Baltic Astronomy, vol. 5, 1-82, 1996.
CLASSIFICATION OF POPULATION II STARS IN THE VILNIUS PHOTOMETRIC SYSTEM. I. METHODS
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 February 7, 1996.
Abstract. The methods used for classification of Population II stars in the Vilnius photometric system are described. An exten- sive set of standards with known astrophysical parameters compiled from the literature sources is given. These standard stars are classi- fied in the Vilnius photometric system using the methods described. The accuracy of classification is evaluated by a comparison of the as- trophysical parameters derived from the Vilnius photometric system with those estimated from spectroscopic studies as well as from pho- tometric data in other systems. For dwarfs and subdwarfs, we find a satisfactory agreement between our reddenings and those estimated in the uvby/3 system. The standard deviation of [Fe/H] determined in the Vilnius system is about 0.2 dex. The absolute magnitude for dwarfs and subdwarfs is estimated with an accuracy of <0.5 mag. Key words: techniques: photometric - stars: fundamental para- meters (classification) - stars: Population II
1. INTRODUCTION
The first attempt to classify Population II stars and to estimate their astrophysical parameters by using the Vilnius photometric sys- tem was made by Bartkevicius & Straizys (1970a, b, c). Later on, Straizys & Bartkevicius (1982) demonstrated a possibility to deter- mine, from photometry alone, the metallicities, temperatures and color excesses of metal-deficient giants. The most detailed calibration 2 A. Bartkevicius and R. Lazauskaite of two-color diagrams and ultraviolet excesses in terms of metallicity for Population II stars has been made by Bartkevicius & Speraus- kas (1983). In addition, for the classification of Population II stars Bartkevicius and Sperauskas suggested a method of comparison of standard and program stars. The effective temperatures for late metal-deficient giants can be estimated using the calibration of Tautvaisiene (1987). In the same paper, a preliminary surface gravity calibration is presented. How- ever, the most recent calibration of metal-deficient giants in terms of log g was published by Tautvaisiene & Lazauskaite (1993). Also, the Vilnius photometric system has been calibrated for some specific types of Population II stars. Sperauskas (1987) showed the possibility of identifying and estimating astrophysical parameters for blue horizontal branch stars, RR Lyrae-type stars and blue strag- glers. CH, barium and carbon stars were investigated by Sleivyte (1985, 1986). In this paper, methods used for classification of Population II stars will be described. The main attention will be paid to the method of comparison of standard and program stars which allows one to recognize Population II stars among other stars, as well as to estimate their spectral types, metallicities and absolute magnitudes. Also, additional calibrations used for the estimation of [Fe/H] and My for metal-deficient stars will be discussed. The methods were applied for the classification of 809 Population II and normal stars observed in the Vilnius system and included into the list of the stan- dard stars. By a comparison of these results with the values deter- mined from spectroscopy, as well as from other photometric systems, the accuracy of our methods will be evaluated. In the second paper of this series (Bartkevicius &; Lazauskaite 1996), about 900 stars which are suspected belonging to Popula- tion II will be classified in the Vilnius system, using the methods described here.
2. METHODS
At present, for the classification of Population II stars in the Vilnius photometric system we use the following methods. 1. The method of comparison of standard and program stars (in this case, the standard stars are those with known parameters; the program stars are stars whose parameters must be estimated); Classification of Population II Stars 3
2. Calibration of two-color diagrams and ultraviolet excesses in terms of metallicity; 3. Calibration of intrinsic color indices in terms of absolute mag- nitude. In this paper, the first and third methods will be described in more detail. We have not made any changes in the second method described by Bartkevicius & Sperauskas (1983).
2.1. Method of comparison of standard and program stars
2.1.1. Set of standard stars
The method of comparison of standard and program stars is based on the assumption that stars with similar photometric quan- tities such as color indices and reddening-free Q-parameters have nearly the same astrophysical quantities. Within the set of standard stars with known astrophysical parameters, we look for stars which, according to their photometric quantities, are as close as possible to a program star. Then the mean parameters of the standard stars, clos- est to the program star, are ascribed to the latter. It is evident that in this case the accuracy and possibilities of classification depend on the accuracy of parameters of the standard stars and on the complete- ness of the available set of standard stars. Therefore, we attempted to form a set of standards, which included as many as possible Pop- ulation II stars with known astrophysical parameters and observed in the Vilnius photometric system. The term Population II is used in this paper for the stars with metallicity [Fe/H]< — 0.5 and with total space velocities V >(60 - 100) km s~K Thus, we included into our set both halo and thick disk (intermediate Population II) stars. Our preliminary set of Population II standard stars was de- scribed by Bartkevicius & Lazauskaite (1993). Later on, these stan- dards were critically analyzed once more, and now the set contains a total of 809 stars of different types (827 records including variable stars in different phases). The groups of standard stars are listed in Table 1. To recognize normal stars in a sample of unknown stars, we included into our set not only Population II stars but also dwarfs, gi- ants, subgiants and supergiants with normal chemical composition. A Bootis-type stars are Population I stars, however, they were in- cluded into our set due to their metal deficiency. White dwarfs were 4 A. Bartkevicius and R. Lazauskaite also included with the purpose of separating them from sdO-B and sdF-G stars. The mean values of astrophysical parameters of standard stars, which were derived as described below, are presented in Table 6. It contains star name, intrinsic color index (Y—V)o, color excess EY-V> metallicity, absolute magnitude, spectral type, group membership and six intrinsic color indices. In the notes after the Table, informa- tion about variability, duplicity and membership in moving groups is presented. Abbreviations used in these notes are explained in Table 7. When compiling astrophysical parameters of standard stars, much attention was given to their absolute magnitudes. The My values were compiled from the literature or estimated by us as de- scribed by Bartkevicius & Lazauskaite (1993). The individual values of My were averaged with the weights inversely proportional to the square of their errors. For averaging, we used only those My values which were consistent within 2 magnitudes. Color excesses EB-V or EY-v for standard stars were obtained from different sources. For a part of stars, their reddenings were es- timated by Bartkevicius &; Sperauskas (1983), Bartkevicius & Taut- vaisiene (1987) and Bartasiute (1989). Color excesses of the remain- ing stars were obtained using estimations of interstellar reddening of different authors, among them, the maps of EG-y constructed by Burstein & Heiles (1982) from H I distribution and deep galaxy counts. In the final stage of this work, for calculation of reddening we used the program kindly supplied us by Dr. David Burstein. Stars with unknown reddening were classified in the Vilnius photometric system by the method of comparison of reddening-free Q-parameters of the standard and the program stars. Color exesses derived in dif- ferent ways were averaged with equal weights. If, however, one source gave a clearly discrepant value, it was eliminated from the average. In addition, it was assumed that stars within 50 pc are unreddened by interstellar matter. Since in most cases reddening of the standard stars is small (Fig. 1), the errors of EY-y values are not significant in determination of the intrinsic color indices. The metallicities were taken from the Catalogue of the mean
[Fe/H], Teff and log g compiled by Bartkevicius &: Lazauskaite (1995). In the case of [Fe/H] derived from high-resolution spectra, the values in Table 6 are given to two decimal places. The remaining metal- licities are derived from the medium-resolution spectra or were esti- mated in the Vilnius photometric system. Classification of Population II Stars 5
Table 1. Groups of standard stars No. Group Abbreviation N
1. Dwarfs ([Fe/H]>-0.2; Mv>4.0) D 159 2. Dwarfs with moderate metal deficiency MDD 85
(—0.2>[Fe/H]>—0.6; Mv>4.0)
3. Subdwarfs (-0.6>[Fe/H]>-1.3; Mv>4.0) SD 98 4. Extreme metal-deficient subdwarfs SDEXTR 66 ([Fe/H]< —1.3; My >4.0)
5. Giants ([Fe/H]> —0.3; Mv<2.0) G 32 6. Metal-deficient giants MDG 56
(—0.3>[Fe/H]> —1.3; Mv<2.0) 7. Extreme metal-deficient giants MDGE 67
([Fe/H]< —1.3; Mv<2.0) 8. Subgiants SG 23
([Fe/H]> —0.3; 2.0 N |——— 500 - 400 300 • 200 • 100 • oU I III! 1 1 0.00 0.02 0.04 0.06 0.08 0.10 Ey-V Fig. 1. Histogram of reddening for standard stars. Only reddenings of Ey~v < 0.10 mag are shown. 55 stars have Ey-V > 0.10 mag. Spectral types of metal-deficient standard stars were taken mainly from earlier classifications in the Vilnius photometric sys- tem (Bartkevicius &; Sperauskas 1983; Bartkevicius & Tautvaisiene 1987; Bartasiute 1989). Also, a preliminary version of the Cata- log of Field Population II Stars (Bartkevicius & Bartkeviciene 1993) was used. The spectral types of CH stars and metal-deficient barium stars are from the catalog compiled by Sleivyte & Barkevicius (1990). For white dwarfs, the spectral types are taken from the Catalog of Spectroscopically Identified White Dwarfs (McCook &; Sion 1987). For the stars of normal chemical composition the spectral types are taken from the Bright Star Catalogue (Hofileit & Jaschek 1982) and the Catalogue of Selected Types in the MK System (Jaschek 1978). 2.1.2. Intrinsic color indices and Q-parameters of standard stars The observed color indices of standard stars were compiled from the General Photometric Catalogue of Stars Observed in the Vil- nius System (Straizys & Kazlauskas 1993). Some additional sources, which were not used in the mentioned catalog, are also included. For the calculation of intrinsic color indices of standard stars, the color excesses Ey-v given in Table 6 were used. The color excess ra- tios were adopted with respect to the spectral and luminosity class as well as to the group dependence of stars. For normal stars and stars Classification of Population II Stars 7 with small or medium metal deficiency, color excess ratios of normal stars (Kuriliene & Sudzius 1974) were used. For extremely metal deficient stars, color excess ratios were calculated by Lazauskaite (1994) using the energy distribution curves of metal-deficient stars. The reddening-free (^-parameters were calculated using the al- gorithm suggested by Kazlauskas (1993). It is based on comparing Q-parameters of the observed stars with those calculated from the intrinsic color indices of different spectral and luminosity classes. The calculation is started with the excess ratios of a GO V type star. Calculations are iterated by changing the color excess ratios until the best agreement between Q-parameters calculated from the intrinsic color indices and those from the observed color indices is reached. In the calculation, Kazlauskas has used a list of the intrinsic color indices and color excess ratios of normal stars. Since the color ex- cess ratios in the Vilnius system are slightly sensitive to metalicities and pecularities in stellar spectra, we supplemented the mentioned list with the intrinsic color indices and color excess ratios of metal- deficient stars (Lazauskaite 1994), CH and barium stars (Sleivyte 1986) and white dwarfs (Bartkevicius 1976). 