: P 0.7282 d, A V 0.086. 297. HD 55195A VB-MD. VB: IDS07068S4949A, 29.5, 1.61. 298. HD 55195B VB-MD. VB: IDS07068S4949B. 299. HD 56167 VAR: RU Cam, CWA, P 22d, V 8.10-9.79. 303. HD 60986 VB: IDS07320N3516A, CCDM07386+3503A, AB: 101.9, 6.0, AC: 157.0, 5.0, CD: 1.6, 1.0, CE: 17.6, 3.5. Var RV. VAR?. 307. HD 72779 Hyades group. Var RV. Praesepe. 308. HD 73017 Var RV. 309. HD 73171 Var RV? Hyades group? 310. HD 73394B VB-MD. VB: IDS08330N5206B, CCDM08404+5145B, AB: 49.1, 3.5, BC: 6.4, 4.7. 311. HD 73394C VB-MD. VB: IDS08330N5206C, CCDM08404+5145C. 312. HD 73709 VB-MD. VB with HD73710. 313. HD 73710 VB-MD. VB: IDS08346N2001A, CCDM08404+1941A, AB: 20.4, 2.5, B: CPM, AC: 64.1, 2.2, AD: 84.9, 2.5. 315. HD 74132 Var RV. 318. HD 76351 Var RV? VAR? 320. HD 79554 VAR: PG 6.3-S.l. 321. HD 80290AB VB: IDS09138N5141AB, CCDM09207+5116AB, AB: 5.9, 4.1, AC: 142.0, 3.9. VAR?. 323. HD 81774 VBP. 324. HD 83189 VB. 326. HD 83489 Var RV? 330. HD 85015 VBP. VB: IDS09440N4428A, 13.7, 2.8. 331. HD 88923 VBP? 333. HD 90040 Var RV? 334. HD 90089 Var RV. VAR? 337. HD 91480 UMa moving cluster. Sirius group. Var RV. 338. HD 92787 VB: IDS10377N4643A, CCDM10437+4612A, AB: 288.6, 2.8, CPM, AC: 149.8, 5.5, BD: 272.3, 6.1, BP: 96.0, 4.8, B: SB: K 45 km/s. 339. HD 99747 Var RV. 342. HD 101906AB VB: IDS11386N2434AB, CCDM11438+2401AB, 5.0, 7.8. 345. HD 104425 VB-MD. VB: IDS11570N4336D, CCDM12021+4304D, AB: 279.0, 1.7, BC: 221.7, 2.4, AD: 370, 3.9. 346. HD 104513 VB-MD. VB: IDS11570N4336A, CCDM12021+4304A. VAR: DP UMa, DSCTC, P 0.04-0.08d, A V 0.03. 566 A. Bartkevicius and R. Lazauskaite Table A3 (continued) 349. HD 106574 VarRV? 350. HD 106677 SB: P 10-20 d. VAR: DK Dra, P 63.15 d, A V 0.15. 351. HD 107054 VBP-MD? Var RV. 352. HD 107346 VarRV. 354. HD 107700 VBP. Coma cluster. VB: IDS12175N2624A, CCDM12225+2551A, AB: 35.0, 7.0, optical, AC: 63.9, 3.5. VAR?: V 4.78-4.89. 357. HD 108464 VBP? 363. HD 110326 Coma cluster member? SB: P 2.7045 d, K 40.7 km/s. 365. HD 111285 VAR?: A V 0.47. 367. HD 111456 UMa cluster, Sirius group. 370. HD 111812 Coma cluster member. 372. HD 112412 Hyades group. VB with HD112413. SB. 373. HD 112413 VB: IDS12514N3851A, CCDM12560+3819A, 19.4, 2.5. SB. 375. HD 112989AB VB: IDS12555N3079AB, 5.2, 9.3, CPM. 376. HD 113001AB VBP-MD. VB: IDS12557N3578AB, CCDM13004+3545AB, 0.6, 0.6. VAR?: V 9.57-10.58. 378. HD 113994 VarRV. 379. HD 117555C VB-MD. VB: IDS13261N2445C, CCDM13308+2414C, AB: 19.2, 5.5, AC: 76.6, 0.5, AD: 84.6, 5.2. VAR: FK Com, FKCOM, P 2.400 d, V 8.14- 8.33. 383. HD 117567 VB-MD. VB: IDS13261N2445A, CCDM13308+2414A, AB: 19.2, 6.5, AC: 76.6, 0.5, AD: 84.6, 5.2. 