2.1.3. Method of comparison The aim of the method of comparison is to select a few stars from the list of the standard stars which have the most similar intrinsic color indices or Q-parameters to those of the program star, by using the criterion: /£" APi-Poi)3 aP = V n = mm' where PQ is the observed color index, the intrinsic color index or the reddening-free Q-parameter of a standard star, P is the same quantity of a program star, n is the number of color indices or Q- parameters used in the comparison. For Population II stars, this method was first applied by Bartkevicius & Sperauskas (1983). They classified stars by compar- ing the intrinsic color indices and Q-parameters. We have slightly modified this approach, namely, we additionally compare the ob- served color indices of the standard and the program stars. For this comparison, the following approach is used. First, by minimizing 2.2. Calibration of intrinsic color indices in terms of absolute mag- nitude For the estimation of absolute magnitudes of dwarfs and sub- dwarfs, as well as of giants of different metallicity, we have derived empirical relations. Here, we present only the final equations which we use for the calculation of absolute magnitudes. Deriving of these relations for dwarfs and subdwarfs on the basis of trigonometric pa- rallaxes is described in more detail by Lazauskaite (1995). The rela- tions for G-K dwarfs and subdwarfs are Mv = -3.053-8.593(P-X)o + 4.702(X-F)o + 16.733(F-F)o, (1) cr = 0.58, R = 0.82 Classification of Population II Stars 9 and Mv = 1.536 - 0.750[Fe/H] - 6.330(P-X)o + 8.693(X-Y)0, (2) a = 0.55, R = 0.84. Here and further, a is the standard deviation and R is the corre- lation coefficient. These equations are valid for dwarfs and subdwarfs with 0.50 < (Y-V)o < 0.75 and -2.5 <[Fe/H]< 0.4. For late dwarfs ((Y—V)o > 0.75), we adopted the equation which was derived on the basis of absolute magnitudes of standard stars presented in Table 6: Mv = 3.373 - 2.995(X-F)0 + 10.587(F-V)0, (3) a = 0.42, R = 0.93. The calibration for giants of different metallicity is also based on My of standard stars. For giants we have Mv = 4.473 - 6.083(tf-P)0 + 2.502(P-X)0 - 3.128(Y-V)0, (4) a = 0.55, R = 0.88 and Mv = 4.999 + 0.532[Fe/H] - 5.132(tf-P)0 - 1.111(Y-V)0, (5) a = 0.53, R = 0.88. These equations are valid for giants in the following ranges: 0.30 < (Y-V)o < 1-30 and -2.9 <[Fe/H]< 0.30. We recommend to use Eqs. (4) and (5) only for giants with My <1.0 because for less luminous giants we find disagreement with the data from the liter- ature. A similar difference of Mv was derived by Anthony-Twarog & Twarog (1994) comparing their absolute magnitudes with those derived by Bond (1980). However, at present we cannot explain the reasons of such disagreement since the trigonometric parallaxes are available for only a few of the metal-deficient giants. Also, we derived the empirical relation for the estimation of ab- solute magnitudes of white dwarfs: Mv = 9.85 + 5.54(i7 —P)o + 4.62(Y-V)0, (6) <7 = 0.42, R = 0.94. The relation is based on the absolute magnitudes of the standard white dwarfs presented in Table 6. 10 A. Bartkevicius and R. Lazauskaite 2.3. Evaluation of various methods 2.3.1. Accuracy of the method of comparison We used the following procedure for evaluating the accuracy of the method of comparison. We considered our standard stars to be the program stars, i.e., the observed color indices and Q-parameters for the program stars and for the standard stars are the same. We made three comparisons: the comparison of observed color indices, the comparison of Q-parameters and the comparison of intrinsic color indices. Then, the astrophysical parameters, derived using all three methods, were compared with those from Table 6. One of the parameters, the estimation of which is problematic when using photometry alone, is interstellar reddening. As was ex- plained on p. 8, we derived the color excesses Ey-v as differences between the observed color indices Y—V and the mean intrinsic color indices (Y"—V)o of five standard stars with the best matching of color indices or Q-parameters. Let us evaluate how reliably (Y—V)o can be estimated by this method. The results of our analysis are presented in Fig. 2. The histograms show a distribution of differences between (y — V)o from the list of standard stars and {Y — V)o derived from a comparison of color indices (a), from a comparison of Q-parameters (b) and from a comparison of intrinsic color indices (c). The mean differences, in the sense of standard value minus the value derived from a comparison, are (+0.017 ± 0.039) mag, (+0.005 ± 0.044) mag and (+0.002 ± 0.025) mag, respectively. As Fig. 2 shows, the distribution of differences, especially in Fig. 2a, is asymmetric, i.e., the (Y — V)o derived by a comparison of color indices show some tendency to be a little smaller than it should be. Therefore, Ey-v derived using such (Y — V)o will be overestimated. This leads to a conclusion that the method of comparison of color indices and Q-parameters of the standard and the program stars gives reddenings which are not reliable enough. Thus, an estimation of reddening for metal-deficient stars from photometry alone remains a problem. We decided to use two approximations in deriving the reddening. First, the mean (Y—V)o was calculated by averaging with equal weights the (Y — V)o obtained from a comparison of observed indices and from a comparison of Q-parameters. Second, these initial estimates of reddening were used for the calculation of the intrinsic Classification of Population II Stars 11 250 N 200 150 100 50 ° -0.10 -0.05 0.00 0.05 0.10 (Y-V)o(ST)-(Y-V)o(CI) 250 N 200 150 100 50 ° -0.10 -0.05 0.00 0.05 0.10 (Y-V)o(ST) -(Y-V)o(Q) 250 N 200 150 100 50 0 -0.10 -0.05 0.00 0.05 0.10 (Y-V)o(ST)"(Y-V)o (CIO) Fig. 2. Distributions of differences between the standard {Y—V)o and the (Y-V)o derived from a comparison of color indices (a), Q parame- ters (b) and intrinsic color indices (c). Only stars with A <0.1 mag are presented. Some of the stars have 0.1< A <0.2: 30 in (a), 34 in (b) and 4 in (c). 12 A. Bartkevicius and R. Lazauskaite Fig. 3. Comparison of the standard values of [Fe/H] with those derived from a comparison of intrinsic color indices (a) and (^-parameters (b) color indices of the observed stars. These latter values were compared with a set of standard stars and gave the final values of reddening. It is expected that the influence of reddening on the astrophysical parameters to be derived will be minimized when the quantities inde- pendent of reddening, i.e. intrinsic color indices and Q-parameters, are used. Therefore, only these quantities will be used in further examination of the accuracy of the method of comparison for esti- mation of [Fe/H] and My. The metallicities derived by the method of comparison of intrin- sic color indices and Q-parameters and the metallicities from the list of standard stars are intercompared in Fig. 3. The mean differences (standard values minus estimated values) are (—0.01 ±0.26) dex and (—0.02 ± 0.32) dex, respectively. A comparison of intrinsic color indices gives more reliable metallicities than a comparison of Q. Also, in the same manner we derived the absolute magnitudes. The results of their comparison with the standard values are pre- sented in Fig. 4. The mean differences between the standard values of My and those estimated from a comparison of intrinsic color indices and Q-parameters are (—0.01 ± 0.78) mag and (—0.03 ± 0.92) mag, respectively. Thus, the analysis of differences between the standard parame- ters and the parameters derived by the method of comparison of stan- Classification of Population II Stars 13 Fig. 4. Comparison of the standard values of Mv with those derived by the method of comparison of intrinsic color indices (a) and Q-parameters (b). dard and program stars leads to a conclusion that the comparison of intrinsic color indices gives more reliable astrophysical parameters than the comparison of reddening-free Q-parameters. 2.3.2. Comparison of astrophysical parameters derived by various methods Our further analysis is restricted to dwarfs, subdwarfs and giants, because the calibration of [Fe/H] by Bartkevicius Speraus- kas (1983) and the calculation of My by the equations are valid only for these types of stars. In addition to the results, following from the method of comparison, we have derived [Fe/H] from the calibrations of Bartkevicius & Sperauskas (1983) and My from the equations de- scribed in Section 2.2. For normal stars, absolute magnitudes and reddenings were also estimated using the program CLASS written by Vansevicius & Bridzius (1994). The derived values were com- pared with those from the list of standard stars, the results being summarized in Table 2. 14 A. Bartkevicius and R. Lazauskaité Table 2. Comparison of standard values with the parameters derived by various methods Method of estimation Mean difference and Number of the parameter standard deviation of stars (standard value minus estimated value) Dwarfs, subdwarfs and giants [Fe/H] (BS) -0.05±0.23 514 [Fe/H] (CIo) -0.03±0.28 552 [Fe/H] (Q) -0.07±0.39 552 Dwarfs and subdwarfs Mv from Eq.(l) +0.02±0.53 197 Mv from Eq.(2) +0.02±0.51 198 Mv (CIo) +0.05±0.58 391 Mv (Q) +0.08±0.64 391 Mv (VB) -0.16±0.76 151 Giants Mv from Eq.(4) -0.18±0.48 113 (only stars with Mv< 1.0) Mv from Eq.(5) -0.16±0.51 114 (only stars with Mv< 1.0) Mv (CIo) -0.08±0.70 151 Mv (Q) -0.13±0.77 140 Mv (VB) -0.07±0.77 28 Abbreviations in the brackets have the following meaning: CIo - the parameter was derived by the method of comparison of intrinsic color indices of standard stars with themselves, Q - the parameter was derived by the method of comparison of reddening-free Q-parameters of standard stars with themselves, BS - the metallicity was estimated using the methods suggested by Bartkevicius & Sperauskas (1983), VB - the absolute magnitude was derived using the program CLASS (Van- sevicius & Bridzius 1994). Classification of Population II Stars 15 2.3.3. A scheme adopted for deriving the astrophysical parameters On the basis of the described accuracy analysis, we have adopted the following procedure for deriving the final values of astrophysical parameters: 1. A preliminary value of (F —V)o is calculated by averaging, with equal weights, the intrinsic color indices of the most similar five standard stars selected by a comparison of observed indices and Q- parameters. Then, Ey-v is a difference between the observed Y—V and the mean preliminary (Y — V)o- After that, the intrinsic color indices are calculated with this preliminary Ey-v and taking into account a preliminary classification of the star. Then, these intrinsic color indices are compared with a set of standard stars and the new value of Ey-v is obtained. 2. The intrinsic color indices of the investigated stars are cal- culated using Ey-v described in the first item. A comparison of these intrinsic color indices with the set of standards is made again. If such a comparison gives Ey-v, significantly different from those used for the calculation of intrinsic color indices, we change Ey-v, calculate new intrinsic color indices and compare them again with the standard stars. This iterative procedure is repeated until con- sistent results are derived. For normal stars, the reddenings derived using the program CLASS are also accepted. If the distance to a star is less than 50 pc or the derived reddening is negative, we adopt Ey-v = 0.00 mag. 3. The final intrinsic color indices are calculated using the final Ey-v and taking into account the preliminary classification of the star. These color indices are used for the estimation of metallicity and absolute magnitude. 4. The mean metallicities are calculated by averaging, with equal weights, the [Fe/H] values derived by the method of Bartkevicius & Sperauskas (1983) and [Fe/H] derived by a comparison of intrinsic color indices. 5. The absolute magnitudes of dwarfs and subdwarfs are derived by averaging, with equal weights, the values from Eqs. (1) and (2). For late dwarfs ((Y - V)0 > 0.75), Eq. (3) is used. The absolute magnitudes of giants are calculated averaging, with equal weights, the values from Eqs. (4) and (5). The values of My for white dwarfs are calculated by Eq. (6). For other stars, as well as for dwarfs and giants outside the intervals of the equations, the absolute magnitudes are calculated by averaging, with equal weights, the values derived 16 A. Bartkevicius and R. Lazauskaite Table 3. Designations of spectral types for stars of different metallicity. (Here Sp is the spectral type). Range of [Fe/H] Ranges of My >+4.0 +2.0 - +4.0 <+2.0 [Fe/H] >-0.2 Sp V Sp IV Sp III -0.2> [Fe/H] >-0.6 MD-[Sp V] MD-[Sp IV] MD-[Sp III] -0.6> [Fe/H] >-1.3 sd[Sp] MDSG-[Sp] MDG-[Sp] -1.3>[Fe/H]>-2.4 sd[Sp]extr MDSGE-[Sp] MDGE-[Sp] -2.4>[Fe/H] sd[Sp]extr! MDSGE!-[Sp] MDGE!-[Sp] by a comparison of the intrinsic color indices and the reddening-free Q-parameters. For normal stars, My given by the CLASS program are also used. 6. For each classified star we also derive its spectral type. This term, which was introduced by Bartkevicius & Sperauskas (1983) for metal-deficient stars, contains a metallicity class, luminosity class and spectral class. In Table 3 we present the designations for spectral types. We have applied the described scheme for classification of the standard stars. The results of the classification are presented in Table 8, where spectral type, (V —V)o, Ey-v, [Fe/H] and My are given. The uncertain values are marked by a colon or given in brackets. The scheme of classification described will be adopted for the estimation of astrophysical parameters of other metal-deficient stars observed in the Vilnius system (Bartkevicius & Lazauskaite 1996). 3. ACCURACY OF ESTIMATION OF STELLAR PARAMETERS 3.1. Reddening Many authors have used the Burstein & Heiles (1982) reddening maps to estimate color excesses for field stars with different metal deficiency (Laird, Carney & Latham 1988; Carney, Latham, Laird & Aguilar 1994; Ryan 1989; Anthony-Twarog & Twarog 1994). How- ever, in all these estimations a doubtful assumption about a uniform distribution of dust along the line of sight to a star was used. Our es- timates are also partly based on these reddening maps which, among other sources, were used to obtain reddenings for the standard stars. Classification of Population II Stars 17 0.10 0) .u CO 0.05 • o w w 0.00 • 0.00 0.05 0.10 Ey-v (Vilnius) Fig. 5. Comparison of EY-v determined from the Vilnius and uvbyp systems In uvbyfi photometry, the values of reddening are estimated us- ing the reddening-free H/3 index and are completely independent of the reddening maps. We have compared our reddenings with those derived from the uvby[3 photometry, kindly provided to us by Dr. William Schuster. These values are based on the Schus- ter & Nissen (1989) calibration of (6 — y)o for dwarfs and sub- dwarfs. The Eb-y values were converted to Ey-v using the relation Ey-v = Ei-y/1.02. The difference between our and Schuster's red- denings is —0.002 ± 0.015 for 52 dwarfs and subdwarfs in common (Fig. 5). Schuster & Nissen (1989) indicate that their calibration gives Eb-y with a standard deviation of 0.01 mag. This value corresponds to the same value of error in Ey-v• Thus, from a comparison with the reddenings from the uvby/3 system, the formal error of Ey-v es- timation in the Vilnius photometric system for dwarfs and subdwarfs is of the order of 0.01 mag. However, we must bear in mind that only dwarfs and subdwarfs with small reddenings have been tested. In the second paper (Bartkevicius & Lazauskaite 1996) we will repeat such comparison for a larger number of common stars. 