386. HD 119425AB PUP, VBP-MD. C Her group. VB: IDS13380N0403AB, CCDM13431+0332AB, 2.9, 2.4. SB. 387. HD 120164A VB: IDS13427N3903A, CCDM13470+3832A, 71.0, 3.2. SB. 392. HD 122052 VAR: V 7.22-7.31. 394. HD 124953 UMa stream, Sirius group. SB? Var: CN Boo, DSCT, P 0.04d, AB 0.03. 400. HD 127337 VB: IDS 14258N0513A, CCDM14308+0446A, 55.6, 3.5. 404. HD 128220 VBP-MD. SB: P 871.78 d, K 23.4 km/»- 405. HD 128902 Var RV? 406. HD 129336 T) Cep group. Var RV. 407. HD 129846 SB. 416. HD 134320 SB. 417. HD 134323 Var RV? 418. HD 134335 VB: IDS15042N2529A, CCDM15086+2507A, 57.5, 4.1. Var RV? 424. HD 138852 Hyades group? Var RV? 425. HD 139074 VarRV. 426. HD 139087 VarRV. 430. HD 140385 ARCT. Classification of Population II Stars 567 Table A3 (continue 432. HD 140716 VarRV? 439. HD 144204 VarRV? 443. HD 148349 VAR: V2105 Oph, SRB:, V 5.0-5.38. 445. HD 148743 SB? 446. HD 149161 ARCT. VAR: V 4.82-4.85. 450. HD 151388 SB. 452. HD 152224 SB. 454. HD 153344 ARCT? 455. HD 153751 VBP-MD. VB: IDS16562N8212A, CCDM16460+8203A, 77.0, 6.8. S] P 39.4809d, K 31.8 km/s, Am 3.44. VAR: EA/RS/D, P 39.4809 d, V 4.19-4.23. 458. HD 155675 VBP-MD. VB: IDS17080N2522AB, CCDM17121+2515AB, 0.8, 2.4. 460. HD 156947 Var RV? VAR: VW Dra, SRD:, P 170 d?, V 6.0-7.0. 463. HD 159501 VarRV? 464. HD 160290 VBP-MD. Var RV? 465. HD 160823 SB: P 45 d. 471. HD 162667 VBP-MD. VB: IDS17471N3652AB, CCDM17505+3651AB, 0.4, 1.4. 472. HD 162714 VAR: Y Oph, DCEPS, P 17.12413 d, V 5.87-6.46. SB: P 2612 d, K 1.8 km/s. 474. HD 164136 SB? VAR: SRD:, DSCT?, P 29: d, V 4.38-4.48. 478. HD 165872 VBP-MD. VB: IDS18031S2327AB, 8.0, 1.7. 480. HD 166479/80 VBP-MD. VB: IDS18057N1627AB, CCDM18101+1629AB, orbit: a 1.500, P 3040 yr, 1.1. VAR? 482. HD 168092 VBP-MD. VB: IDS18129N5633A, CCDM18146+5635A, AB: 95.6, 3.4, BC: 0.9, 0.8, BD: 5.4, 0.6. SB: P 2.0476 d, Kl 104.9 km/s, K2 108.0 km/s. 484. HD 169191 VarRV. 485. HD 169223 SB. 487. HD 169689 VBP. SB: P 385 d, Kl 25.3 km/s, A'2 33.1 km/s. 490. HD 170899 VB? 491. HD 171245 VB?: IDS18286N2333, CCDM18328+2337. Var RV? 501. HD 173764 VBP. SB: P 834 d, K 16.7 km/s. 507. HD 175679 VB: IDS18514N0220A, CCDM18564+0229A, AB: 100.1, 5.7, BC: 5.0, 0.3. 508. HD 176155AB VB: IDS18538N1714AB, CCDM18582+1722AB, AB: 7.141, 5.7. SB: P 1435 d, K 3.5 km/s. VAR: FF Aql, DCEPS, P 4.470916 d. 509. HD 176408 VarRV? 510. HD 176704 VBP-MD. ARCT. VB: 0.1, 0.0. Var RV? Sil. HD 176707 VB: AC: 22.0, 6.5. 513. HD 179094 SB: P 28.59 d, K 40.3 km/s. VAR?: V 5.81-5.87. 568 A. Bartkevicius and R. Lazauskaitè Table A3 (continued) 514. HD 180583 VAR: V473 Lyr, DCEPS:, P 1.49078 d, V 5.99-6.35. 