18 A. Bartkevicius and R. Lazauskaite 3.2. Metallicity [Fe/H] values derived by us in the Vilnius photometric system were compared with the metallicities determined from spectra and by using other photometric systems. The results of these comparisons are summarized in Table 4, where A is a difference between our [Fe/H] values and those from the literature. We consider that the standard deviation in comparison of our values of [Fe/H] with those determined using high dispersion spectra is about 0.25 dex (see Table 4). If the standard deviation in high- dispersion metallicities is ±0.13 dex (Laird & Carney 1988), then 3.3. Absolute magnitude In an effort to evaluate the accuracy of our estimates of absolute magnitudes, comparisons were made with the My values determined by other authors as well as with My from trigonometric parallaxes. The results are given in Table 5, where the mean A are the differ- ences between My from the Vilnius photometry and that from the literature. The comparisons show no significant dependence of A on spec- tral class, metallicity or absolute magnitude itself. Only the My values of Anthony-Twarog & Twarog (1994) show systematic dif- ferences with respect to our values, depending on the luminosity of stars (Fig. 6). Here we see the same dependence, as was noticed by Anthony-Twarog and Twarog by comparing their data with the My values of Bond (1980), i.e., for absolutely fainter stars the Anthony Twarog and Twarog values are more negative than ours. In Fig. 7, our My values are compared with MV(TT), the val- ues calculated from trigonometric parallaxes. The parallaxes were taken from van Altena et al.(1991). We restricted our sample to <7(7r)/7r < 0.175 and Lutz-Kelker corrections were applied to My(n). The majority of stars with trigonometric parallaxes are dwarfs and subdwarfs, and only six of them are giants. Therefore, using trigono- metric parallaxes, we can evaluate the accuracy of our My determi- nations only for dwarfs and subdwarfs. The criterion cr(7r)/7r < 0.175 corresponds to cr(My) < 0.38 mag. Bearing in mind that the stan- dard deviation of our My values from My{7r) is 0.60, we obtain ® o ® o ® ® © + 11+11 I I I I I I I o So EC t- co o c© o o o n o cs in os lo io 3 § jT ts fi ri H m « M O o O O CS o o O I I I I I I I D ctffe. U + + I I + + u I I I I I I I «S® ,C0 CO 3 IM O htoooaioio 3 n g CÖ co g * Ji g.s 03 es es eö ec es es es cö S "O -e g » I I I I I I I 0) Xl "O W) XI XI 3 % 43 (30 3CA CO 3 3 •n o. <<2 <¿2 <2 JS ™ «s 42 xi >» co -o -o -O m 43 3 cö <ö S e cö g 3 3 3 s CO fc, i i i-2 cö cö cö §« -o -o -O bO S)^ .2 « T3 «S3 ^ — X) Xl -Sc '3S 3 > Fig. 6. Comparison of our absolute magnitudes with those from Anthony-Twarog & Twarog (1994). The solid line is a 45° line. The estimates of My for other types of stars should be less accurate. However, there are no reliable lists in the literature for a comparison. In the future, we will try to evaluate the accuracy of our method by classifying globular cluster giants. 4. CONCLUSIONS A new set of standard stars with estimated astrophysical pa- rameters was compiled. In comparison with the previous set of Bartkevicius & Sperauskas (1983), the number of Population II stars is larger and their astrophysical parameters, particularly the My values, are more reliable. The stars are classified by three methods based on a comparison of the intrinsic color indices, Q-parameters and observed color indices with the corresponding values for the stan- dard stars. The last two methods allow us to estimate the interstellar reddening of Population II stars from photometry alone. Also, we derive the equations which relate the absolute magnitudes with the intrinsic color indices of the Vilnius system. Classification of Population II Stars Fig. 7. Comparison of our absolute magnitudes with those from trigonometric parallaxes. The Lutz-Kelker corrections are applied to My(7r).The solid line is a 45° line. However, groups of Population II standard stars are represented with unequal completeness. Therefore, only the parameters for the largest groups, such as dwarfs, subdwarfs and giants, can be evalu- ated with acceptable accuracy. Other types of Population II stars can be successfully recognized among the unknown stars but their parameters are evaluated with lower accuracy. For this, we need more Population II standard stars of different groups. Recently, Axer et al. (1994) published physical parameters from spectroscopic analysis for more than 100 metal-deficient stars. In comparison with the results of other authors, their metallicities are shifted to higher iron abundance for the most metal-poor stars. This shows that so far the metallicity scale for metal-poor stars is not very well defined. Since the estimation of metallicities and absolute magnitudes is very sensitive to errors in the intrinsic color indices, special attention must be paid for a better evaluation of interstellar reddening. About 450 of our standard stars are located nearer than 200 pc. So, the HIPPARCOS parallaxes will improve their absolute magni- tudes. However, other stars are more distant and we do not expect 22 A. Bartkevicius and R. Lazauskaite a considerable improvement of their My in the near future. The stars of globular clusters may help, if used as the standards for the comparison methods. As a first application of the methods described in Section 2, we have classified in the Vilnius photometric system the same 809 standard stars. Approximately 600 of them are Population II stars. An attempt has been made to evaluate the accuracy of estimation of the reddening, metallicity and absolute magnitude. For dwarfs and subdwarfs with small reddenings, we have found a satisfactory agreement between the reddenings estimated in the uvbyfl system and those derived by us. The standard deviation of photometrically determined [Fe/H] is about 0.2 dex. The absolute magnitudes of dwarfs and subdwarfs are estimated to be accurate to about 0.5 mag. However, reliable evaluation of My errors for other types of Population II stars, among them for giants, remains problematic. Accurate observations and classification of bright giants in globular clusters would be helpful. The results of the classification in the Vilnius photometric sys- tem of about 900 suspected Population II stars will be presented in the second paper of this series (Bartkevicius & Lazauskaite 1996). In machine-readable form, the published tables as well as the individual values of My from various sources, the observed color indices, the color excess ratios and the Q-parameters of standard stars may be obtained on a request to the authors. The software for calculation of Q-parameters and for comparison of program stars with the standard stars is also available. ACKNOWLEDGMENTS. We wish to thank David Burstein for the reddening calculation program. Thanks are due to W. J. Schus- ter, B. J. Anthony-Twarog and B. A. Twarog for data supply. We are also thankful to V. Vansevicius and S.Bartasiute for critical reading of the manuscript and helpful suggestions. 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F., Lee J.T., Hoffleit E.D. 1991, The General Catalogue of Trigonometric Stellar Parallaxes (1991): a Preliminary Version, Yale University Observatory, New Haven Vansevicius V., Bridzius A. 1994, Baltic Astronomy, 3, 193 Classification of Population II Stars CMCOCOlCOSCOOiOOiHCS N W H CO Ifl 10 S «i s io CO IC IC I 00 IC t-; 00 CO 0000000000 OhOOOOOOOO 00000 0000 0 CONOOOCOCNNCOI« t-aimcowt-coNTCTr COrHCM-'J'MOCNMi-IP» 1 0000000000 0000000000 00000000 o'o M «»oiciHinBOi Hicnujsonnnnn 0000000000 0000000000 OOOOOOOOOO lO^OOHOOCOt-NN ooooco-^t^t^csfoißo O — MOOOO-H OHOHOOHOOH WOO — OOOOOO OHISÄNDOtOt-ffl »niooisnestN HWtqoicOHiocoo« OOOOO oi-jo^oooooo riocioodddao fiDiOHNnnnt NoO'rwcO' ü g CC Cd cd Od cd Od ö uSB tü a ta o. c- ü t £ b X 3 OGü a DfflO O Da 0 a XHn u>. L* o E89"ddqqQ QqqqQQQÄQQ SagSgagsaiQ OD CO O X Cl- cd M iO co od _ co ic s S9o t* h > ü h O i 50 m u. 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I oooooooooo oooooooooo oooooooooo è Hrtnn^fOONOio n^noco^oioœ^ UÎOOOH^tûNSSN CO^Wt-CO^lO^lOCS HoddoHÒddd NinuîiOHtoiouîNîD HoddoHodoH sddddddddd m CO IO o co HOWtOJOOOON to OltOlO^QOOOtOlrtOOiC t ¡ä. ddodoHOOOrt 666h6666OO 0666666660 0 HHH^rtVHHNTT 1 0000060000 0000000000 0000000000 tS) (ßioioiovspiHnDO o c^coroco^uscsrteo^ ©nrtnvioTnTrn s? 6000000000 0000000000 0000000000 0 rlNNOBIOeWlOiO oooooohühio;D o) o) »HMfNfflWeONH ST liNNNfia»®«» CONOOOiÖOONhiOO cqoqoqtoi^toqwt^oo 1 «ooOHHHd-id * O O O O -H OOO-I OOOINOOOOO- o P5(ONlO!ßuiO(OHU5 »HOOHSHNlOHlf OOODOOJiO^flOrtWN R (filCiniOOJONlOlßN IßtßfO^lOtDiOlflDÜOO OtfÄOCtNMDPlil oL OOOOOr-iOOOi-t odoHOOodo'o I-H O O O 0 h-to-^'rtociiot^to'^' ST 1 0666666666 Sa 0666666660 0000000000 H h b toQQ U O Q Q üfflfflO Up* OUüS Q QQOqqQ Q Q- D QöjQ Din QQQq Q t/3 2! SüQOSQS-iliS SosKQSSSWOS CQ O < CO ui 0 0 a co > > > 3 > > " > X BBB £ > OOO ALfn 10 c t n » i IM B ! Ü X!ü0«»0 •>>B™> -'au B" Qa-2« Ü £ 9 9 9 > 6 H 00 ¥ S00SS0SS10 nNToqqnMcoq to vt^dnflH^OH NCJCJNiDrtOOOrt a NlÖtlOHOHl'^d »woortnnooio «-irnpOOpO^' III I T I I i-4r-« O «uihvtßionooOH N^NNntöOOO^N 00000 ooor-! ddd"ddo'dod 0060000000 o MOU!00®NSN1000 hûOUÎOWHNNHH (0UÏSONCÇNCDOOOOV 0000000000 döddddddd— 0000000000 — vnt-o — wnaies «lonONionno* co« — me* — te» — M HCOPlMPiNMIANU) ddoddddodd 000 0 000000 o'ddo'dddddd — ift — fr- — O — Wî ST «•«'cjTrmcMco^'coco 0000000000 0000000000 0000000000 MPicemv^ooMi®''* SHMOSOHOIOO® nNoiHfiDNSTro tÇCjNœuirtDOtOHCO ooinnoûoooinuiao HrtOHOOHÒdÒ O — — O — — O — — — — o — — 000 — — o O 11 N 10 Tf 01 O O V ooîDQOJCNcsoecpajoo OlIQrHkOCDO^^CO (û Cl 01 ' Oí 00 IO O O) co t»t-ooo O O m< û w CQ ^ ÜO r, OQ O OQ O & S Û en en O g^ooalfflQ 8 ÛÛ Q ÛÛiÛ ÛÛ 8ö883832__Q o ÛSSoSjûSSÛ SûSSûSûûSS œ OQ a a t¿ Ü P ®ai 00 Cb a i— - °o _r rn o> a ">5"Os V a £ < o H a 5 3 5 » û, • N 10 n 01 00 CO CS 00 — oo ri <0 ñ "i ^(¿cód^ícscót^cvid ^nOîViOOiOJNiûCO O CO CO T rH T T T t i i i i i i. VC- «o^meíns»» OOOOtflCON") (ÛOO^DOiftPSNtOWiO iû(OflO!ÛONiONNO (O^NN^N^^flOu) ddddoddddd 0 000—0000 — OOOOÒOOOÒO m < rtOWiOiûBlCOS^' t^OO^ÇOCOOOOO — 100 BOJHVifluìtìOOS Ofi^ONfcnioojoo îOiO^HHHNrtnn ^•^v^uîuîifluîioio ÛÛÛQÛÛÛÛÛÛ ÛQÛÛÛQQÛQÛ ÛÛÛQÛÛÛÛÛÛ XSXXIXXSXX a —C a a a S hC X Œ S cscô-^ricïôi^oocïd SSNNNl-NSNtO uooooooooooooooooooi NNNMNNWMWN NNNNNWNNON NNNNWCSMNMrt Classification of Population II Stars 35 NOAOOOCßflONVN ddo—dddddd oooooooooo OrHOOOOOOOO »HMflONI-DO® 0«H1H»SH(. iOwrtMcoooootooin HCiNWMONNM oooooooooo oooooooooo oooooooooo o 0»r<001Bf)0)«N lOMrHnvniCNHOo i? n on f « - « co co cm il. 0000000000 0000000000 0—00000006 »"CHOOflOON^V« 1/5 — CMOt-'VCOQt-O coo>»cMt-oO"»,cot-eM qt-coqcoooqcot-.© Docosssciowinco NOHtiOOrtiHO'"' ddodod—o—d dtiddooHOH oco^cof-t-i-wcoo (SN«oooinai(-c<® i-OlWCO^CMCOOOOlOO « tfjl i « i« Ol « S N(DtO(DiOOOtOtDr«in ^IrtLOLOiiOON^lOO) dod—doddod 00000000^0 o — 00000000 Hnnsoemet-n M 00 <0 n M CO 1 00 CM CM onnigsiotSH®« «uitooous^'io'r^'N ^t to ^ (ß 0000000000 oooooooooo 000 0000000 05 U H a Cd c- Q B 3 cn cn O Q O Q Q m m CQ Q QOOffl 0 Q Q ki 889 ™q§Q88 SC Dil I QjQQQiüüi ü SQDSüQ E o-> > £ I K « « 3 o riS > t- s ugogo X V >>>>e! 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Lazauskaitè «nooMWHSiflN» o dodoòdòdo o o o o o o o « o 0000000—0 0 «»ndSHHltHS VOOlOOINOOIti S" HNflflflrlHÏH Nfift^NNNHU)« S 1 — — O — — COCO — es (sa dddddddddO dddddddddd dddddddddd oiNito«)tnH»H í? — m — — — n n s n n dddddo'dddd dddddddddd dddddddddd 0 t- co co — V OU S X «NOOOfU-fílOO fSooïoiûœvNN sr œ s œ N U5 »C 00 ^ O OOIOt-, HNIOICn» Ncoesco'vcooescot- 1 OOHOhOOHÓH — — O — — 00 0 — — 00000© — oído ÍÍHNOlHHfflO)» cot^coocot-usus SW^SH^OOCOtO s? lOwquiNijtofitos (ûiflShûOuïStCDiO i 000—0000 0000000 — 00° a. donsooondó ooencciHrinpi» OI — (CiOOiOOOOOiOO) T^ul'VSVNNSW dddddddddd 000000000 dddddddddd 0¿ « 8g m HVNNNUÎ^WUJUÎ 0000000 00000000—0 0ÒOÒOÒOHOO 0>0>— Cii-^"«- Olt- «Ot-ttlONNiOin ÖHoddosdsd — 000000000 00000000 NCSOONOWIOIOS ulHOOtDOOSONOO) »otHieooNUN iHTPinnHnfinH iop»^ — — eo — «ScinonrtrtHn 0000000000 0000000000 0000000000 o «cvooaot-v^ooo »tott^foinciH HSTPiciHnnioo 0° 000000000 0000000000 0000000000 Ol^OlH^ißrtflCCOO 10 n so tß n 0) 10 « 0) — — — ^ — Cl^CO CO H 01 » O) V u) N w OHHrtHOHOHO «OHOOHO O O — O — O — OOOOO — sn«ni««co 10 O O M (i « 00 I OOOOOO — O idd — dddo 00000000 0 0 0, «lOtOSISTIOt-OR 00t< OS < < o. a Efi w a CQ S o Q Q Og « 2 ^ X C3 Q Cd lO Q Da Q QaÜÜDj ü a o 5ÜOÜQoiDQ2S üSQSQSSQQS QSOSSSD 02 J3 s o 2 o iß d u. u a Ii S nh 55 2 O 5 "1 Q SÜ gt s 00 x +So. o ¡¿2 ü 3 «1=1 >>£>>§ £ «->>>> » o n » o » oh » 1« — 00 QüOÜ!i! o <0 — 00 (•iOO Iß — <0 CS TT CS — (0 C1 IN 10 O O O ?? ?7?7 Od ü. 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Lazauskaitè M CO W co oo oo oo os oí o oo m i--oscooso^t,>»-«,oeo Off) s œ s s I- to oo « « i-i NÍSÍOONSViCM o'sdd ci dodo ri ddddoddddd mtoh«oooi®O »«»•»oinionaiH «oi«H®»ne'ioi ^HNihCOMCÎCIOCO 0«WHf «sno^NnpiH» coQcoMooto (caooiox(00isoiß otposcïflojsifltû coeoa>o>t- te gi 10 « to a m io « NQO1O1XVCMMCOCO cototeooi-oiooNosoo «eStOHtootDsio T-iOOOOOOOOO 00000 O O O odoond-ód oiiHinmooooooiat- ddddoddddd 00000 0000 0000000000 OS M M H M C-. C- ^ « O O O co O U XH CQ~ u 00 ïk9<99ÏS a ÛQy a Pä a ® Û Q Q cS üQüiíSfflSSmo oiûSmSûmQcûÛ SQÜQSQSosqq .. 00 1=1 o _ » « 00 d sfüOffl 1,5 t; u O íitáss» i f > X ^ rr ta M « „ ¿ « „ O íuo .o £>gAH>£> :> §>S>5>5fc>> 3MIÍ HÛ «ÛÛ00 SOlúUdOulgMfflM "NOlffi-fOOc,»« ¡¡SfaUCSfflSSCO . rttiHiji-fflnOí >1 os i »»i«® TO » qvwMSSooiCNio 00 -V ' « 10 N s T œ w HOHoddoddo ddddoddddd 0000000000 ü OD < < nsn«o»MfciH« ^rMoocococ-t-OT fOl't-O^'OítON® íJuiuioinníNÍS c^ooçôb-w^coi'i^co ÍOf $H001N01fl S pHcscó-^io^p^oóoid HCSrtfUííONOOOiO 000000000-* Classification of Population II Stars 1 PH ST" 0) in co 0 IN 10 00 0 CO ic CO 00 TT CS t- 0 r CS co t- 05 co 0 IC TT co t-; co 1» CO es 00 co 1/3 00 00 IC CO co N IC IC h- co IC pH co IC os ¡1 0 0 0 O 0 0 0 0 0 0 0 O 0 0 0 0 Tl 0 0 0 0 0 0 0 0 0 0 c s CO co iß oo 1—1 0 TT CO CS O 0) 00 01 TP 0 co co CO t- 0 Ii ic TT OS 0 CO CS CS CO r-) CS es CN CS 0 CO CS CS O 0 CO IC CS CO CS CS 11 CS CS CS IN Ii co CS CS IC 0 0 0' d d O d O 0 0 0 O O 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 w 0 c CO <0 00 CO O m CO co 00 CS ^ CO IC CO CO CO IC CS l- CO CO ^ 00 CO IC t- CS CS t- CS 11 H M CS CO to CO CO * ^ •"C CO tp V CO 0 CO CO TP 0 T CO CO CO CO co 0 £ 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 d *•' 0 d 0 0 0 0 0 0 0 0 0 ^ CO CO CO t- 10 <0 co 10 CS CO 0 CS CS 1 CS Ii CO K t- n Ii 0 IC 05 0 V 05 00 CN CO TP CO f» CO t-t CS IC CO TT CS IC t- t- 00 OS co co oo t- co 1 0 ii 0' 0 •"< 0° 0 O 0 ll 0 0 0 0 -H 11 0 •1 CS 1-i 0 0 0 0 0 0 ** 0 0 CS 0 10 CS 0 00 CO 00 CS i-t ^ 00 h- 00 co CO r- •vn 0) t" IC 0 CS 00 co Ii IC 0 >< CO f-H co IC 00 IC 10 CO 00 pH Iii IC 00 10 00 0 IC 00 os CO CO CO IC K IC 0 CO CO CO 1 0 1"< 0 O 0 0 0 0 0 rH 0 O 0 0 0 11 0 0 Ii 0 0 0 0 0 0 0 n 0 0 « 0, 0 CO CS •»r rH U5 10 Ol TP IC 0 IC CO CO 0 TP CS 00 00 CO IC h CO CO CS 0 0 CO t- IC IC 10 N tp IC IC IC IC TP t-; t- t- 10 IC Oi CO CO CO V 00 0 "i CO CO ö 0 Ö O O O 0 0 d O O O 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 Ö 0 0 DQ CQ 0 < < < D a a m - CD CD a a c^- a a a a ¡¿"WS ü ü dq ü Q Q o o Sq0Qi05 Q Q 55 Q On Q Q Q Q in S QÄwSScCSjQS SOfflQSQSüOO SQDSQSQSoiü m 35 o > cd CD rM o > ^ FFI > ü A o a < dl o a cd tä . 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T ? i ? o o' c* 0 (OOHMONHOOW OOOQ'-t'-*QQO'-t i oooooooooo 0000000000 £ 6666666606 6606666606 oooooooooo ST ooNiowotqtßtovto ooHHodddo'd oooooooooo oooooooooo 1<9 m<<< »®nno«Hni-H oioNrtLoiooifl'r-co aOOOOQiOOOUl^NlMffiWOlQNOlCCOOt TIDtDfflONOOlOOO» oiO^rtTt-oo^i-^fO 00 00 00 00 00 00 0>0)0>0 t-I i-l r-l I t-H i-< OIOOOOOO — CNCNCNCSOiCSCNC^CSCN QQQQQQQQQQ QQQQQQQQQQ QQQQQQQQQQ XIIIIIISIX rnr^rnrnr^irrP^rnr^iP*! IIIIIIIUI HNfOTTifttONOOdd HfiniioiohBoio t- r- r- t- r- c- f- I- fOCOCOCOCOfOCOCÖCO'^' 50 A. Bartkevicius and R. Lazauskaitè OOHOA^OIAOO suiiotoisNoaion ST nvuìieiANStooioi) dsoHsosdoo 6000000000 0060000000 OHNlöWNMtO HHnwwMPjcin« H()t«Ht)ÏNHC(N g I osddoodsdd 000'0000000 6666660666 w O oiaov^tDHHsoiooi M«";««««««* «»nfiTinnfiw MWrtcortiococ^coco oéooóodddo o o'00000000 6660660666 HflOffHh.tDrtrtHl' itNioiiii'ingiieios viflfloaow'inißNw o o^^OÒOÒH H ¿«¿OHHOddö odddoHHHHrt 0 u5 looiicaoíTsnoi t-onOHTtrtVi« dddddddddd 0000000000 6666666660 M a s X ÛÛ Û O a. Q 8 yo uyy.QQyÛ y ay uQq Xx <<9y o SaiOQmSSSûS biSQQOOQmSm SûûûûoSû >>f-4 N. >^H « •SB. > >>> . o> > M O * 00 > Ch > S o > O n Cl* sööü rk 2 u ¿ i w 1 ^ 1 i i ^ ^ DliQgSQDûCû Sgñ^SSsgQQ ««(INS flS'Ooofci fcSOfcülüOSSS < [fa O O O DB 2 * S S nwhwNooiOHifl uîOflOrtNwhnoiq »»stoiOTniooo; ""rioNi'iow^fd^ rifiíriNfíujriióv m t~ — csomoopîowoo <0 HrtH Vfr-lOtO ? s. CSi-fQOQOQQC^ '»00000000 i qqqqoqqqo §.qqoq000—0 0606666660 OOOOOOOOOO 0666666660 è HioicooNioœœsn OSTfl/JtOrHtOCOÇOOïa) N»inu>(OoossoN 6666666660 OOOOOOOOOO 6066606 o — o C Nn^iflONOOOlO ^CSCO^iO^t-OOCíO NSNS(-NSSt-Jl NI-t-l^t-l-Nt-KK Classification of Population II Stars _ <2 00 10 0 0> CO <0 05 co CS CS O N 00 T 05 U5 0 05 CS co 1/5 10 t- 1/5 co cq U5 co CO U5 1/5 U5 CO co 1/5 co * co 00 •w CO U5 10 0 0 0 0 O O O 0 0 O 0 O 0 o O O ö 0 O 0 0 0 O 0 O 0 O 0 0 so CS es O 1/5 co 0 0 CS co •V I-H CO es ri t- 00 CO O 00 1/5 CO CO i- 05 ^ 05 <0 CS CS CS co CS CS CS co CS r-> CS CO CS CS CS cs CS CS CS CS • »0 co V co U5 CS "5 CO CO CS 1/5 U5 co CO CO 1/5 CO 00 N • »ß r- CS 00 CS iH 0 0 CO »/5 05 K CO 05 00 00 N 0 CO 05 ^ 1/5 1/5 0 o> CS 0 ST 0 05 00 N es 00 05 K I-« 00 U5 00 CS 00 N t- 05 00 05 to CS 00 U5 0 CO i ** O 0 O 1-H 0 0 0 i-l 0 O 0 O O 0 O O O 0 O 0 I-H O 0 -- 6 s^rtrtPjftHfloejo 00 - 0000000000 0000000000 o 100 — 00000 0000000000 6660666660 6666666660 CS Di DD a U U H ^^ 3 Q 00 O vi Q QQO 03 ; H H " O l* a 1 oQ QQ max q 9 9 9 s QÖDSq QQ>>Q O SaDciOmSaSS fflraüamSSSQa: ¿EliOicnQcnaiCdaicß 03 B OS es es B 1— <0 o o U 1 u >e s o> dl Sei « HJ. „üifcoo ü 10 > s'5 0 ^ v « o OOol ü ü h SS 10 >n 1- I I 00 ü Dr. Q Q a tOQgädiiQgQ ^ J- cn SOUOÖ^SSSS SS «>• ^ s* 73 73 'S'SSoSS'SSüS ool cofr^ososeococoojcoco cc*/5Tro**i/5cßeocsu5 pjuidu'j'i^wduid £ ^ u: iß es rV o o O ^ ^H ??? I I I El,. OOOWTTOOOOO OOC^oinoocso^ cowwoooonnn 0000000000 0000000000 ocooooooe^c^o 00'0000'0000 ddddddoood 0000000000 I £ o ««(COTrtrtWHS COCO^^t-COCOiftt'-io 0066060600 0000000000 ,00000000 CO CO < < o o I-I TT 00 TT CS o 00 o <- t- i- a rH l-t d h- t- H t- N ^ to v N (p (O IO I~c0c00»00cs00u5u500 N O 0) "5 h- CS U5 N CO 00 5s N 1/5 00 «0 CS O O 1-1 t» CO <0 05 _ rtuntflotäsoo fl) 05 05 H m 00 h n ia 9) i-< M Ol O co v 00 O O m ^j« ^r m i)N«nnN n n n w 00 00 co T » f «WWMNMNWWN N W N CS ^ CS CS CS CS CS CS CS C* CN NNW W M rt CSCSCSCSCSCSCSCSCSCS N N N N "aBBaa H H Cd a a tc a uuu QQQQQQQOQQ aaaQ QQQQQD QQQQ QQQ IXXXXXXXXX B B B B B B B BS B xxxx BBS BEB rtMCO^ifltONCOOlO OOOOOOOOOOOOOOOOOO 05 0505050501050)0505 O OOOOOOOOO^ NNNNt-NSSt-OO oooooooooooooooooooo A. Bartkevicius andR. Lazauskaitè o ST oiHtcoivowwo)»-! MV »N NP) Ut ) «* O"l OHHodoooort 060000' sr oontct-^H oooooooooo 0060000 ntoiovnn^^Sv HHNflWCÇiß 01 ^r 00 00 M Hto 0000000000 6666660 0 ST (ostos«»iosst 1 OMHOódóódH * 0000000 SOOHOOH'fOlBN ooion^noTf t- <0 <0 <0 <û )0 0 0-1-1000000--1 0000000 ce ti ce ce H H H H ti a XXX X H s O HH(iU S CD hol û. ->ÛÛÛÛÛÛ D ti ce ti ti oc X O -QQISaicni/iaicncft D ti o£ c¿ ce ti 00 r* Ol V t-; 01 FH O 1 o FHI WI CI* I »I- rHi T11O f"" ** 1** ' 00 co co co co co »-i IM o o o o o o oooooooooo 6666060 ciroieuisSHioios uicOHiûio^Nifluiq OHHoddodoH OOOOOOO 00000 II II II II II S-a.S.S-9- JS^t-oootSSmcoS HfJO»»ttt«0 «1 b h h h U HHCO^HUIUIOIH >s j>.>.> j j . j> > j>.2 o? Shhhhhhhhh 3 ti Si Di ti ï ¡o S H H B h H H fri H h ti ti ti ti ti ti cs> o rtl-ll-HFHl-lF-HNPÎVmtûhOOft — — rtP»O i-i fi cö V "> 6 t- Z ooooooooooœoooooooo Ctf00 00l N00 N00 P00I «00 0«0 Classification of Population II Stars 53 Notes (abbreviations explained see in Table 7) 13. BD +04°4551AB VBP-MD. VB: IDS 20438N0450AB, 9.0, 1.2. 14. BD +04° 5012 Var: VZ Psc, EW/KW, P 0.261 d, V 10.20-10.45. 18. BD +06° 4990 Var: DH Peg, RRC, P 0.25551040 d, V 9.15-9.80. 24. BD +09°4955 ARCT. 25. BD +10°6 VB: IDS 00045N1112A, 288, 0.2. 27. BD +10°2495 SB. 29. BD +11°4381 Var: DX Del, RRAB, P 0.47261673 d, V 9.52-10.26. 35. BD +13°3683 SB: P 40.27 d, K 24.4 km/s. 40. BD +18°2757 Var RV. 41. BD +18°2776 VB: IDS 13402N1781A, AB: 66.1, 1.4, AC: 464.1, 0.7. 42. BD +18° 2890 SB. 43. BD +18°2976 Var RV. 44. BD +18° 3423 VB: IDS 17344N1837C, AB: 267.9, 1.3, AC: 372.8, 0.5. 45. BD +20° 3603 KAPT. VB?. 46. BD +21° 4633 Var: AV Peg, RRAB, P 0.3903747 d, V 9.88-10.92. 48. BD +22°4409 W630 group. 55-58. BD +24°4742 VBP-MD. Var: EZ Peg, NL:, RS. SB: P 11.6598 d, Kl Ii2 24.3 km/s, G5V+G5V. 60. BD +25 1981 KAPT. 66. BD +27°2891 ARCT. VB: IDS 17437N2750A, 77.5, 5.2. 69. BD +29°366 PUP. VB: IDS 02046N2921A, AB: 103.7, 3.2, AC: 158.4, 2.7, AD: 213.4, 1.8. 75. BD +32°4645 VB: IDS 23215N3126A, 261, 1.5. >—91. BD +38° 2803 Var: UU Her, SRD - Prototype of the UU Her var. P 80.1 d, PG 8.5-10.6. 93. BD +39°4926 Var?: F 9.25-9.28. 101. BD +46°4128 Var: WY And, SRD, P 108 d, PG 9.5-10.9. 102. BD +48° 739 ARCT. 105. BD +57°2161 Var? 108. BD +68° 946 VB: IDS 17370N6826B, AB: 181.4, 1.4. 111. BD +71°851 VBP. VB: IDS 17401N7122AB, 13.2, 3.8. 116. BD +76° 524 VB: IDS 14236N7635A, 131, 2.3. 118. BD +84°19 Var: RU Cep, SRD, P 109 d, V 8.2-9.8. 119. BD -00°4234 VBP-MD, RS. VB: IDS 21270S0013A, 133.5, 3.7. SB: P 3.7565 d, A'l 43.2 km/s, K2 53.7 km/s, K3Ve+K7Ve. Var: RS/BY?. 120. BD -00°4470AB KAPT, VBP-MD. VB: IDS 23045N0012AB, 9.3, 0.8. 129. BD -03°5215 VB? 131. BD -07°86 Var RV? 137. BD -09°6150 VB-MD. VB: IDS 23088S0929B, AB: 22.9, 1.1, AC: 102.7, 3.1. 54 A. Bartkevicius and R. Lazauskaite Notes (continued) 144. BD -12 134 VBP-MD. Central star of the planetary nebulae NGC246. VB: IDS 00420S1185AB, 3.8, 2.4, sdO+G? 145. BD —13°3834 KAPT. 152. BD -15°872 Var: RX Eri, RRAB, P 0.58724622 d, V 9.17-10.10. 158. BD -18°271 Var RV. 165. BD —22°395 Var RV. 173. CD -29°15254 SB: P - long. 176. CD -30° 19358 SB? 182. G 3-13 KAPT. 184. G 5-36 KAPT. 188. G 18-54 KAPT. 190. G 28-40 VB: IDS 23031N0837A, 15.5, 3.5. CPM. 191. G 28-42 Var RV? 195. G 29-44 Var? 196. G 29-71 SB. 206. G 78-26 KAPT. 210. G 99-8 VB: IDS 05228N0006A, 83.1, 1.2, CPM? 218. G 175-34B VBP. VB: IDS 04224N5849, 6.8, 1.35, P 350: yr. 220. G 184-48 VB-MD. VB: IDS 19209N2044A, 113.1, 0.01. 221. G 184-49 VB-MD. VB: IDS 19209N2044B. 225. G 191-B2B VB-MD. VB: 73, 1.70. 228. G 226-29 Var: DN Dra, ZZA, P 109s, A V 0.01. 236. G 270-52 Var RV? 245. HD 249 PUP. 246. HD 352 VBP-MD. SB: P 96.439 d, K 24.3 km/s, blue companion?, ¿ = 0.002, Am 2.0. Var: EB?, AV0.2. Composite: gk+F. 247. HD 432 VB: IDS 00038N5826A, 31.3, 11.3. SB: P 27 d, optical companion. Var: p Cas, DSCTC, P 0.10430 d, V 2.25-2.31. 253. HD 1835 VB: IDS 00177S1246A, 102.1, 5.4. 260. HD 2925AB VB: IDS 00274N2238AB, AB: 3.7, 4.8, AC: 17.7, 5.5, AD: 95.2, 2.2. 261. HD 3008 Var RV. 263. HD 3266AB ARCT, VBP-MD. VB: IDS 00307N2927AB, AB: 6.0, 0.8, AC: 32.3, 2.4. 265. HD 3457 PUP. 266. HD 3512A VB: IDS 00330S0063A, 30.5, 3.9. 268. HD 3567 Var RV? 269. HD 3627 VB: IDS 00340N3019A, AB: 28.7, 9.5, CPM, AC: 41.4, 12.2, optical. SB: P 15000 d, I< 4.0 km/s. 270. HD 3628 SB. Var: V 7.30-7.35. Classification of Population II Stars 55 Notes (continued) 271. HD 3651 VB: IDS 00341N2043A, 122.0, 4.9. Var RV. Var: V 5.83-5.89. 272. HD 3690AB VBP-MD. VB: IDS 00347N2053AB, 6.5, 2.7. 273. HD 3715 VB?: IDS 00348S1451A, 40.2, 1.5. 279. HD 4307 VB: IDS 00405S1285A, 69.5, 6.3. 280. HD 4374 VB: IDS 00411S0571A, 14, 8.6, CPM. 282. HD 4628 VB: IDS 00431N0446A, 181.2, 4.6, optical. 283. HD 4744 AECT. VB: IDS 00444N2954A, AB: 114.7, 1.6, AC: 119.1, 2.7, CR: 19.6, 0.8. 286. HD 5268 Var RV. 288. HD 5351 PUR 290. HD 5780 VB: IDS 00543N0015A, AB: 29.2, 0.4, BC: 179.6, 1.8. 292. HD 5917 VB? 294. HD 6186 VBP-MD. VB: 0.0, 0.2 298. HD 6474 Var: V487 Cas, SRD, P 134 d, V 7.44-7.74. 299. HD 6497 ARCT. 300. HD 6582 VB: IDS 01016N5427Aa, Aa: orbit: a 0.186, P 21.43 yr, AB: 423.8, 5.8, AC: 204.1, 5.8, CD: 4.2, 1.7, AP: 280.6, 7.0. SB: P 8393 d, K 2.8 km/s, Am 4.5. 301. HD 6734 ARCT. 302. HD 6755 SB. 304. HD 6860 VB: IDS 01041N3505A, AB: 27.0, 12.0, AC: 94.8, 10.5, AD: 80.4, 9.7, BQ: 24.6, 0.7. Var?:2.01-2.10. 307. HD 7672 VB: IDS 01115S0301A, 177.8, 5.7. Var RV. Var: AY Cet, RS, V 5.35- 5.58. Composite: G5IIIe+DA. SB: P 58.8147 d, K 7.2 km/s. 309. HD 7983 (U, V)(-130, -70) group? VB: IDS 01140S0886A, 205.4, 1.7. 310. HD 8724 KAPT. 312. HD 9826 VB: IDS 01310N4054A, AB: 114.0, 8.2, AC: 280.2, both components optical? SB?: P 197.9 d, K 1.8 km/s. 314. HD 10700 VB: IDS 01394S1588A, 89.8, 9.5. 315. HD 11397 ARCT. 316. HD 11636 SB: P 106.9973 d, A'l 37.1 km/s, K2 66.6 km/s. Var?: V 2.56-2.70. 317. HD 11909 SB: P 1567.66 d, K 10.8 km/s. 318. HD 12235 Var? Var RV? 319. HD 12929 SB. Var?: V 1.98-2.04. 321. HD 13783 VB: 65.4, 8.5. SB. 322. HD 13826 Var: V Ari, SRB, P 771 d, PG 9.8-10.8. 323. HD 13974 VB: IDS 02108N3346A, 65.3, 8.5. SB: P 10.0201 d, K 9.4 km/s. 324. HD 13979 KAPT. 325. HD 14056 PUP. 56 A. Bartkevicius and R. Lazauskaite Notes (continued) 330. HD 16160 VB: IDS 02307N0626AP, AB: 164.6, 6.1, B: dM6, CPM, AP: 2.5, 5.0, P 50 yr. SB. 331. HD 16234 VBP-MD. VB: IDS 02312N1200AB, 0.021, 0.1. 332. HD 16397 SB. 333. HD 16458 Var RV? 334. HD 17820 ARCT. 337. HD 19510 KAPT. Var: X Ari, RRAB, P 0.6511426 d, V 8.97-9.95. 338. HD 19735 ARCT. VB: IDS 03055N4721AB, AB: 7.4, 7.9, AC: 21.2, 6.3, AD: 212.2, 3.9, DE: 19.9, 2.7. 339. HD 19931 Var: SV Eri, RRAB, P 0.7137964 d, V 9.56-10.23. 340. HD 20084 VBP-MD. SB. Composite: G3IIp:+F0:V. 341. HD 20512 VB: IDS 03129N1451A, AB: 138.9, 8.13, CPM. 342. HD 21018ABVB: IDS 03184N0432AB, 1.0, 5.7. SB. 343. HD 21019AB VB: IDS 03185S0769AB, 3.9, 6.4. 345. HD 21120 SB: P 1645.9 d, K 4.4 km/s. 346. HD 21543 PUP. 348. HD 21674 PUP, VBP-MD. VB: IDS 03249N2916AB, orbit: a 0.35, P 184, Am 0.7. 349. HD 22225 ARCT. 350. HD 23249 Var? 351. HD 23441 VBP. VB: 0.1, 0.0. Var RV. 354. HD 23642 VBP. SB: P 2.4611 d, A'l 98.1 km/s, A'2 140.6 km/s, Am 1.11, 1.4, A0V+A5. 358. HD 25408 Var: UV Cam, SRB, P 294: d, V 7.5-8.1. 359. HD 25532 KAPT. 360. HD 25878 Var: XX Cam, RCB:, B 8.09-9.8. 