516. HD 180928 VB: IDS19133S1542A, CCDM19190-1532A, 48.5, 5.5. 517. HD 181053 VB: IDS19137N0010A, CCDM19187+0023A, AB: 424.1, 0.2, AP: 49.5, 6.1, BQ: 59.0, 4.4. Var EV? 518. HD 181182A VBP. JD 2447028.208 VB: IDS19145N1925, 92.0, 3.0. SB: P 3.3806, K1 69.7 km/s, K2 209 km/s. VAR: U Sge, EA/SD, P 3.38061933d, V6.45- 9.28. 519. HD 181182A JD 2447028.20 520. HD 181182A JD 2447023.231 521. HD 181276 SB. VAR? 525. HD 183098 VBP. VB: IDS19228N6100AB, CCDM19241+6112AB, 2.3, 2.7. 526. HD 183344AB VB: IDS19240S0715AB, CCDM19294-0703AB, AB: 1.5, 5.5, AC: 35.2, 0.5. Var RV. VAR: U Aql, DCEP, P 7.02393 d, V 6.08-6.86. SB. 527. HD 183439 VB: IDS19245N2427A, CCDM19288+2442A, 424.1, 1.2. Var RV?. VAR?: V 4.39-4.46. 529. HD 183864AB VB: IDS19265N2455AB, CCDM19306+2507AB, 3.6, 4.6. SB: P 296.0 d, K 15.3 km/s. 530. HD 184293 Var RV? 534. HD 185018A VB: IDS19322N1103A, CCDM19369+1116A, AB: 16.4, 7.8, AC: 20.1, 6.3. 535. HD 185353 VBP-MD. VB: IDS19336N2234AB, CCDM19379+2248AB, 0.4, 1.5. 536. HD 185657B VB-MD. VB: IDS19352N4903B, CCDM19379+4917B, AB: 24.8, 2.9, AC: 55.9,2.9, CD: 10.5, 5.3. 537. HD 185657C VB-MD. VB: IDS19352N4903C, CCDM19379+4917C. 538. HD 185657D VB-MD. VB: IDS19352N4903D, CCDM19379+4917D. 539. HD 185732 VB? 541. HD 186253 VB? 544. HD 186776 ARCT. VAR: V973 Cyg, SRB, P 40: d, V 7.75-8.6. 546. HD 187982 SB. 549. HD 189410 SB. 551. HD 190211A VB-MD. VB: IDS19588N1813A, CCDM20033+1830A, 47.3, 3.3. 552. HD 190211B VB-MD. VB: IDS19588N1813B, CCDM20033+1830B. 555. HD 190771 VB: IDS20015N3811A, CCDM20052+3829A, AB: 12.4, 6.6, optical, AC: 40, 6.19. 556. HD 191010 VAR?: A V 0.15. 559. HD 191546 VAR: V395 Cyg, SRD:, P 40.5 d, V 7.9-8.62. 561. HD 192876 VB: IDS20121S1249A, CCDM20176-1231A, AB: 44.3, 9.5, AC: 43.7, 5.0, CD: 29.4, 4.7. SB. 562. HD 193410 VBP-MD. Classification of Population II Stars 569 Table A3 (continued) 566. HD 194378 VB: IDS20201N3810A, CCDM20238+3830A, AB: 38.5, 3.1, AC: 66.8, 0.8, A: VAR: V1322 Cyg, GCAS, V 8.77-9.70. 569. HD 195564AB VB: IDS20269S1012AB, CCDM20324-0952AB, AB: 2.9, 5.5, CPM, AC: 103.1, 4.2. 571. HD 196741AB VBP-MD. VB: IDS20342N1439AB, CCDM20388+1500AB, 3.0, 2.8. 572. HD 196821 VAR?. SB? 573. HD 196866 ARCT. 574. HD 196882B VB-MD, PUP. VB: IDS20351N2122B, CCDM20396+2143B, 9.3, 1.8. 575. HD 196925 VB: IDS20353N8044A, CCDM20297+8106A, AB: 213.9, 3.3, B: CPM, BC: 107.3, 3.2. SB. 577. HD 197121 VAR? 580. HD 197433 VBP. JD 2447018.335. VB: IDS20388N7514AB, CCDM20374+7536AB, AB: orbit: a 0.51, P 30.45yr, 2.9, AC: 0.63, 3.4. VAR: VW Cep, EW/KW, P 0.27831460 d, V 7.23-7.68. 