361. HD 26976BC VBP. BC: BD-0700781. VB: IDS 04108S0749BC, AB: 88.4, 5.2, BC: orbit: a 6.8945, P 247.92, A V 1.64, AD: 485.5, 8.4, AE: 573.8, 8.7. 362. HD 27108 Var? 363. HD 27370 ARCT? 366. HD 28527 VBP. VB: IDS 04249Nl558Aa, Aa: 0.02, 0.0, AB: 250.3, 1.9. 370. HD 30353 SB: P 360.47 d. Var: KS Per, P 30: d. 372. HD 30649 PUP. VB: IDS 04444N4541A, 101.7, 5.3. 373. HD 32147 SB. 375. HD 33564 VB: IDS 05061N7907A, AB: 25.5, 4.0, AC: 208.6. 376. HD 33708 ARCT. SB: P 3683 d, K 5.2 km/s. 378. HD 34411 VB: IDS 05121N4001A, AB: 106.1, 8.6, AC: 87.3, 7.3, AD: 201.6, 3.8, DE: 145.3, 1.3, AF: 92.9, 5.3, EG: 33.1, 0.2, EH: 146.8, 0.8. 379. HD 35296 SB. VB: IDS 05186N1716A, 104.6, 3.8. Classification of Population II Stars 57 Notes (continued) 381. HD 36283 ARCT. 382. HD 37160 PUP. 383. HD 41870 Var: SS Gem, RVA, P 89.31 d, PG 9.3-10.7. 384. HD 43039 Var?. 385. HD 44007 KAPT. 386. HD 46588 SB: P 60.0 d, K 1.7 km/s. 387. HD 46703 Var:V382 Aur. 393. HD 59643 Var: NQ Gem, SR+ZAND, P 70: d, V 7.4-7.99. 395. HD 62509 VB: IDS 07392N2816A, AB: 35.1, 12.5, AC: 249.3, 7.7, CD: 1.4, 1.8, AE: 281.6, 8.5, AF: 305.5, 9.2, AG: 152.0, 11.8. Var?: V 1.10-1.17. 397. HD 73394A Var RV. VB-MD. VB: IDS 08330N5206A, AB: 49.1, 3.5, BC: 6.4, 1.2. 399. HD 74721 ARCT. 401. HD 76644ABC VBP. VB: IDS 08524N4826ABC, Aa: orbit: P 11.02, A-BC: orbit: a 9.092, P 817.91, BC: orbit: a 0.68, P 639.69. SB: Aa, P 4028 d, K 6.0 km/s. 402. HD 79096 VBP. VB: IDS 09068N1524AP, AB: 35.6 , 6.8, AC: 206.6, 4.2, AP: orbit: a 0.126, P 2.65, A V 0.0. 403. HD 79452 VB: IDS 09091N3503A, 139.9, 3.5. 405. HD 81192 PUP. 406. HD 84035 Var?: V 8.12-8.16. 407. HD 84937 Var RV? 408. HD 86728 VB: IDS 09553N3225A, 407, 3.2. 410. HD 88230 VB: IDS 10053N4958A, AB: 152.4, 2.2, BC: 303.0, 1.1. 413. HD 91612 Var RV? 414. HD 92168 SB: P 7.7991 d, K 24.1 km/s. 416. HD 97603 VB: IDS 11088N2104A, AB: 191.2, 6.0, AP: 95.4, 9.5. Var?: V 2.54-2.57. 417. HD 100470 PUP. SB. 418. HD 100971 KAPT. Var: SU Dra, RRAB, P 0.66042001 d, V 9.18-10.27. 419. HD 101501 VB: IDS 11357N3446A, 159.3, 4.9. 420. HD 102647 VB: IDS 11440N1508A, AB: 39.8, 13.5, AC: 80.3, 11.0, AD: 240.9, 6.3. 421. HD 102870 VB: IDS 11454N0219A, AB: 245.5, 6.8, AC: 423.2, 5.0. 422. I ID 103036 KAPT. Var: TY Vir, SRD, P 50: d, V 7.97-8.5. 423. HD 103095 VB: 1.7, 5.5. Var: B component, CF UMa, UV?, mpv 8.5-12. 425. HD 104979 Var RV? 429. HD 106591 Sirius group. VB: IDS 12105N5735A, AB: 189.7, 6.6, AC: 186.5, 8.2. Var?: V 3.27-3.34. 430. HD 107328 PUP. VBP-MD. VB: IDS 12152N0352Aa, Aa: orbit, a 0.6, P 0.0, AB: 132.2, 6.5. SB. Var?: V 4.94-4.99. 58 A. Bartkevicius and R. Lazauskaitè Notes (continued) 432. HD 109358 VB: IDS 12210N4154AB, SB: P 2429.9 d, K 2.6 km/s. Var: RS, A V 0.05. 433. HD 109995 KAPT. 438. HD 111908C Var RV. VB: IDS 12474N0745C, AB: 37.9, 0.0, AC: 35.6, 1.1. 439. HD 112869 Var: TT CVn, SRB, P 105 d, B 10.4-11.11. 440. HD 113226 Hyades group? VB: IDS 12572N1130A, 248.7, 8.9. 442. HD 114710 VB: IDS 13072N2823A, 90.8, 5.8. SB: P>5 yr. 443. HD 115383 VB: IDS 13118N0957A, 34.3, 9.1. 445. HD 117043 Var. 449. HD 121370 VB: IDS 13499N1854A, 111.7, 6.0, SB: P 494.173 d, K 8.4 km/s. 451. HD 122563 Var?: V 6.17-6.21. 452. HD 122742 VB: a 0.1. SB: P 9.907 yr, K 6.9 km/s. 454. HD 124897 ARCT. Var: V -0.13 - -0.03. 456. HD 125162 Var?: V 4.15-4.19. 457. HD 126053 Var RV. 460. HD 126660 W630 group. VB: IDS 14218N5219A, 69.6, 7.0. Var?: V 4.02-4.07. 462. HD 127665 VB: IDS 14275N3049A, 35.7, 7.7. Var?: V 3.56-3.62. 463. HD 128167 VB: IDS 14304N3011A, AB: 237.1, 5.3, AC: 237.0, 6.8. Var?: DSCT, V 4.45-4.49. 466. HD 129502 SB: P 358: d. 468. HD 131511 SB: P 125.369 d, K 19.5 km/s. 469. HD 134083 UMa stream, Sirius group. VB: IDS 15029N2515A, AB: 107.4, 5.8, AC: 244.0, 4.9, Var?: V 4.92-4.96. 471. HD 134439 VB-MD. VB: IDS 15047S1553A, AB: 29.6, 2.3, AC: 449.5, 0.6, AD: 301.7, 0.4. 472. HD 134440 VB-MD. VB: IDS 15047S1553, AB: 29.6, 2.3, AC: 449.5, 0.6, AD: 301.7, 0.4. 473. HD 135148 SB. 474. HD 135722 VB: IDS 15115N3341A, 104.9, 5.2, CPM. Var?: V 3.44-3.50. SB: A. 475. HD 137391 VBP. VB: IDS 15207N3742A, AB: 108.3, 2.7, A: Var?: DSCT, V 4.29-4.34, BC: orbit: a 1.463, P 260.10, Am 0.6. 479. HD 140573 VB: IDS 15393N0644A, AB: 58.0, 9.0, B: optical, AC: 136.0. 480. HD 141004 SB?: P 1837 d, K 2.8 km/s. Var?: V 4.39-4.44. 481. HD 141527 Var: R CrB, RCB, V 5.71-14.8. 482. HD 142267 VB: IDS 15485N1331A, 98.4, 5.6. Var?: K6.06-6.il. SB: P 138.603 d, K 6.0 km/s. ' 484. HD 142780 Var?: A V 0.12. 485. HD 142860 VB: IDS 15518N1559A, AB: 201.6, 6.6, BC: 177.1, 0.4. Var?: V 3.79-3.88. Classification of Population II Stars 59 Notes (continued) 487. HD 144579 PUP. VB: IDS 16013N3926, Am 9.2. 489. HD 144921 Var: SX Her, SRD, P 102.90 d, PG 8.6-10.9. 490. HD 145148 Var RV. 494. HD 146233 VB: IDS 16102S0806A, 25.8, 7.7, optical. Var?: V 5.48-5.59. 495. HD 147379 VB: IDS 16166N6729A, 63.3, 2.0. 497. HD 148897 W630 group. Var RV? Var?. 499. HD 149661 VB: IDS 16310S0207A, 100.4, 7.7. 506. HD 153687 VB: IDS 16557S0404A, 93.4, 4.0. 507. HD 154276 ARCT. 508. HD 154278 7 Leo group. VB: IDS 16590N1345B, AB: 305.3, 0.2, BP: 152.4, 3.9, PQ: 98.5, 0.5. Var RV?. 510. HD 154417 Var RV. 511. HD 156164 VB: IDS 17109N2457AB, AB: 8.9, 5.1, AC: 159.0, AD: 190.9. SB. 513. HD 157214 VB: IDS 17169N3236A, AB: 230.0, 4.3, BC: 8.7, 3.2. Var: A, V 5.38-5.45. 516. HD 158226 ARCT, VB-MD. VB: IDS 17230N3109A, 67.8, 1.1. 517. HD 158633 SB. 519. HD 159222 6 Cen group. 521. HD 159482 VB: IDS 17299N0606C, AB: 26.3, 3.0, AC: 88.9, 0.5, CD: 180.2, 2.9. 522. HD 159561 UMa stream, Sirius group. VB: IDS 17303N1238Aa, orbit: a 0.065, P 8.5. SB? Var?: DSCT?, V 2.02-2.13. 526. HD 161096 Possibly close double. Var RV. 529. HD 161797 VB: IDS 17425N2747A, AB: 34.0, 6.7, BC: orbit: a 1.360, P 43.20, Am 0.5, AD: 256.1, 7.7. 530. HD 161817 Var: V 6.94-6.98. 531. HD 163506 Var: V441 Her, UU HER, P 70 d, V 5.34-5.48. SB? 532. HD 163810AB VBP-MD. VB: IDS 17530S1304AB, 0.45, 2.3. 533. HD 164058 VB: IDS 17543N5130A, AB: 19.4, 11.0, AC: 43.8, 10.5, AD: 59.3, 10.5, AE: 95.4, 9.5, AF: 125.1, 8.8, AG: 142.0. 535. HD 164922 VB: IDS 17584N2620A, AB: 31.5, 5.7, AC: 80.3, 3.9. 537. HD 165401 PUP. 538. HD 165634AB VBP-MD. VB: 0.8, 0.3. 539. HD 165908AB VBP-MD. VB: IDS 18032N3033AB, AB: orbit: a 1.00, P 55.8, AC: 93.5, 5.4. 541. HD 166181 H, K emission. SB: P 1.8098 d, K 54.6 km/s. Var: RS, AK0.1. 543. HD 166620 W630 group. Var?: V 6.38-6.42. Var RV?. 544. HD 167768 ARCT. Var RV. 546. HD 168656B VB: IDS 18159N0320B, AB: 28.2, 6.6, AC: 57.7, 7.0. 547. HD 168723 VB: IDS 18161S0255A, 179.8,8.7. Var?: V 0.91-1.28. Var RV?. 60 A. Bartkevicius and R. Lazauskaitè Notes (continued) 549. HD 170737 PUP. SB: P 1284 d, K 6.4 km/s. 550-554. HD 170756 Var: AC Her, EVA, P 75.01 d, V 6.85-9.0. 555. HD 171314 Var: V774 Her, UV, B 9.45:-10.90:. 557. HD 172167 VB-MD. VB: IDS 18336N3841A, AB: 76.7, 9.4, AC: 81.3, 10.9, CD: 33.5, AE: 91.3, 9.4. 559. HD 173399 VB: IDS 18400N4450A, 26.4, 1.5. 560. HD 173667 VB: IDS 18414N2027A, AB: 59.0, 8.3, AC: 73.2, 6.7, AP: 12.6, 9.7, AQ: 58.6, 9.4. 561-562. HD 173819 Var: R Set, RVA, P 146.5 d, V 4.2-8.6. 564. HD 174638 VBP-MD. VB: IDS 18464N3315A, AB: 45.4, AC:46.6, AD: 64.2, AE: 67.8, AF: 85.2, SB: A: P 12.9349 d, K 184.0 km/s, also P 4.2 yr, B: P 4.34 d, K 12.0 km/s. Var: EB, P 12.913834 d, V 3.25-4.36. Composite: B7Ve+A8p. 566. HD 174974 VB: IDS 18481S2252AB, AB: 2.5, 5.8, AC: 27.4, 5.8. Composite: CK2+B0V:. 568. HD 175190 SB. 569. HD 175225 Var RV? 570. HD 175305 ARCT. 571. HD 175545 ARCT. 576. HD 177758 ARCT. VB: IDS 19009S1203AB, 1.5, 6.1. 579. HD 181007 KAPT. 580. HD 181615/6 VBP-MD. VB: 0.011, 1.0. SB: P 137.9567 d, K 49.1 km/s. Var: EB/GS, P 137.939 d, PG 4.53-4.61. 581. HD 181984 SB. Var? 584. HD 182572 71 Cyg group. VB: IDS 19202N1143A, AB: 99.6, 3.5, AC: 143.0, 5.4. Var?: V 5.10-5.19. 589. HD 184406 VB: IDS 19292N0710A, AB: 53.0, 8.5, AC: 53.8, 8.5, AD: 84.1, 8.0, AE: 166.6, 5.1, AP: 45.2, 8.3. 590. HD 184467 VBP-MD. VB: IDS 19295N5824AB,d= 0.1. SB: P 491.9 d, Kl 9.5 km/s, K2 10.5 km/s. 592. HD 184700 ARCT, VB-MD. VB: IDS 19306S0027A, 113.1, 2.3. 593. HD 184711 VB-MD. 594. HD 184768 ARCT, VB-MD. VB: IDS 19309S0007AB, AB: 3.3, 6.2, AC: 109.2, 4.0. 595 . HD 185144 VB: IDS 19325N6929A, 315.4. 596, HD 185657A VB: IDS 19352N4903A, AB: 24.8, 2.9, AC: 55.9, 2.9, CD: 10.5, 5.3. 600, HD 186408 VB: IDS 19392N5017A, AB: 39.6, 0.24, AC: 70, 7.17. 601, HD 186478 SB. 602, HD 187013 VB: IDS 19426N3330A, AB: 25.4, 4.2, AC: 112.0, 4.0, Var RV?. 606. HD 187642 VB: IDS 19459N0836A, AB: 189.9, 8.7, AC: 238.1, 9.2. Classification of Population II Stars 61 Notes (continued) 608. HD 188512 VB: IDS 19504N0609AB, AB: 13.0, 7.4, Var?: A component, V 3.68-3.74. 612. HD 189558 ARCT. VB: IDS 19555S1231AB, 6.9, 6.2. 613. HD 189711 Var?: V 8.37-8.48. 617. HD 190390 VB: d=25, Var RV?, Var?: BV592, A V 0.4. 619. HD 190712AB VBP-MD. VB: IDS 20012N7911, 9.1, 1. 620. HD 191026 VB: IDS 20026N3541A, AB: 12.0, 4.0, AC: 23.3, 8.2, AD: 36.2, 6.1, CPM. 621. HD 191046 ARCT. 624. HD 192310 Var?: V 5.72-5.76. SB. 625. HD 192455 VB: IDS 20100N6147A, 93.1, 9.4. 626. HD 192640 VB: IDS 20108N3630A, AB: 216.7, 1.6, AC: 214.3, 5.0, AP: 35.7, 7.2. Var: V1644 Cyg, DSCT, P 0.031 d, V 4.94-4.97. 627. HD 193242 KAPT. 628. HD 193664 Var RV. 630. HD 194012 Var RV? 631. HD 194598 KAPT. 633. HD 195636 SB. 634. HD 195987 SB: P 57.3210 d, K 28.8 km/s. 635. HD 196610 Var: EU Del, SRB, P 59.7 d, V 5.79-6.9. 636. HD 196882ABPUP, VBP-MD. VB: IDS 20351N2122AB, 9.3, 1.8. 637. HD 197076 Hyades group. VB: IDS 20362N1934A, AB: 93.7, 5.1, AC: 125.0, 7.0. 638. HD 197177AB VBP. VB: IDS 20370N3157AB, AB: 2.7, 2.1, AC: 68.3, 5.9. SB. 641. HD 197989 VB: IDS 20422N3336A, AB: 54.8, 9.0, optical, AC: 77.9, C: CPM. SB. 642. HD 198084 VB: IDS 20429N5713A, 50.1, 5.7, optical. SB. 644. HD 198300 VB: IDS 20443N5929AB, 1.1, 5.1. 645. HD 198809 SB. 647. HD 199305 VB: IDS 20513N6148A, AB: 101.7, 0.4, AC: 57.8, 4.6. 650. HD 199939 SB: P 581.4 d, K 8.0 km/s. 656. HD 202109 VB: IDS 21086N2949A, AB: 69.0, 8.2, AC: 90.4, 7.9, AD: 102.9, 9.2. SB. Composite: G8+III-IIIa+WD. 659. HD 202573 W630 group? 660. HD 202759 Var: AW Mie, RRC:, P 0.479: d, V 9.04-9.13. 662. HD 203280 VB: IDS 21162N6210A, AB: 206.9, 7.8, BC: 19.9, 0.7, CD: 2.6, 0.2. Var: DSCT?, V 2.41-2.47. 663. HD 203454 VBP-MD. Sirius group. UMa stream. SB: P 3.2434 d, K 62.0 km/s. 664. HD 204075 VB: IDS 21210S2251A, 21.2, 8.6. SB: K 3.7 km/s. 675. HD 206778 VB: IDS 21393N0925A, AB: 81.8, 8.8, AC: 144.7, 6.0. Var: LC, V 0.7-3.5. 62 A. Bartkevicius and R. Lazauskaitè Notes (continued) 676. HD 206860 Variable H, K emission. Var RV? Var: HN Peg, BY, P 24.90 d, V 5.92-5.95. 678. HD 207098 VBP. VB: IDS 21415S1635A, AB: 69.2, 12.0, AC: 118.8, 9.7. Var: 6 Cap, EA, P 1.0227688, V 2.81-3.05. SB: P 1.0228 d, K 70.8 km/s, occultation binary: a 0.0018, Am 3.0. 682. HD 208110 SB: P 3400? d. 684. HD 208906 VB: IDS 21543N2921A, 29.8, 7.6. 685. HD 209621 RV -381 km/s. Var: HP Peg, LB, V 8.80-8.91. 686. HD 209813 Very strong H and K emission. SB: P 24.4284 d, K 34.6 km/s. Var: HK Lac, RS, P 25.83 d, V 6.77-7.04. 687. HD 210027 VBP? VB: IDS 22023N2458A, 103.7, 7.4, optical. SB: P 10.2130 d, K 49.1 km/s. 691. HD 210595 VBP-MD. VB: IDS 22063N2359AB, 0.3, 0.0. 692. HD 210884 VB: IDS 22084N6938A, 15.9, 2.0, CPM. 693. HD 211336 VB: IDS 22113N5633A, 119.6, 5.3. SB. Var: DSCTC, P 0.041242 d, V 4.15-4.21. 694. HD 212061 A Boo type star? VB: IDS 22165S0153A, 36.4, 8.2, optical. SB: unresolved by specie interferometry. 697. HD 213893 ARCT. 700. HD 214714A VB: IDS 22350N3704A, 18.7, 6.9. 701. HD 214925 Var RV. 704. HD 215648 W630 group. VB: IDS 22417N1139A, AB: 11.8, 8.0, AC: 145.0, 6.8. 709. HD 216385 VB: IDS 22474N0918A, 248., 8.4. SB. 710. HD 216777 VB: IDS 22506S0821A, 43.0, 7.4. 712. HD 217014 Var?: V 5.43-5.53. 715. HD 217877 Hyades group. 718. HD 218356 W630 group. SB. Var?: V 4.72-4.78. Composite:K0IIp+WD. 720. HD 218527 Var RV? 721. HD 218549 PUP. Var: DY Peg, SXPHE(B), P 0.072926297 d, V 9.95-10.62. 723. HD 218634 VBP-MD. VB: IDS 23045N0808A, 32.8, 4.6. SB. Var: GZ Peg, SRA, P 92.66 d, V 4.95-5.23. Composite:M4IIIs+A2V. 724. HD 218732 Var RV. 728. HD 219134 VB: IDS 23084N5637A, 266.7, 3.8. Var RV, Var: V 5.52-5.61. 729. HD 219175 VB-MD. VB: IDS 23088S0929A, AB: 22.9, 1.1, AC: 102.7, 3.3. SB. 731. HD 219449 VB: IDS 23106S0938A, AB: 49.2, 4.5, BC: orbit: a 0.6, P 130, A m 0.5, CPM with A, C: close double. AD: 108.8, 9.0, BE: 40.3, 5.3. Var RV. 732. HD 219615 SB. 733. HD 219617AB VBP-MD. VB: IDS 23119S1422AB, AB: orbit: a 0.48, P 90, A m 0.2, AC: 194.1, 3.1, AD: 93.3, 3.3. 734. HD 219623 VB: IDS 23121N5241A, 129.4, 7.3. Classification of Population II Stars 63 Notes (continued) 735. HD 219685 ARCT. 737. HD 219829AB VBP. VB: IDS 23138N0452AB, AB: orbit: a 0.768, P 91.8, Am 1.0, AC: 118.8, 1.0, AD: 221.1, 0.4, AE: 243.3, 0.8, CF: 24.3, 1.8. 738. HD 219834A VB: IDS 23139S1400A, 14.4, 2.0, SB: A component, P 2323.6 d, K 5.5 km/s. 739. HD 219877A Hyades group. VB: IDS 23142S0540A, 11.0, 4.9, CPM. SB: A. 740. HD 219953 PUP. 745. HD 220460 VBP-MD. SB: P 6.0499 d, Kl 48.2 km/s, K2 49.8 km/s. 748. HD 221148 Var?: Var RV. 752. HD 221377AB VB?: IDS 23266N5152A, 17.2, 2.8. 754. HD 221503 VB: IDS 23276S1723A, AB: 338.1, 3.6, BC: IDS 23275S1718, 0.5, 0.8. 758. HD 221830 VB: IDS 23305N3027A, 8.0, 7.6. 761. HD 221950 VBP-MD. VB: 0.011, 0.1. SB: P 45.49 d, Kl 40.1 km/s, K2 41.5 km/s. 762. HD 222107 VB: IDS 23327N4555A, AB: 47.6, 9.3, optical, AC: 217.7, 6.5, CD: 68.4, 1.0. SB: P 20.5212 d, K 6.6 km/s. Var: X And, RS, P 54.20 d, V 3.69-3.97. 764. HD 222368 VB: IDS 23348N0505A, 69.9, 8.7, optical. 765. HD 222404 Var?: V 3.18-3.24. 