581. HD 197433 JD 2447013.306. 582. HD 197433 JD 2447019.332. 583. HD 197941 VBP-MD. VB: IDS20342N1439AB, CCDM20388+1500AB, 3.0, 2.8. 585. HD 198364 VB: B: BD+41°3893. 586. HD 198390 VB: IDS20449N1210A, CCDM20496+1233A, AB: 65.7, 8.1, AC: 108.0, 5.2. 587. HD 198456AB VBP-MD. VB: IDS20454N3855AB, CCDM20492+3917AB, 6.0, 0.9. 588. HD 199178 VAR?: FK Com type? 591. HD 200205 VarRV. 592. HD 200466 VBP-MD. VB: IDS20585N3716AB, CCDM21024+3739AB, 4.7, 0.0. 595. HD 201078 VAR: DT Cyg, DCEPS, P 2.499215, V 5.57-5.96. HD 201251 VB: IDS21032N4715A, CCDM21066+4739A, 15.8, 9.5. VAR?: V 4.51- 596. 4.56. HD 202144 VB: IDS21089N4527A, CCDM21125+4552A, AB: 23.9, 5.4, AC: 38.2, 598. 5.5, CD: 4.8, 0.5. HD 202908AB VBP. VB: IDS21138N1109AB, CCDM21186+1134AB, AB: orbit: a 0.52, 600. P 761 yr, Am 1.9, AC: 27.5, 6.3, AD: 44.1, 5.7, AE: 88.9, 3.6. A: SB. HD 203156AB VBP. JD 2446636.300. VB: IDS21154N3749AB, CCDM21194+3814AB, 601. a 0.130, P 30: yr, Am 0.0. SB. VAR: V1334 Cyg, DCEPS, P 3.332816 d, V 5.77-5.96. 602. HD 203156AB JD 2446632.311. 604. HD 205539 VBP-MD. SB: P 12.21 d, Kl 52.0 km/s, A'2 65.2 km/s, Am 0.67. 605. HD 206301 VBP-MD. W630 group. VB: 0.0008, 2.0. SB: P 13.1736 d, K 23.0 km/s. 606. HD 206445 Var RV. 611. HD 207673 VarRV. 570 A. Bartkevicius and R. Lazauskaitè Table A3 (continued) 612. HD 207739 VB. VAR? 614. HD 208501 VAR?: V 5.79-5.82. Var RV? 615. HD 208728 VBP-MD. 618. HD 209761 Var RV. 620. HD 210354 VB: IDS22048N3241A, CCDM22092+3310A, AB: 29.3, 6.3, AC: 70.2, 5.8. Var RV? 621. HD 210752 VB? 622. HD 210905 61 Cyg group. 625. HD 211998AB VBP-MD. VB:IDS22160S7244AB, CCDM22246-7215AB, 0.100, 0.1. Var RV? 627. HD 212430 Var RV? 628. HD 212943 VB: IDS22228N0412A, CCDM22278+0441A, AB: 98.3, 5.0, AC: 181.5, 4.9. Var RV. 630. HD 213022 Var RV. 631. HD 213389 VB: IDS22260N4851A, CCDM22302+4921A, 63.9, 3.2. SB: P 17.755 d, K 40.2 km/s. VAR: V350 Lac, P 17.748, V 6.27-6.47. 635. HD 214558 VBP-MD. 636. HD 214850AB VBP-MD. VB: IDS22359N1401AB, CCDM22409+1433AB, AB: orbit: a 0.30, P 20.93 yr, Am 0.0, AC: 72.1, 5.0. 637. HD 214995 Var RV. 638. HD 215242 VBP-MD. VB: IDS22388N4638ABC, CCDM22431+4710ABC, AB: 0.5, 1.8, BC: 0.15, 2.0, SB. VAR?. 639. HD 215510 Var RV. 640. HD 215684A VB: IDS22419N5134A, CCDM22461+5206A, 18.8, 5.0. 641. HD 215943 VAR?: V 5.82-6.18. 648. HD 217459 W630 group. 649. HD 217476 VBP. VAR: V509 Cas, SRD, P 3yr, V 4.75-5.5. Var RV? 650. HD 217782AB VBP-MD. VB: IDS22580N4213AB, CCDM23026+4245AB, AB: orbit: a 0.277, P 76.6 yr, 3.7, AC: 92.4, 8.6. SB. B: VAR?: DSCT? 651. HD 217833A VB: IDS22584N5441A, CCDM23027+5514A, 20.1, 3.2. 