766. HD 222455AB VB: IDS 23356S0008AB, 3.7, 4.3. 770. HD 222794 VB: IDS 23386N5730A, AB: 156.6, 2.5, AC: 139.4, 2.5, AD: 216.2, 2.2, AE: 165.9, 2.5, AF: 269.8, 2.1. 775. HD 223498A VB: IDS 23449N0219A, 18.3, 5.0, optical. 777. HD 223778 VBP-MD. VB: IDS 23475N7459AB, AB: 4.6, 4.9, AC: 161.8, 2.7. SB: P 7.7531 d, Kl 39.9 km/s, A'2 49.7 km/s. 779. HD 224014 MDI-SRD. Var RV. Var: p Cas, SRD, P 320 d, V 4.1-6.2. 780. HD 224085 SB: P 6.7242 d, K 36.8 km/s. Var: II Peg, RS, P 6.7026 d, V 7.18-7.78. 784. HD 224342 Var RV. Composite: gK+F. 788. HD 224635/6 VBP. VB: IDS 23544N3310AB, AB: orbit: a 3.125, P 355, Am 0.2, AC: 81.2, 6.3. 791. HD 224927AB VBP-MD. VB: IDS 23567S2581AB, orbit: a 0.1, P 30, Am 0.4. Var RV. 792. HD 224930 VBP-MD. VB: IDS 23669N2633AB, AB: orbit: a 0.803, P 26.386, Am 3.04, AC: 173.2, 2.8, AD:191.9, 7.2, SB: P 26,27 yr, K 5.1 km/s. Var?: V 5.72-5.83. 794. HD 225185 VB: 23., 10.2, CPM. 797. HD 231510 VB: IDS 19236N1347A, 23.0, 1.2. 803. HDE 239124 Var: XZ Cyg, RRAB, P 0.46670 d, V 8.9-10.16. 804. HDE 250792A VB: IDS 05573N1922A, 7, 4.07. 64 A. Bartkevicius and R. Lazauskaite Notes (continued) 805. HDE 283750 Hyades group. VB: IDS 04305N2638A, 123, 7.52. 808-809. HDE 340667 Var: V Vul, RVA, P 75.7 d, V 8.05-9.53. 812. LTT 114 VBP. VB: astrometric binary, 0.14, 2.83. 816. LTT 1566 KAPT. VB: IDS 03135S0730A, 85., 3.9. 821. PU Vul Var: NC. 822. RR Lyr Var: RRAB, P 0.56686776 d, V 7.06-8.12. Classification of Population II Stars 65 Table 7. Abbreviations used in Notes of Table 6 Members of the moving groups: KAPT Kapteyn star group; GR1830 Gr 1830 star group; ARCT Arcturus star group; PUP <7 Puppis star group. Visual binaries: VB Visual binary; VB? Suspected visual binary; VB-MD Population II visual binary, observed separate components; VBP-MD Population II visual binary with <¿<10-15 arcsec and Am>4 mag, both components observed together; VBP Population I visual binary with d<10-15 arcsec and Am>4 mag, both components observed together; IDS Number from C. E. Worley, G. G. Douglass, The Washington Visual Double Star Catalogue, 1984.0, CDS Magnetic Tape S1107, Strasbourg. First numeral is the distance between components in arcsec, second numeral is the difference of magnitudes . When the orbit is given, the next numeral means the semi-major axis of the VB orbit in arcsec, number after P is the period in years. Spectroscopic binaries SB Spectroscopic binary; SB? Suspected SB, P is its period in days, K is the semiamplitude of the radial velocity curve in km/s. Other abbreviations: CPM Comon proper motion; Var RV Variable radial velocity; Var RV? Suspected variable radial velocity; Var Variable star, P is the period in days, V, PG and B are the corre- sponding magnitudes in maximum and minimum. Data are from P. N. Kholopov (Ed.), General Catalogue of Variable Stars, 4-th ed. Vol. I-IV, Moscow, Nauka Publ. House, 1985-1990. 66 A. Bartkevicius and R. Lazauskaite Table 8. Results of classification of standard stars in the Vilnius system No. Name Spectrum (Y-V) o Ey-V [Fe/H] MV 1. BD +00°145 A1V 0.21 0.00 0.97 2. BD +01°2916 MDGE-KO 0.98 0.06 -1.80 -1.83 3. BD +01° 4042 MDSG(sd):-G5pec 0.60 0.20 -0.90 5.49: 4. BD +02° 2446 C3.2CH 0.88 0.11 -1.21 5. BD +02°3336 C2,2CH 1.34 0.12 -2.02 6. BD +02°3363 sdG3 0.57 0.04 -1.02 6.47 7. BD +02° 3375 sdF7extr 0.50 0.01 -2.13 5.22 8. BD +02° 4651 sdF7extr 0.48 0.04 -1.88 4.22 9. BD +03° 740 sdF5extr 0.46 0.02 -2.27 4.57 10. BD +04° 59 MD-K1V 0.67 0.00 -0.31 6.04 11. BD +04° 2621 MDGE-G6 0.72 0.00 -2.07: -0.60 12. BD +04° 3561a (sdM3pec) 1.31 0.00 11.73: 13. BD +04°4551AB sdF7extr 0.51 0.02 -1.63 4.90 14. BD +04° 5012 MD-K4V 0.82 0.00 -0.62 7.33 15. BD +05° 3098 MDGE-G2 0.59 0.11 -1.99 0.24 16. BD +05°4314 sdG5extr:pec, CH? 0.69 0.00 . -1.51: 6.72 17. BD +06° 648 MDGE-Kl 0.92 0.07 -2.14 -1.84 18. BD +06° 4990 BHB-A0 0.31 0.09 -1.29 1.00 19. BD +07° 4841 sdF7extr 0.50 0.00 -1.52 4.87 20. BD +08° 2856 MDGE-G8 0.81 0.00 -1.86: -1.32 21. BD +08° 4982 MD-K2III 0.85 0.06 -0.34 0.60 22. BD +09° 2860 EHB:-G2 0.61 0.00 -1.53 -0.03 23. BD +09° 2870 MDGE-G8 0.76 0.00 -1.94: -0.92 24. BD +09° 4955 sdK4 0.72 0.00 -0.49 7.56 25. BD +10°6 MDGE-G5, RHB 0.66 0.07 -1.48 -0.05 26. BD +10°2179 He-B5: 27. BD +10° 2495 MDGE-G5, RHB? 0.61 0.00 -1.54 0.31 28. BD +11°2998 RHB-G0 pec 0.51 0.11 -1.21: 1.80: 29. BD +11°4381 RR-F5: 0.46 0.06 -0.34: 1.00 30. BD +11°4725 sdG2 0.58 0.01 -0.69 5.78 31. BD +12°853 sdG3: 0.58 0.05 -0.99:: 5.66 32. BD +12°2547 MDGE-G9 0.77 0.00 -1.82 -0.52 33. BD +12°4231 MD-G0V 0.54 0.02 -0.39 4.45 34. BD +13°3224 (He) 35. BD +13° 3683 sdF5extr 0.52 0.14 -2.27 5.31 36. BD +13° 4536 MD-F8V 0.50 0.03 -0.40 4.29 37. BD +16°2188 MD-Ba3-K0II/C3,lCH: 0.91 0.02 -0.36 -0.31 38. BD +17° 3248 MDGE-Gl 0.54 0.12 -1.82 0.51 39. BD +17°4708 sdF7extr 0.48 0.03 -1.78 4.72 40. BD +18°2757 MDGE-G3, AGB? 0.69 0.00 -2.52 -0.69 41. BD +18°2776 (sdMO:) 1.02 0.00 -1.08 8.59 42. BD +18°2890 MDGE-G3 0.61 0.06 -1.63 0.34 43. BD +18° 2976 MDGE-G5 0.75 0.05 -2.03 -1.19 44. BD +18°3423 sdF8 0.51 0.00 -1.10 4.66 45. BD +20° 3603 sdF5extr 0.47 0.00 -1.88 4.66 46. BD +21°4633 RR:-F3III 0.41 0.10 -0.03 1.25 47. BD +21°4996 GOV 0.54 0.03 -0.11 4.41 48. BD +22° 4409 MD-K3Vpec 0.81 0.00 -0.49 7.39 49. BD +22° 4454 MD-KOV 0.61 0.00 -0.19 5.53 50. BD +24°2490 MD-F5V: 0.44 0.01 -0.37 3.12 Classification of Population II Stars 67 Table 8 (continued) No. Name Spectrum Ey-V [Fe/H] My 51. BD +24°4460 sdKl 0.63 0.00 -0.69 6.24 52. BD +24°4563 G3V 0.57 0.00 0.12 4.77 53. BD +24°4592 K2V 0.68 0.01 -0.05 6.11 54. BD +24°4627 KOV 0.65 0.00 0.00 5.72 55. BD +24°4742 sdKO 0.68 0.00 -1.40 6.40 56. BD +24°4742 sdKO 0.72 0.00 -1.49 6.19 57. BD +24°4742 sdKO: 0.69 0.00 -1.61 6.26 58. BD +24°4742 MD7-G5V 0.57 0.00 -0.13 5.07 59. BD +25c404 sdF9 0.53 0.00 -0.87 4.59 60. BD +25°1981 sdF6 0.40 0.00 -1.34 3.36 61. BD +25°2534 sdO: 62. BD +25°4655 sdO: 63. BD +26° 2606 sdF7extr 0.48 0.00 -1.76 4.95 64. BD +26°4136 sdF9:extr 0.55 0.00 -1.73 5.80: 65. BD +26°4251 sdF8extr 0.50 0.00 -1.43 4.94 66. BD +27°2891 MD-G6V 0.58 0.00 -0.28 4.60 67. BD +28°4211 DAO/sdO 68. BD +29°95 C2,0CH 0.86 0.05 -1.06 69. BD +29°366 sdGl 0.55 0.00 -0.82 5.45: 70. BD +30°2022 MD-K0III, WG? 0.82 0.00 -0.36 0.47 71. BD +30°2431 B5III/sdB5: 72. BD +30°2512 K3V 0.87 0.00 0.12 7.35 73. BD +30°2611 MDGE-G9:pec 0.94 0.00 -1.46: -0.96 74. BD +32°2188 A1II 0.19 0.00 -3.50 75. BD +32°4645 G6V 0.59 0.05 -0.08 5.18 76. BD +32°4670 K2V 0.68 0.01 -0.11 6.30 77. BD +33°529 sdK5pec 0.96 0.00 -1.06 8.62 78. BD +33°2171 A Boo-Fl/sdFl 0.36 0.00 -0.65 1.03 79. BD +34° 2476 sdF3extr 0.46 0.00 -2.22 3.87 80. BD +34°2541 K7:V 0.90 0.00 0.11 7.52 81. BD +35°4669 G1V 0.53 0.00 0.12 4.37 82. BD +36°2233 MD-F5V 0.47 0.00 -0.63 3.32 83. BD +36°2242 B9IV-V 0.15 0.03 0.00 84. BD +37°1458 sdGOextr, MDSGE? 0.59 0.00 -1.98 5.53 85. BD +37° 2446 MD7-F7V 0.47 0.00 -0.06: 3.70 86. BD +38° 2803 UU Her-(F2Ib) 0.46 0.09 -1.41 -4.29 87. BD +38° 2803 UU Her-(FlIb) 0.37 0.09 -1.50: -4.92 88. BD +38° 2803 UU Her-(F2Ib) 0.45 0.09 -1.50 -4.56 89. BD +38° 2803 UU Her-(Fl:Ib) 0.38 0.09 -1.50: -4.75 90. BD +38° 2803 UU Her:—(F3II) 0.53 0.09 -1.43 -3.41 91. BD +38° 2803 UU Her-(F2Ib) 0.42 0.09 -1.55 -4.45 92. BD +38°4955 sdG5:extr 0.59 0.00 -1.94 6.74 93. BD +39°4926 UU Her-(A7Ia) 0.26 0.07 -7.11 94. BD +41°3306 MD-K0V 0.65 0.00 -0.44 6.16 95. BD +41°3931 sdG5extr 0.57 0.03 -1.57 6.21 96. BD +42°2173 C3,1CH 0.90 0.04 -1.49: -1.19 97. BD +42°2667 sdF6extr 0.49 0.00 -1.67 4.82 98. BD +42°3607 sdF7extr 0.51 0.04 -2.22 5.19 99. BD +44°3682 MD-G9V 0.61 0.00 -0.50 5.61 100. BD +46°3014 MD-F8V 0.50 0.01 -0.45 3.67 68 A. Bartkevicius and R. Lazauskaite Table 8 (continued) No. Name Spectrum (Y-V)o Ey-V [Fe/H] Mv 101. BD +46°4128 MDGE-K3:pec 1.16 0.22 -1.50: -1.25 102. BD +48° 739 MD7-K3V 0.71 0.00 -0.21 7.30 103. BD +48° 1777 He/sdO/DO 104. BD +49°4124 G3V 0.57 0.00 0.21 4.82 105. BD +57°2161 C2.1CH (-1.86) 106. BD +59°2723 sdF7extr 0.49 0.03 -2.13 5.18 107. BD +66° 268 sdG6extr 0.61 0.00 -2.03 6.86 108. BD +68° 946 (sdM:pec) 1.18 0.00 11.34 109. BD +70°1218 KOV 0.64 0.00 -0.08 5.63 110. BD +71°31 sdF5extr! 0.45 0.04 -2.62: 3.80 111. BD +71°851 K5V 0.78 0.00 0.07 6.75 112. BD +72°94 sdF5extr 0.47 0.01 -2.12 4.55 113. BD +73°39 sdF5extr 0.50 0.02 -1.38 4.81 114. BD +75° 348 C1,0CH 0.83 0.00 -1.56 -1.08 115. BD +75°839 sdGO 0.54 0.00 -1.08 5.18 116. BD +76° 524 RHB-Gl 0.58 0.00 -1.21 0.46 117. BD +78° 738 G6V 0.58 0.01 -0.03 5.13 118. BD +84° 19 (MDGE:-K9:) 119. BD -00°4234 sdK4 0.74 0.00 -1.29 7.64 120. BD -00°4470AB sdG5pec 0.63 0.00 -1.30:: 6.82 121. BD -00°4475 KlV 0.67 0.00 -0.05 5.71 122. BD -00° 4534 K2V 0.68 0.01 -0.02 6.31 123. BD -01° 306 sdGO 0.57 0.00 -1.09: 5.58 124. BD -01° 2582 MDG(SG)E-G3 0.59 0.01 -1.76 0.47 125. BD —01°3438 He-B8: 126. BD -01°4420 KlV 0.65 0.00 0.02 5.49 127. BD -02° 129 KlV 0.66 0.00 -0.08 6.10 128. BD -03° 56 sgCH-GO/sdGl 0.54 0.00 -1.27 5.19 129. BD -03° 5215 RHB-Gl 0.59 0.00 -1.39 0.43 130. BD -06° 27 KOV 0.64 0.01 -0.13 5.42 131. BD -07° 86 MD-G5V 0.58 0.00 -0.28 5.42 132. BD -08° 156 MD-G8III 0.72 0.06 -0.44 0.73 133. BD -08° 3901 MDSG:-G2 0.68 0.10 -1.16 1.47: 134. BD -09° 40 sdMl 1.01 0.00 -1.20 8.40 135. BD -09° 4395 sdO/DO/He? 136. BD -09° 5831 MDGE-G5 0.76 0.05 -1.89 -0.97 137. BD -09° 6150 MD-G5V 0.58 0.00 -0.50 5.17 138. BD -10°109 sdK9 1.00 0.00 -0.93 8.62 139. BD -10° 388 sdF5extr 0.47 0.01 -1.99 4.30 140. BD -10° 548 RHB-G5 0.63 0.02 -1.62 0.10 141. BD -11°145 MDGE!-G7 0.72 0.00 -2.60 -0.88 142. BD -11°162 He:/sdB 143. BD -12° 130 K3Vpec 0.74 0.04 0.07 6.57 144. BD -12°134 sdO/DAO 145. BD -13°3834 sdG8/sgCH-G0 0.53 0.00 -1.16 5.35: 146. BD —14°142 MDSG7-G0 0.51 0.00 -1.20: 3.86: 147. BD -14° 5850 sdF7extr 0.52 0.05 -2.20 5.04 148. BD -14° 5890 MDGE-G3 0.70 0.03 -2.35 -0.60 149. BD -15°67 K3Vpec 0.71 0.00 0.04 6.21 150. BD -15°115 He-B2III/sdB3: Classification of Population II Stars 69 Table 8 (continued) No. Name Spectrum (Y-V) o Ey-V [Fe/H] MV 151. BD -15° 560 A Boo—Fl: 0.41 0.04 -0.57 0.79 152. BD —15°872 RR-F6: 0.45 0.08 -1.39 0.75 153. BD -15°4515 A Boo-AlIII 0.36 0.27 -0.68 0.08 154. BD -15°5781 MDGEI-G3 0.73 0.04 -2.56 -1.13 155. BD -16°4187 sdKO 0.62 0.05 -1.12: 6.86 156. BD -17°484 sdF5:extr 0.47 0.01 -1.80: 4.23 157. BD -17°6036 MDGEI-G5 0.70 0.03 -2.57 -0.80 158. BD —18°271 MDGE-K0 0.95 0.04 -2.16 -2.63 159. BD -18° 5550 MDGE!-G3 0.66 0.17 -2.65 -0.36 160. BD -19°117 G2V 0.56 0.00 -0.13 4.77 161. BD -19° 132 C3,1CH 1.35 0.01 -1.98 162. BD -19° 290 C1,2CH 1.05 0.08 -1.46 -1.13 163. BD -20° 170 EHB:-G5 0.62 0.04 -1.28 0.78 164. BD -20°6008 MDGEI-G5 0.72 0.07 -2.56 -1.20 165. BD -22°395 MDGE-G5, AGB? 0.70 0.01 -2.48 -0.70 166. BPM 1034 He/WD/sdO 9.59 167. CD -23° 72 EHB-G3 0.61 0.00 -1.35 0.52 168. CD -23°16310 MDGE-G8 0.76 0.00 -2.13 -1.22 169. CD -24° 1782 MDSG-G2/sdF8extr 0.58 0.04 -2.33: 3.11: 170. CD -25° 13871 MDGE1-G5, AGB? 0.69 0.11 -2.48 -0.78 171. CD -25°16747 BS-sdF5 0.42 0.01 -1.23 3.49 172. CD -26° 13465 MDGE-G5 0.75 0.10 -1.65: -0.43 173. CD -29°15254 MDGE-G9 0.89 0.04 -1.65 -1.23 174. CD -30° 15602 UU Her?—AOIab 0.20 0.15 -0.88 -5.95: 175. CD -30° 16751 MDGE-G5 0.77 0.09 -1.43 -0.49 176. CD -30° 19358 MD-K2III 0.86 0.04 -0.35 0.50 177. CD -31°622 sd(MDSGE:)G0extr 0.55 0.08 -2.06 6.24 178. CD -38° 245 MDGEI-G5 0.71 0.03 -2.72 -0.64 179. G 1-27 WD? 14.15 180. G 1-30 sdF7extr 0.50 0.04 -1.51 4.74 181. G 3-9 sdKl 0.63 0.00 -0.91: 6.41 182. G 3-13 sdl<2 0.74 0.00 -1.32: 8.97 183. G 3-36 (sdMl) 1.08 0.00 9.90 184. G 5-36 sdF5extr 0.49 0.08 -1.79 4.65 185. G 8-6 sdGl 0.58 0.07 -0.91: 6.02 186. G 14-24 sdG3 0.60 0.02 -1.34 7.61 187. G 14-39 sdG5: 0.70 0.02 -1.55: 7.81 188. G 18-54 sdF8extr 0.51 0.00 -1.43 4.50 189. G 21-6 sdKO: 0.71 0.10 -0.81 6.19: 190. G 28-40 sdG7: 0.60 0.03 -0.81: 6.07 191. G 28-42 sdG3extr 0.56 0.03 -1.51 6.03 192. G 28-48 KlV 0.65 0.00 -0.06 5.78 193. G 29-31 (sdMO) 0.90 0.00 8.24 194. G 29-33 (sdMl) 1.04 0.00 8.56 195. G 29-44 K7V 0.93 0.00 0.33 7.98 196. G 29-71 sdF8extr 0.53 0.01 -1.84 5.60 197. G 30-2 sdK3 0.73 0.02 -0.63 7.35 198. G 31-26 sdG3extr 0.56 0.04 -1.85: 5.70 199. G 31-52 sdK5: 0.94 0.00 -0.66: 8.60 200. G 33-31 sdKl 0.66 0.00 -1.15: 7.44 70 A. Bartkevicius and R. Lazauskaite Table 8 (continued) No. Name Spectrum (Y-V)o Ey-V [Fe/H] Mv 201. G 35-29 DA3 0.13 0.00 10.78 202. G 37-40 (sdMl) 0.99 0.12 -1.20 8.55 203. G 38-1 sdK6 0.98 0.00 -0.81 8.60 204. G 64-12 sdF6extr 0.46 0.00 -1.98 4.48 205. G 70-17 sdK2 0.68 0.02 -0.60: 6.61 206. G 78-26 sdK5 0.86 0.00 -0.43 7.94 207. G 87-7 DA3 0.12 0.00 10.63 208. G 92-49 0.85 0.00 9.26 209. G 99-2 sdKO 0.64 0.00 -0.99 6.72 210. G 99-8 sdK3 0.72 0.02 -1.18 8.06 211. G 102-22 (sdM?) (12.57) 212. G 113-40 sdK2 0.71 0.00 -1.08 7.61 213. G 126-63 sdG3extr 0.54 0.00 -1.42 5.85 214. G 130-36 sdK3 0.73 0.00 -1.19 7.77 215. G 154-34 sdG5:extr 0.57 0.07 -2.08 6.63 216. G 158-53 (sdM2) 10.9 : 217. G 158-71 sdF8extr 0.52 0.00 -1.41 4.97 218. G 175-34B (WD) 13.57 219. G 180-58 sdG5extr 0.59 0.05 -1.95 6.34 220. G 184—48 sdM2 1.20 0.00 10.85 221. G 184-49 sdM2 1.21 0.00 10.60 222. G 186-26 sdF7extr 0.46 0.00 -1.95 5.04 223. G 186-31 DA3 0.11 0.00 10.69 224. G 188-30 sdG3extr 0.57 0.05 -1.43 6.90 225. G 191-B2B sdO/DO: 9.88 226. G 202-48 sdM2 1.21 0.00 10.88 227. G 206-34 sdF6extr 0.49 0.02 -2.20 4.28 228. G 226-29 DA4: 0.25 0.00 11.61 229. G 238-44 DA3 0.09 0.00 10.54 230. G 243-62 MD-K0V 0.66 0.04 -0.53 6.97 231. G 266-135 (DA4/DC) 12.00 232. G 268-32 sdF7extr 0.49 0.03 -1.76: 5.27 233. G 270-15 sdG5 0.58 0.00 -0.71 6.08 234. G 270—44 sdF8 0.53 0.00 -1.28 4.76 235. G 270-48 DO/sdOB: 11.16 236. G 270-52 sdG7:extr 0.58 0.09 -2.00 7.02 237. G 270-53 sdG2extr 0.56 0.02 -1.80 5.56 238. GD 645 sdF7extr,pec 0.47 0.12 -2.08 4.41 239. HD 26 CH:-K0 240. HD 97 RHB:-G3, MDSG? 0.65 0.04 -1.64 0.49 241. HD 187 sdF3, A Boo? 0.40 0.06 -0.71 0.92 242. HD 202 MD-G0V 0.53 0.00 -0.50 4.48 243. HD 208 MD-G0V 0.52 0.00 -0.41 4.90 244. HD 245 MD-G0V 0.54 0.01 -0.57 4.86 245. HD 249 MD-G9III 0.78 0.00 -0.27 1.08 246. HD 352 K5III+F9III/MDG-KlII-Ba 0.92 0.12 -1.44 -0.51 247. HD 432 FlIII 0.38 0.00 -0.20 1.51 248. HD 693 MD-F6V 0.49 0.00 -0.35 3.51 249. HD 702 sdGO 0.53 0.00 -0.78 4.44 250. HD 787 MD-K4III 1.04 0.03 -0.38 -0.25 Classification of Population II Stars 71 Table 8 (continued) No. Neune Spectram (Y-V)0 Ey-v [Fe/H] MV 251. HD 1368 MD-GOV 0.52 0.00 -0.59 4.41 252. HD 1388 G1V 0.55 0.00 -0.09 4.56 253. HD 1835 G5V 0.57 0.00 0.05 4.77 254. HD 1879 M2III 1.13 0.03 -0.18 -1.10 255. HD 2454 MD-F6V, BS? 0.46 0.00 -0.42 3.17 256. HD 2525 GlV 0.55 0.00 -O.Ol 4.72 257. HD 2665 MDGE-G3 0.62 0.08 -2.07 0.19 258. HD 2796 MDGE-G2, RHB? 0.64 0.06 -2.32 -0.41 259. HD 2857 BHB-AO 0.30 0.02 -1.10 1.02 260. HD 2925AB MD-G8III 0.73 0.01 -0.30 0.90 261. HD 3008 MDGE-KO 0.98 0.00 -1.65 -1.99 262. HD 3179 RHB-G5 0.60 0.00 -1.46 0.65 263. HD 3266AB MD-G2V 0.59 0.00 -0.28 5.40 264. HD 3296 F5V 0.47 0.00 -0.06 3.67: 265. HD 3457 K3III 0.94 0.05 -0.13 0.30 266. HD 3512A MD7-K3III 0.90 0.06 -0.30 0.25 267. HD 3546 MD-G7III, RHB? 0.67 O.Ol -0.37 0.78 268. HD 3567 sdF8extr 0.50 0.00 -1.35 4.64 269. HD 3627 K3III 0.92 0.00 0.01 0.46 270. HD 3628 G2V 0.57 0.00 -0.15 4.89 271. HD 3651 K1V 0.66 0.00 0.07 5.69 272. HD 3690AB MD-KOIII 0.79 0.05 -0.28 0.70 273. HD 3715 sdF5 0.46 0.00 -0.65 3.22 274. HD 4145 K2III 0.82 0.01 -0.02 1.09 275. HD 4156 sdGO 0.55 0.00 -0.66 4.99 276. HD 4158 A Boo-A5 0.38 0.00 -0.66 0.08 277. HD 4256 K3V 0.73 0.00 -0.02 6.46 278. HD 4306 MDGE!