652. HD 217906 VB: IDS22589N2732A, CCDM23038+2804A, AB: 108.5, 9.2, AC: 253.1, 7.0. Var RV. VAR: LB, V 2.31-2.74. 656. HD 218396 SB. 658. HD 218568 SB. 660. HD 218790AB VBP-MD. VB: IDS23057N4828AB, CCDM23104+4901AB, 4.1, 2.9. 661. HD 218792 Var RV? 663. HD 219018AB VBP-MD? VB: IDS23075N0209AB, CCDM23126+0241AB, AB: orbit: a 0.20, P 29.5 yr, Am 0.1, AC: 53.4, 4.1. 664. HD 219139 VB: IDS23084N1031A, CCDM23134+1104A, 33.4, 3.3. Var RV. Classification of Population II Stars 571 Table A3 (continued) 665. HD 219150A VB: IDS23085N0140A, CCDM23136+0213A, AB: 118.4, 2.5, BC: 0.7, 0.5. 666. HD 219215 ARCT. 668. HD 219657AB VBP-MD? VB: IDS23125S0204AB, CCDM23176-0131AB: AB: orbit: a 1.99, P 388.35 yr, Am 1.6, AC: 16.2, 8.3. 670. HD 219834AB VBP-MD. 671. HD 219834B VB-MD. VB: IDS23139S1400B, CCDM23191-1328B, 14.4, 2.0. Ar SB: P 2323.6 d, K 5.5 km/s. 672. HD 220140 VB: IDS23163N7827AB, CCDM23194+7900AB, 11.1, 7.3. 681. HD 222093 VB: IDS23325S1337A, CCDM23377-1304A, 33.1, 3.9. 683. HD 222582 VB: IDS23367S0593A, 113, 6.6, B: CPM. 685. HD 223024AB VBP. VB: IDS23408S1914AB, CCDM23460-1841AB, orbit: a. 14.21, P 11813 yr, 6.6, 1.0. VAR? 686. HD 223047 VBP. VB: IDS23411N4552A, CCDM23461+4624A, AB: 24.7, 9.5, AC: 62.0, 8.0, AD: 184.4, 4.0. 694. HD 223737 VAR: Z Aqr, SRA, P 135.5 d, PG 9.5-12.0. 699. HD 224253AB VBP-MD. VB: IDS23513S1003AB, CCDM23563-0930AB, 3.6, 0.5. 703. HD 224763 Var RV. 706. HD 225015AB VBP-MD. VB: IDS23575S0903AB, CCDM00026-0829AB, orbit: a 0.379, P 218.0 yr, Am 0.1. 710. HD 232121A VBP, JD 2447022.404. VB: IDS00056N5420A, CCDM00107+5453, 19.3. SB: P 36.5610 d, Kl 27 km/s, K2 91.1 km/s. VAR: SX Cas, EA7/GS, P 36.56375 d, V 8.96-9.83. 711. HD 232121A JD 2447021.452. 712. HD 232121A JD 2447024.436. 713. HD 232121A JD 2447032.394. 715. HD 236429 SB: P 688.0 d, K 14.0 km/s. VAR: DL Cas, DCEP, P 8.000669 d, V 8.63-9.26. 716. HD 236433 SB: P 2440 d, K 15.1 km/s. 729. HD 340730 VB: IDS20314N2502A, CCDM20356+2523A, 192.1, 1.7. 762. LTT 334 SB. 772. LTT 575 VB: IDS00567S0684A, 30, 0.95, B: CPM. 773. LTT 576 VB. 778. LTT 10169 VBP-MD. VB?: IDS00247N0028AB, 4.8, 0.4. 783. LTT 17007 VB: IDS23428N0551A, 930, 0.1. 843. G 99-31 VBP-MD. VB: 61.0, 0.8. 845. G 158-77 VB: IDS00210S1070A, 90, 2.70, B: CPM. 848. G 266-85 VB: IDS00129S1975A, 17, 2.6, B: CPM. 572 A. Bartkevicius and R. Laza.uska.ite ABBREVIATIONS KAPT Kapteyn group. GR1830 Groombridge 1830 group. ARCT Arcturus group. PUP <7 Puppis group. VB Visual binary. VB? Suspected visual binary. VB-MD Population II visual binary, components observed separately. VBP-MD Population II visual binary with