-G2 0.67 0.01 -2.62 -0.28 279. HD 4307 MD?-GlV 0.55 0.00 -0.21 4.52 280. HD 4374 G2V 0.56 0.00 -0.11 4.97 281. HD 4607 MD-F7IV-V 0.49 0.01 -0.25 3.12 282. HD 4628 MD7-K2V 0.66 0.00 0.09 6.19 283. HD 4744 MD-G9III 0.77 0.04 -0.57 1.05 284. HD 4906 MDSG:-G5 0.61 0.05 -0.83 3.69: 285. HD 5223 C3.1CH 0.97 0.10 -1.49: -1.25 286. HD 5268 MD-G8III 0.71 0.03 -0.50 0.97 287. HD 5338 MD-G2V 0.56 0.00 -0.24 4.99 288. HD 5351 MD-K3V 0.76 0.00 -0.52 6.99 289. HD 5395 MD-G9III 0.72 0.00 -0.45: 1.19 290. HD 5780 MD-K4II-III 1.04 0.02 -0.38 -0.38 291. HD 5916 MD-G7IVpec 0.73 :0.00 -0.41 3.22: 292. HD 5917 G6IV-V 0.59 0.01 0.10 4.88 293. HD 6101 MD-K4Vpec 0.73 0.00 -0.17 7.35 294. HD 6186 MD-G9III 0.77 0.00 -0.51 0.86 295. HD 6229 RHB-G5 0.61 0.04 -1.38 0.63 296. HD 6268 MDGE!-G5, AGB? 0.72 0.04 -2.46 -1.08 297. HD 6461 RHB-G3 0.66 0.00 -0.56 0.71 298. HD 6474 MDGE-KO, RV Tau? 0.98 0.27 -1.86 -2.85 299. HD 6497 K2III 0.85 0.03 -0.02 0.75 300. HD 6582 MD-G5V 0.58 0.00 -0.49 5.79 72 A. Bartkevicius and R. Lazauskaite Table 8 (continued) No. Name Spectrum (Y-V) o Ey-V [Fe/H] MV 301. HD 6734 G7IV 0.67 0.02 -0.14 2.80 302. HD 6755 MDSGE-G3 0.56 :0.09 -1.89: 3.16: 303. HD 6833 MDG-KO 0.78 0.12 -0.65: 0.47 304. HD 6860 K9III 1.13 0.00 -0.08 -0.75 305. HD 6903 RHB-G3 0.62 0.00 -0.78 0.91 306. HD 7424 MD-G1V 0.56 0.01 -0.47 5.32 307. HD 7672 MD-G6III, RHB? 0.67 0.05 -0.44 1.36 308. HD 7808 MD-K3V 0.74 0.00 -0.45 7.66 309. HD 7983 MD-GOV 0.55 0.00 -0.64 5.07 310. HD 8724 MDGB-G5 0.76 0.08 -1.93 -0.63 311. HD 9549 A9IV 0.30 0.09 0.05 1.76 312. HD 9826 F8V 0.53 0.00 -0.11 3.57 313. HD 10307 G2V 0.54 0.00 0.09 4.73 314. HD 10700 MD-G7V 0.58 0.00 -0.17 5.23 315. HD 11397 MD-G5:V 0.59 0.00 -0.48 5.86 316. HD 11636 A4IV-V 0.21 0.00 2.07: 317. HD 11909 G7II-HI, WG 0.73 0.00 -0.12 0.91 318. HD 12235 G2(IV)-V 0.54 0.00 -0.01 4.10: 319. HD 12929 MD-K2III 0.86 0.00 -0.26 0.78 320. HD 13359 RHB-G4 0.59 0.06 -1.45 0.28 321. HD 13783 MD-G5V 0.59 0.00 -0.38 4.86 322. HD 13826 (C5,3CH) 323. HD 13974 MD-GOV 0.54 0.00 -0.29 5.14 324. HD 13979 MDGE!-G3 0.66 0.00 -2.53 -0.36 325. HD 14056 sdGO 0.55 0.02 -0.68 5.40 326. HD 14829 BHB-A2III 0.23 0.00 -1.30 0.97 327. HD 15096 MD-KOV 0.64 0.00 -0.22 6.45 328. HD 16031 sdF5extr 0.48 0.00 -1.92 4.96 329. HD 16115 CO,ICH 0.90 0.01 -1.44 -1.06 330. HD 16160 MD7-K3V 0.71 0.00 -0.14: 6.71 331. HD 16234 MD-F6V 0.51 0.00 -0.41 3.64 332. HD 16397 MD-GOV 0.55 0.00 -0.53 5.13 333. HD 16458 MD-Ba4-Kl III 0.90 0.04 -0.31 -0.22 334. HD 17820 sdGO 0.54 0.00 -0.68 4.60 335. HD 18474 MD-G 5II-III/G1 lab 0.74 0.00 -1.33 -0.90 336. HD 19445 sdF6extr 0.50 0.00 -2.25 4.77 337. HD 19510 RR Lyr-F6 0.45 0.15 -1.32: 0.77 338. HD 19735 MD-K4III 1.05 0.00 -0.23 0.09 339. HD 19931 RR Lyr-F7 0.45 0.08 -1.33: 0.80 340. HD 20084 MD-G8III 0.69 0.00 -0.47 1.46 341. HD 20512 MD7-G8V 0.65 0.00 -0.19: 5.96 342. HD 21018AB RHB:-G6 0.68 0.03 -0.38 0.64 343. HD 21019AB sd(MDSG)-G5pec/G2V 0.61 0.00 -1.02: 5.84 344. HD 21110 K4III 0.93 0.17 -0.07 0.70 345. HD 21120 MD-G8III/G4II-III 0.72 0.00 -0.30 0.79 346. HD 21543 MD-GOV 0.55 0.00 -0.18 4.86 347. HD 21581 MDGE-G5, RHB? 0.64 0.07 -1.76 0.16 348. HD 21674 MD-F6V 0.49 0.00 -0.29 3.58 349. HD 22225 M2III 1.20 0.12 -0.17 -0.39 350. HD 23249 MD7-G9III-IV: 0.71 0.00 0.10: 1.65: Classification of Population II Stars 73 Table 8 (continued) No. Name Spectrum (Y-V) o Ey-V [Fe/H] MV 351. HD 23441 AOV 0.19 0.00 0.64 352. HD 23511 MD?-F7Vpec 0.47 0.00 -0.16 3.54 353. HD 23568 AOV 0.17 0.07 0.80 354. HD 23642 A1V 0.19 0.04 1.17 355. HD 23763 A4V, A Boo? 0.25 0.01 -0.24: 1.56 356. HD 25173 sdF8 0.52 0.00 -0.70 4.30 357. HD 25329 sdKl 0.69 0.00 -1.47 7.47 358. HD 25408 (C4,3CH) 1.34 0.19 -1.88 359. HD 25532 RHB-G0 0.57 0.08 -1.39 0.80 360. HD 25878 (MDGE, R CrB) 361. HD 26976BC (DA/DC) 11.64 362. HD 27108 (C3,3CH) 363. HD 27370 MD-G8III 0.76 0.12 -0.27 0.96 364. HD 28258 K0IV-V 0.65 0.00 0.11 5.55 365. HD 28462 K1V 0.67 0.00 -0.03 5.84 366. HD 28527 A5V 0.23 0.01 0.10 1.23 367. HD 28783 MD-K1V 0.67 0.00 -0.22 6.03 368. HD 28805 G8IV-V 0.61 0.00 0.07 5.20 369. HD 29574 MDGE-KO 0.99 0.11 -1.93: -2.29 370. HD 30353 (He?) 371. HD 30443 (C5,3CH:) 1.34 0.42 -2.16 372. HD 30649 MD-G1V 0.55 0.00 -0.56 5.07 373. HD 32147 K5V 0.76 0.00 0.06 6.86: 374. HD 33256 MD-F7IV 0.45 0.00 -0.27 2.79: 375. HD 33564 F6V 0.48 0.00 -0.03 3.51 376. HD 33708 MD?-KlIII 0.85 0.05 -0.27 0.81 377. HD 34250 A6II-III/UU Her-F3: 0.37 0.32 -1.48 -4.00 378. HD 34411 G2V 0.56 0.00 0.05 4.71 379. HD 35296 MD?-F9V 0.50 0.00 -0.09 4.49 380. HD 35993 MD-Ba2-K0III 0.81 0.00 -0.41 -0.17 381. HD 36283 MD?-G2V 0.58 0.00 -0.22 5.31 382. HD 37160 MD-G9III 0.74 0.00 -0.52 0.87 383. HD 41870 MDG-F9:, CH-RV Tau, RV Tau 0.62 0.34 -1.23: -3.60 384. HD 43039 MD-G8III 0.77 0.00 -0.25 0.86 385. HD 44007 MDGE-G5 0.66 0.03 -1.60 0.13 386. HD 46588 MD-GOV 0.52 0.00 -0.50 3.79 387. HD 46703 UU Her-FOIb 0.45 0.07 -1.61 -4.73 388. HD 49709 FOIV 0.34 0.07 -0.17 1.87 389. HD 50060 F9V 0.50 0.00 -0.07 3.64 390. HD 51959 MD-Ba5-K0lII 0.76 0.03 (-0.4 ) (0.0) 391. HD 56243 MD7-K5III 1.04 0.00 -0.20 -0.13 392. HD 58807 F3IV-V 0.41 0.00 -0.11 3.05: 393. HD 59643 (CH) 394. HD 60778 BHB-AOV 0.22 0.00 -1.31 1.03 395. HD 62509 MD-G9III 0.76 0.00 -0.48 0.86 396. HD 67447 MD?-G7II, Ba? 0.76 0.05 -0.25 -1.76 397. HD 73394A MDGE-G8 0.78 0.07 -1.67: -0.77 398. HD 74462 MDGE-G5 0.76 0.08 -1.83 -0.29 399. HD 74721 BHB-A2III 0.21 0.00 -1.27 1.02 400. HD 76396 C1,1CH: 0.81 0.05 -1.49 -0.47 74 A. Bartkevicius and R. Lazauskaite Table 8 (continued) No. Name Spectrum (Y-V) 0 Ey-V [Fe/H] MV 401. HD 76644ABC A7V 0.24 0.00 -0.01 2.15 402. HD 79096 MD7-G9V 0.61 0.00 -0.22 5.66 403. HD 79452 MD-G5III, RHB? 0.67 0.02 -0.58 0.73 404. HD 79657 sdFl, BS 0.36 0.00 -1.16 2.63 405. HD 81192 MD-G8III, RHB? 0.71 0.04 -0.49 0.64 406. HD 84035 K6Vpec 0.77 0.00 0.03 6.72 407. HD 84937 sdF3extr 0.46 0.00 -2.13 4.02 408. HD 86728 G6V 0.56 0.00 0.17 4.40 409. HD 86986 BHB-AOV 0.23 0.03 -1.28 1.06 410. HD 88230 MOV 0.92 0.00 0.29 7.71 411. HD 88609 MDGE!-G9 0.76 0.07 -2.41 -1.36 412. HD 89744 F7IV-V 0.49 0.00 0.13 2.91 413. HD 91612 G9III-IV, Ba? 0.68 0.00 -0.12 2.19: 414. HD 92168 GOIV 0.53 0.00 0.25 2.43 415. HD 96833 MD-K2III 0.84 0.00 -0.20 0.81 416. HD 97603 A5IV 0.25 0.00 1.30 417. HD 100470 KOIII 0.79 0.00 -0.16 0.89 418. HD 100971 RR Lyr-F5 0.45 0.03 -1.47 0.75 419. HD 101501 G8V 0.60 0.00 0.02 5.24 420. HD 102647 A3V 0.24 0.00 -0.17: 1.34 421. HD 102870 F9V 0.50 0.00 0.17 3.74 422. HD 103036 MDGE-KO, SRD? 0.98 0.05 -1.71 -2.35 423. HD 103095 sdG8 0.62 0.00 -1.06 6.67 424. HD 103545 MDGE!-G3, RHB 0.67 0.08 -2.46 -0.78 425. HD 104979 MD-Ba2-G9III 0.74 0.00 -0.40 0.78 426. HD 105546 RHB-G3 0.60 0.02 -1.46 0.31 427. HD 105791 MDSGE:-Gl: 0.56 0.00 -1.94 0.58 428. HD 106223 A Boo-F2 0.40 0.00 -1.35: 0.81 429. HD 106591 A3IV 0.22 0.00 0.96 430. HD 107328 MD-K2III 0.85 O.Ol -0.23 0.65 431. HD 108577 MDGE-G3 0.65 0.00 -2.15: -0.32 432. HD 109358 MD-GOV 0.54 0.00 -0.31 4.67 433. HD 109995 BHB-AOV 0.22 0.00 -1.26: 1.02 434. HD 110166 B8III-IV, BHB? 0.16 0.00 -0.10 435. HD 110184 MDGE-Kl 0.97 0.00 -2.24 -2.57 436. HD 110315 K7V 0.77 0.00 0.04: 6.93: 437. HD 110897 MD-GOV 0.53 0.00 -0.41 4.32 438. HD 111908C C3,0CH 0.81 0.00 -0.77 439. HD 112869 (C4,4CH) 1.30 0.00 -2.22 440. HD 113226 G7III 0.73 0.00 -0.14: 0.95: 441. HD 113284 MD-FOV, BS 0.39 0.03 -0.62 1.76: 442. HD 114710 GOV 0.53 0.00 -0.06 4.45 443. HD 115383 GOV 0.55 0.00 -0.09 4.35 444. HD 115444 MDGE!-G3 0.66 0.08 -2.59 -0.91 445. HD 117043 G7IV-V 0.60 0.00 0.14 4.87 446. HD 119516 RHB-F9 0.54 O.Ol -1.89: 0.69 447. HD 119850 M2V, sdM2 1.07 0.00 10.60 448. HD 121135 MDGE-G5 0.66 0.00 -1.65: -0.16 449. HD 121370 F9IV-V 0.54 0.00 0.25 3.03 450. HD 121447 C2,1CH: 1.25 0.00 -2.14 Classification of Population II Stars 75 Table 8 (continued) No. Name Spectrum (Y-V)o Ey-V [Fe/H] MV 451. HD 122563 MDGE!-G7 0.74 0.05 -2.47 -1.23 452. HD 122742 G8V 0.61 0.00 -0.09 5.34 453. HD 122956 MDGE-G5 0.71 0.08 -1.35 -0.07 454. HD 124897 MD-K2III 0.91 0.00 -0.31 0.09 455. HD 125079 MD-G8IV: 0.69 0.00 -0.35 2.78 456. HD 125162 A1V 0.22 0.00 0.10 1.11 457. HD 126053 MD-G2V 0.58 0.00 -0.56 5.20 458. HD 126512 MD-GOV 0.56 0.00 -0.42 4.68 459. HD 126587 MDGE!-G3 0.66 0.08 -2.61 -0.16 460. HD 126660 F7V 0.51 0.00 -0.13 3.53 461. HD 126681 sdGl 0.54 0.01 -1.29 5.68 462. HD 127665 K3III 0.94 0.00 -0.13 0.74 463. HD 128167 MD-F3V 0.43 0.00 -0.54 3.03 464. HD 128279 MDSGE:-G0:pec, sd? 0.60 0.00 -2.32 5.47 465. HD 128750 MD-KOIII, WG 0.81 0.00 -0.27 0.72 466. HD 129502 MD-F3IV-V 0.46 0.00 -0.33 3.35 467. HD 130948 MD7-G0V 0.54 0.00 -0.14 4.66 468. HD 131511 K1V 0.65 0.00 -0.02 5.63 469. HD 134083 F5V 0.46 0.00 -0.08 3.43 470. HD 134169 sdF8 0.51 0.00 -0.77 4.65 471. HD 134439 sdG8 0.64 0.00 -1.08 6.82 472. HD 134440 sdKl 0.68 0.00 -1.04 7.51 473. HD 135148 MDG-KO, CH? 0.94 0.06 -0.97 -1.35 474. HD 135722 MDG-G8III 0.76 0.00 -0.55 0.86 475. HD 137391 MD7-F0IV 0.34 0.00 -0.49 1.99 476. HD 137569 AOIb, UU Her? 0.18 0.02 -5.00 477. HD 139195 G9III-IV 0.73 0.00 -0.08 1.98 478. HD 140283 sdF9extr 0.53 0.00 -1.87 5.06 479. HD 140573 K2IIIpec 0.77 0.00 -0.03 0.90 480. HD 141004 G2V 0.56 0.00 -0.13 4.65 481. HD 141527 (R CrB) 482. HD 142267 MD-GOV 0.55 0.00 -0.34 4.93 483. HD 142373 MD-F9V 0.51 0.00 -0.26 4.40 484. HD 142780 M2III 1.15 0.10 -0.07 -0.93 485. HD 142860 MD7-F7V 0.48 0.00 -0.18 3.96 486. HD 144287 G8V 0.61 0.00 0.05 5.31 487. HD 144579 MD-G7V 0.61 0.00 -0.38 5.80 488. HD 144872 K3V 0.70 0.00 -0.13 6.86 489. HD 144921 MDGE-KO 1.07 0.17 -1.85: -2.21 490. HD 145148 KlIV:pec 0.74 0.00 0.00 2.20: 491. HD 145293 RHB/RR Lyr-F3 0.48 0.15 -1.14 0.83 492. HD 145675 KlV 0.67 0.00 O.Ol 6.11 493. HD 145777 C3,2CH 0.96 0.28 -1.17 494. HD 146233 G2V 0.57 0.00 -0.04 4.85 495. HD 147379 K8:Vpec 0.97 0.00 0.33 7.70 496. HD 148816 sdF8 0.55 0.00 -1.20: 4.55 497. HD 148897 MDG-KO, CH?, WG? 0.89 0.08 -1.75: -0.39: 498. HD 149382 sdO/DO 499. HD 149661 KlV 0.65 0.00 -0.03 5.71 500. HD 149933 G9IV-V 0.62 0.00 0.13 5.19 76 A. Bartkevicius and R. Lazauskaité Table 8 (continued) No. Name Spectrum (Y-V)0 EY-V [Fe/H] MV 501. HD 150875 MD-F2IV 0.44 0.13 -0.32 2.65 502. HD 151288 K8V 0.93 0.00 0.32 8.09 503. HD 151877 K2V 0.64 0.00 0.06 5.52 504. HD 152391 G8V 0.62 0.00 -0.05 5.43 505. HD 152792 GOV 0.57 0.00 -0.04 4.59 506. HD 153687 K5II-III 1.07 0.00 -0.19 -0.13 507. HD 154276 MD-G1V 0.55 0.02 -0.27 4.40 508. HD 154278 MD-KOIII 0.79 0.00 -0.25 0.88 509. HD 154345 G8V 0.60 0.00 0.00 5.06 510. HD 154417 GOV 0.52 0.00 0.05 4.57 511. HD 156164 A4IV 0.23 0.00 1.18 512. HD 157089 MD-GOV 0.55 0.00 -0.64 4.85 513. HD 157214 G2V 0.56 0.00 -0.20 4.81 514. HD 157415 MD-KOIII 0.77 0.21 -0.34 0.93 515. HD 157881 K9V 0.94 0.00 0.22 8.22 516. HD 158226 MD-GOV 0.54 0.03 -0.67 4.85 517. HD 158633 MD-KOV 0.62 0.00 -0.29 5.69 518. HD 158809 MD-G3V 0.55 0.00 -0.34 5.33 519. HD 159222 G3V 0.56 0.00 0.07 4.48 520. HD 159370 MD-F4IV, A Boo 0.41 0.14 -0.71 1.45 521. HD 159482 sdGl 0.54 0.00 -0.83 5.24 522. HD 159561 A5III-IV 0.27 0.00 0.98 523. HD 160346 K3V 0.70 0.00 0.03 6.15 524. HD 160641 sdOB 525. HD 160693 MD-GOV 0.54 0.00 -0.52 4.45 526. HD 161096 K2III 0.85 0.00 0.06 1.07 527. HD 161770 sdGOextr, MDSGE? 0.54 0.10 -2.13 5.56 528. HD 161796 UU Her:, A9Iab 0.34 0.12 -6.39 529. HD 161797 G7IV 0.62 0.00 0.16 3.01: 530. HD 161817 BHB-B9 0.30 0.00 -1.13 0.94 531. HD 163506 UU Her?, A9Ia 0.34 0.07 -5.27 532. HD 163810AB sdG5extr 0.57 0.00 -1.36 5.74 533. HD 164058 K7III 1.09 0.00 -0.09 -0.39 534. HD 164259 MD-F3IV-V 0.42 0.00 -0.34 2.97 535. HD 164922 KOIV 0.64 0.00 0.03 4.26: 536. HD 165195 MDGE-KO 0.95 0.10 -2.23 -2.32 537. HD 165401 MD-G1V 0.56 0.00 -0.48 4.87 538. HD 165634AB G9IIIpec 0.74 0.00 0.03 0.39 539. HD 165908AB MD-GOV 0.51 0.00 -0.64 4.66 540. HD 166161 RHB-G5 0.62 0.20 -1.45 0.54 541. HD 166181 sdG5pec 0.61 0.00 -0.77 5.68 542. HD 166208 MD-G7III 0.73 0.02 -0.37 0.28 543. HD 166620 K2V 0.68 0.00 -0.15 5.93 544. HD 167768 RHB7-G7 0.69 0.02 -0.35 1.33 545. HD 168151 MD-F5V/F9Ib+B5II 0.45 0.00 -0.63 2.96 546. HD 168656B MDG-G5 0.67 0.23 -1.28 0.42 547. HD 168723 G9IV 0.74 0.00 -0.14 1.37 548. HD 168785 He-B2, sdOB 549. HD 170737 MDSG-G5 0.61 0.06 -0.88 3.86 550. HD 170756 CH-RV Tau, (A9V) 0.18 0.09 -1.23: -1.40: Classification of Population II Stars 77 Table 8 (continued) No. Name Spectrum (Y-V)o Ey-V [Fe/H] MV 551. HD 170756 CH-RV Tau, A6V 0.20 0.09 -1.23: -3.70: 552. HD 170756 CH-RV Tau, A7V 0.19 0.09 -1.23: -3.70: 553. HD 170756 CH-RV Tau?, (F8III) 0.56 0.09 -1.01: (-0.45) 554. HD 170756 CH-RV Tau, F2Ia 0.62 0.09 -1.23 -3.38 555. HD 171314 K5V 0.81 0.00 0.03: 6.87 556. HD 171620 MD-F9V 0.50 0.00 -0.50 3.37 557. HD 172167 A2IV 0.15 0.00 1.07 558. HD 172594 UU Her-Flla 0.35 0.40 -7.43 559. HD 173399 G7IV 0.69 0.00 -0.06 2.38 560. HD 173667 F7V 0.45 0.00 -O.Ol 3.53 561. HD 173819 (MDGE-KO) 0.99 0.20 -1.68: -2.24 562. HD 173819 (CH-RV Tau) 563. HD 173920 RHB-G6 0.67 0.00 -0.39 0.92 564. HD 174638 (He) 565. HD 174912 MD-GOV 0.53 0.00 -0.47 4.36 566. HD 174974 G7Ib 0.89 0.20 -5.6 567. HD 175179 MD-G1V 0.54 0.00 -0.50 5.16: 568. HD 175190 K3II-III 0.96 0.04 -0.15 -0.57: 569. HD 175225 KOIV 0.66 0.00 0.01 4.01: 570. HD 175305 MDSGE-G3pec 0.59 0.07 -1.68 2.68: 571. HD 175545 K2III 0.84 0.03 0.13 1.99 572. HD 176203 RHB-GO 0.59 0.09 -1.32 0.66 573. HD 176441 MD-F7V 0.48 0.00 -0.28 4.48 574. HD 176609 BS-sdF5 0.44 0.05 -1.20: 3.46 575. HD 177249 G7III 0.68 0.00 -0.16 0.75 576. HD 177758 MD-GOV 0.53 0.00 -0.44 4.73 577. HD 177830 K1III-IV 0.79 0.00 0.07 1.76 578. HD 179626 sdF8 0.53 0.00 -1.07 4.80 579. HD 181007 MDSG:-G2 0.56 0.14 -1.24 3.72 580. HD 181615/6 (He)/B91a+Kllb 581. HD 181984 K3III 0.93 0.00 -0.05 0.61 582. HD 182335 G1V 0.53 0.00 -0.06 4.55 583. HD 182488 KOV 0.64 0.00 -0.03 5.14 584. HD 182572 G8IV-V 0.63 0.00 0.11 4.18 585. HD 183255 MD7-K3V 0.71 0.00 -0.35 6.74 586. HD 183418 MD-G7III, RHB 0.71 0.05 -0.19 1.13 587. HD 183968 K3III 0.89 0.00 -0.02 0.74 588. HD 184266 RHB-F8 0.53 0.05 -1.62 0.68 589. HD 184406 K2III 0.87 0.01 -0.05 0.67 590. HD 184467 MD?-K1V 0.68 0.00 -0.24 6.15 591. HD 184499 MD-GOV 0.54 0.00 -0.48 4.57 592. HD 184700 G2V 0.56 0.00 0.13 4.59 593. HD 184711 MDGE-KO 0.95 0.15 -2.34: -2.33 594. HD 184768 G5V 0.58 0.00 0.00 4.62 595. HD 185144 KOV 0.62 0.00 -0.06 5.74 596. HD 185657A MD7-G9III 0.76 0.01 -0.18 0.85 597. HD 185737 MD- G7III, RHB 0.68 0.03 -0.30 1.03 598. HD 186259 F7V 0.48 0.03 -0.18 3.18 599. HD 186379 MD-F8V 0.53 0.00 -0.32 4.41 600. HD 186408 G5IV-V 0.57 0.00 0.04 4.58 78 A. Bartkevicius and R. Lazauskaite Table 8 (continued) No. Name Spectrum (Y-V)o Ey-V [Fe/H] MV 601. HD 186478 MDGE-G5 0.72 0.11 -2.04 -0.66 602. HD 187013 MD-F7V 0.48 0.00 -0.23 3.13 603. HD 187111 MDGE-KO 0.86 0.12 -1.77 -1.36 604. HD 187162 MD-G7III 0.72 0.05 -0.38 0.81 605. HD 187216 C2,2CH: 1.12 0.23 -1.74: -1.41 606. HD 187642 A7IV 0.28 0.00 1.77 607. HD 188510 sdG7extr 0.58 0.00 -1.80 6.22 608. HD 188512 MD7-G9IV 0.68 0.00 -0.16 2.71 609. HD 188650 Gllllpec 0.60 0.04 0.31 1.26: 610. HD 189087 KOV 0.63 0.00 -0.08 5.53 611. HD 189276 K5III 1.09 0.05 -0.14 -0.37 612. HD 189558 sdGO 0.56 0.00 -0.93 4.60 613. HD 189711 (C4.4CH:) 1.37 0.25 -2.16 614. HD 190007 K7V 0.77 0.00 0.03 6.91: 615. HD 190178 sdF8 0.48 0.00 -0.63 3.05 616. HD 190283 MD-G8III-IVpec 0.70 0.13 -0.50 1.11 617. HD 190390 UU Her-A9lb 0.44 0.13 -1.69 -4.23 618. HD 190404 MD-KlV 0.66 0.00 -0.56 6.26 619. HD 190712AB A3IV-V 0.24 0.11 1.23 620. HD 191026 G9IV-V 0.69 0.00 0.03 4.89: 621. HD 191046 MD-KOIII, WG 0.82 0.04 -0.35 1.25 622. HD 192042 BS-sdF5 0.42 0.01 -0.79: 3.15 623. HD 192239 KOV 0.66 0.00 -0.11 5.95 624. HD 192310 K2V 0.66 0.00 -0.03 5.48 625. HD 192455 F7V 0.50 0.00 -0.04 3.38 626. HD 192640 A1V, A Boo? 0.26 0.02 0.91 627. HD 193242 MDGE-G5 0.72 0.02 -1.75: -0.39 628. HD 193664 MD7-G2V, sg-CH? 0.55 0.00 -0.14: 4.85 629. HD 193901 sdG5: 0.54 0.00 -1.37 5.36: 630. HD 194012 MD-F7V 0.50 0.00 -0.29 3.78: 631. HD 194598 sdF7extr 0.52 0.00 -1.52 4.96 632. HD 195633 sdF8 0.51 0.02 -0.77 4.25 633. HD 195636 MDGE-GO, RHB 0.55 0.06 -2.05 0.00 634. HD 195987 MD-KOV 0.64 0.00 -0.44 5.81 635. HD 196610 (M?) 636. HD 196882AB K3III 0.88 0.03 -0.10 0.50 637. HD 197076 G3V 0.53 0.00 0.09 5.23 638. HD 197177AB MD-G8III 0.72 0.02 -0.42 0.99 639. HD 197604 C2,0CH: 0.84 0.22 -1.06 640. HD 197988 BS-sdF5extr 0.43 0.03 -1.40 3.47 641. HD 197989 MD-KOIII 0.79 0.00 -0.28 1.29 642. HD 198084 F8V 0.50 0.00 0.12 3.50 643. HD 198269 C3,0CH 0.82 0.14 -0.57 644. HD 198300 MD-G1V 0.54 0.00 -0.38 4.65 645. HD 198809 MD7-G7III-IV 0.68 0.00 -0.21 1.34 646. HD 199191 MD-G7III 0.71 0.04 -0.42 0.94 647. HD 199305 sdK9/M3V 1.14 0.00 9.33: 648. HD 199476 MD7-G2V:, sg? 0.59 0.00 -0.16 5.36 649. HD 199854 RR-F5: 0.44 0.05 -1.35 0.77 650. HD 199939 MD-Ba-G8III 0.90 0.02 -0.39 -1.10 Classification of Population II Stars 79 Table 8 (continued) No. Name Spectrum (Y-V) o Ey-V [Fe/H] Mv 651. HD 200544 MD-G2V 0.57 0.00 -0.46 5.19 652. HD 200580 MD-GOV 0.53 0.00 -0.44 4.24 653. HD 201503 MD-GOV 0.53 0.00 -0.37 4.66 654. HD 201626 CO,ICH: 0.78 0.09 655. HD 201891 sdF8 0.52 0.00 -1.26 4.97 656. HD 202109 MD-Ba-G8II 0.76 0.00 -0.41 -1.10 657. HD 202123 K2V 0.67 0.00 -0.11 6.16 658. HD 202314 MD-Ba-G7II 0.76 0.10 -0.33 -0.42 659. HD 202573 RHB:-G7 0.68 0.03 -0.41 1.07 660. HD 202759 BHB-Al 0.29 0.08 -1.26 0.92 661. HD 202851 C1,2CH 0.92 0.05 -1.12 662. HD 203280 A7IV 0.29 0.00 1.50 663. HD 203454 MD-GOV 0.52 0.00 -0.38 4.45 664. HD 204075 MD-G8III: 0.70 0.00 -0.26 1.16 665. HD 204153 MD-F2IV-V 0.39 0.00 -0.43 2.77 666. HD 204155 sdGl 0.54 0.00 -0.71 4.65 667. HD 204543 MDGE-G5 0.77 0.00 -1.70 -0.74 668. HD 204613 G2V 0.56 0.00 -0.02 4.90 669. HD 204814 G8V 0.62 0.00 -0.05 5.53 670. HD 205011 MD-Ba-KlIII 0.79 0.02 -0.28 -0.06 671. HD 205142 K2V 0.66 0.00 -0.06 5.78 672. HD 205202 MDSG(sd)-F5 0.44 0.02 -0.62 2.70 673. HD 205650 sdF8 0.52 0.01 -1.11 4.80 674. HD 206739 MDGE-G5 0.77 0.00 -1.47 -0.25 675. HD 206778 K2Ib, MD-BA? 1.11 0.00 -0.40 -0.62 676. HD 206860 MD7-G1IV-V 0.53 0.00 -0.10 4.36: 677. HD 206983 K2Ib:, Ba? 1.07 0.14 -0.13 -1.45: 678. HD 207098 A9IV: 0.32 0.00 0.01 1.91: 679. HD 207692 F7V 0.46 0.00 -0.09 3.06 680. HD 207897 K2V 0.67 0.00 0.06 5.97 681. HD 207978 MD-F7V 0.46 0.00 -0.52 3.28 682. HD 208110 RHB-G3 0.65 0.04 -1.22 1.11 683. HD 208776 GOV 0.54 0.00 -0.16 4.26 684. HD 208906 sdF8 0.52 0.00 -1.01 4.65 685. HD 209621 C2,2CH: 1.00 0.13 -1.50: -1.22 686. HD 209813 MD-G8III 0.76 0.06 -0.46 1.63 687. HD 210027 F6V/F9Ib+B5lII 0.45 0.00 O.Ol 3.42 688. HD 210295 MDG-G3: 0.66 0.09 -1.21 0.71 689. HD 210523 MDGE-KO 0.81 0.04 -1.70 -1.05 690. HD 210585 MDGE-G5 0.67 0.04 -1.92 -0.31 691. HD 210595 BS-sdF5 0.44 0.05 -0.59 3.51 692. HD 210884 BS-F3IV-V 0.42 0.00 -0.34 3.31 693. HD 211336 A9IV 0.35 0.00 1.95 694. HD 212061 AOIV 0.15 0.00 0.41 695. HD 212857 MD-GlV, sdCH 0.55 0.00 -0.47 5.32 696. HD 213487 RHB-G3 0.65 0.07 -0.76 0.65 697. HD 213893 K5III 1.07 0.05 -0.11 -0.61 698. HD 213996 KOV 0.67 0.00 -0.04 5.57 699. HD 214362 RHB-Gl 0.53 0.00 -2.61: 0.53 700. HD 214714A RHB:-G5 0.66 0.06 -0.78 0.93 80 A. Bartkevicius and R. Lazauskaite Table 8 (continued) No. Name Spectrum (Y-V)o Ey-V [Fe/H] MV 701. HD 214925 MDGE-Kl, SRD 1.09 0.12 -1.70 -2.57 702. HD 215065 MD-G1V 0.58 0.00 -0.28 5.11 703. HD 215257 sdF8 0.51 0.00 -0.77 4.34 704. HD 215648 MD-F7IV-V 0.49 0.00 -0.26 3.25 705. HD 216135 (B3V) 706. HD 216143 MDGE-G7 0.78 0.05 -2.00: -1.13 707. HD 216174 K1III 0.87 0.01 -0.33 0.31 708. HD 216219 G2V 0.58 0.00 -0.15 4.05 709. HD 216385 MD-F7V 0.49 0.00 -0.37 3.06 710. HD 216777 MD-G8V 0.58 0.00 -0.40 4.89 711. HD 216899 sd:K6pec 1.12 0.00 9.84: 712. HD 217014 G3V 0.57 0.00 0.05 4.11 713. HD 217143 MD-Ba-KOIII 0.81 0.08 -0.34 -0.04 714. HD 217786 GOV 0.53 0.00 -0.06 4.52 715. HD 217877 F9V 0.53 0.00 -0.09 4.47 716. HD 218201 G3V 0.55 0.00 0.00 5.01 717. HD 218249 K2V 0.66 0.00 -0.03 5.86 718. HD 218356 MD-K1III 0.87 0.11 -0.43 0.32 719. HD 218502 sdF7extr 0.48 0.00 -2.08 4.59 720. HD 218527 MD-G7III 0.72 0.00 -0.38 0.94 721. HD 218549 A5IV, A Boo? 0.24 0.07 1.05 722. HD 218566 K3V 0.75 0.00 -0.04 6.75 723. HD 218634 M5II-III+A1V 1.17 0.08 724. HD 218732 MDGE-K0: 1.18 0.04 -1.56 -2.11 725. HD 218804 F5V 0.46 0.00 -0.21 3.80 726. HD 218857 MDGE-G3 0.57 0.10 -2.03: 0.27 727. HD 219116 MD-Ba-G8III-IV 0.73 0.04 -0.35 1.88 728. HD 219134 K3V 0.72 0.00 0.13 6.52 729. HD 219175 MD-F9V 0.52 0.00 -0.28 4.32 730. HD 219210 BS-sdF5 0.45 0.00 -0.64 3.45 731. HD 219449 K1III 0.81 0.00 0.00 0.84 732. HD 219615 MD-G8III 0.74 0.00 -0.47 0.83 733. HD 219617AB sdF8extr 0.50 0.00 -1.67 5.05 734. HD 219623 F9V 0.53 0.00 -0.09 4.40 735. HD 219685 MD-K4III 1.05 0.00 -0.44 -0.45 736. HD 219715 MDSGE:G3pec,sd? 0.58 0.06 -1.06 4.91: 737. HD 219829AB K0V 0.65 0.00 -0.11 5.99 738. HD 219834A G7IV 0.60 0.00 0.29 3.03: 739. HD 219877A MD-F3IV 0.42 0.00 -0.26 2.99 740. HD 219953 MD-K0V 0.66 0.00 -0.50 6.35 741. HD 219983 MD-F7V 0.50 0.00 -0.32 3.27 742. HD 220009 MD-KlIII 0.86 0.05 -0.57 0.06 743. HD 220182 KOV 0.64 0.00 -0.10 5.74 744. HD 220339 K2V 0.68 0.00 -0.08 6.09 745. HD 220460 MD-F7V 0.48 0.00 -0.50 3.53 746. HD 220787 (He)-B3 747. HD 220859 MD-G8III 0.76 0.04 -0.44 0.71 748. HD 221148 K2III 0.82 0.00 0.14 1.73 749. HD 221170 MDGE-G8 0.78 0.11 -2.15 -1.46 750. HD 221354 KlV 0.67 0.00 -0.05 5.72 Classification of Population II Stars 81 Table 8 (continued) No. Name Spectrum (Y-V)0 Ey-V [Fe/H] Mv 751. HD 221356 MD-F8V 0.51 0.00 -0.25 4.82 752. HD 221377AB BS-sdF3 0.43 0.05 -0.75: 3.33 753. HD 221409 MD-KlIII 0.86 O.Ol -0.36 0.56 754. HD 221503 K9V 0.88 0.00 7.68 755. HD 221585 G7IV-V 0.62 0.00 0.21 4.49 756. HD 221613 MD7-G1V 0.55 0.00 -0.19 4.78 757. HD 221822 MD-G7V 0.59 0.00 -0.20 5.56 758. HD 221830 MD-GOV 0.56 0.00 -0.39 4.94 759. HD 221851 K1V 0.67 0.00 -0.04 6.07 760. HD 221858 MDG-G5 0.72 0.03 -1.25: 0.02 761. HD 221950 sdF5 0.49 0.00 -0.70: 3.49 762. HD 222107 MD-G9III 0.79 0.00 -0.57 0.64 763. HD 222143 G3V 0.58 0.00 -0.02 5.04 764. HD 222368 F6V 0.48 0.00 -0.09 3.33 765. HD 222404 K2III 0.79 0.00 0.14 1.01 766. HD 222455AB K2III 0.85 0.01 -0.04 0.76 767. HD 222591 G8V 0.59 0.00 0.11 4.94 768. HD 222717 MD-F2IV 0.41 0.00 -0.29 2.94 769. HD 222766 MD-G5V 0.57 0.00 -0.33 5.38 770. HD 222794 MD-G1V 0.58 0.00 -0.53 5.24 771. HD 223065 (A3:IV) 0.29 0.00 1.05 772. HD 223130 MD-F5V 0.46 0.02 -0.31 3.56 773. HD 223238 G2V 0.55 0.00 0.07 4.53 774. HD 223241 G2V 0.56 0.00 -0.06 4.68 775. HD 223498A G8V 0.61 0.00 0.12 4.99 776. HD 223617 MD-K2III 0.84 0.02 -0.29 0.58 777. HD 223778 MD7-K3V 0.73 0.00 -0.25 7.34 778. HD 223782 K5V 0.76 0.00 0.01: 6.65 779. HD 224014 G7Ia 0.81 0.38 -9.0 780. HD 224085 (MD-KOIV:), VB? 0.78 0.01 -0.77 781. HD 224087 MD-KOV 0.65 0.00 -0.31 6.11 782. HD 224156 G8V 0.62 0.00 -0.06 5.40 783. HD 224233 G2V 0.56 0.00 -0.01 4.72 784. HD 224342 RHB-G5 0.55 0.10 -0.94 0.64 785. HD 224458 MD-G9III 0.78 0.00 -0.32 1.00 786. HD 224532 MD-G3V 0.61 0.00 -0.65: 5.91 787. HD 224618 MD-KOV 0.61 0.00 -0.22 5.76 788. HD 224635/6 MD-F8V 0.52 0.00 -0.23 4.41 789. HD 224745 KOIV 0.68 0.03 -0.22 3.16 790. HD 224828 MD-G2V 0.57 0.00 -0.47 5.08 791. HD 224927AB BS-sdF3 0.39 0.00 -1.31 3.15 792. HD 224930 sdG3 0.57 0.00 -0.57 5.66 793. HD 224959 Cl.lCH 0.81 0.04 -0.82 794. HD 225185 G5V 0.58 0.00 0.00 4.76 795. HD 225239 MD-G1V 0.59 0.00 -0.57 4.88 796. HDE 228710 MD-GOV 0.54 0.01 -0.36 4.90 797. HDE 231510 MD7-G9V 0.63 0.00 -0.23 5.96 798. HDE 233891 MDGE-G5 0.65 0.08 -1.71 -0.07 799. HDE 235674 G8V 0.60 0.00 0.11 5.07 800. HDE 229274 RHB-GO 0.57 0.03 -1.51 0.50 82 A. Bartkevicius and R. Lazanskaite Table 8 (continued) No. Name Spectrum (Y-V)0 Ey-V [Fe/H] MV 801. HDE 231014 MD-G9III 0.76 0.05 -0.37: 0.82 802. HDE 232078 (MDGE-K2) -1.23 -1.55 803. HDE 239124 RR Lyr-F5: 0.44 0.02 -1.53 0.75 804. HDE 250792A sdG3extr 0.60 0.00 -1.65: 5.73 805. HDE 283750 MD-K4Vpec 0.81 0.00 -0.34 6.71 806. HDE 284248 sdF5extr 0.48 0.00 -1.70 4.68 807. HDE 338529 sdF7extr 0.47 0.00 -1.90 4.36 808. HDE 340667 G2Ia, RV Tau? 0.71 0.18 (-7.90) 809. HDE 340667 G2Ia, RV Tau? 0.66 0.17 (-9.00) 810. HDE 345957 sdF7extr 0.51 0.03 -1.58 4.94 811. HDE 355547 sdF9 0.54 0.01 -0.90 4.55 812. LTT 114 (sdM5) 11.73: 813. LTT 137 sdM2: 1.15 0.00 10.56 814. LTT 300 sdG5extr, WD? 0.65 0.00 -1.85 6.21 815. LTT 458 sdGl 0.53 0.00 -1.09 5.33 816. LTT 1566 sdF8extr 0.49 0.00 -1.54 4.95 817. LTT 5299 sdG3extrpec 0.56 0.15 -2.32 8.36 818. LTT 5454 sdG2extr 0.56 0.02 -1.66 5.63 819. LTT 9239 sdG5extr 0.57 0.01 -1.80 6.34 820. LTT 10049 (sdK7:) 10.33 821. PU Vul UU Her?-A3Ia 0.20 0.33 -1.04 -8.0 822. RR Lyr (ip =0.0 ) BHB-A9 0.30 0.02 -1.20 0.99 823. RR Lyr (ip =0.15) BHB:/RR Lyr:-F3 0.38 0.02 -1.35 0.88 824. RR Lyr ( TN n n a t «o M M , _ -. co i« rt m •^(NMrtCUTPCOCN-^CÛ HDHtíOI«,, I T[ TT YI I I I I I i «rttOOTOOQOiOOt I I I I I I I I I I OHNnuiuîiûsooco •»iciocOHNictocon HHHHHC4N(SN»»oooooiOONnNv ¿«OOOOOjgS ÜOÜÜÜOOÜÜO OOOOOOOOOO ouoouooaii o HMP11HO(DS«00)0 «NOfUŒSOOOO 1I1I1I1I1I1I1I1I1ICS COCOCOCOCOCOCOCOCO^* Z NWMfflNMNNMN Classification of Population II Stars ONuin l-COONOJOWHhlft US C0 CÛ O) (D Ol _ .. 01 o « ñ 00 H co^oooi kAiaiACOOO — — (O U1 h ^ U) Ifi )A (Û t- K t- t- O — — — C4C4C4C4C4 Gì OI Ol 01 w <01 01 01 01 8ÖOOOOOOOO ÛQQQÛQOQQQ ÛÛQQÛÛÛÛQQ QQQQQQQQQQ X S X £ X S X X X X X X X X X X X X X X X X X X X X X X X X rlMm-ÍUÍCOÍ-OOOlO HMBíiíSOMOSO HNrtVkÔtÔNûÔoiQ cococortcocooeírt^ cocococococococococo COCOCOCOCOCOCOCOCOCO Classification of Population II Stars
0>(0 -— ««B^nti-HitfO) O (S <0 — — —- NMOOoiHviosovioOSO — N ooHNNnnn^i——————————' —————————— @Nt-SS0O0O»0O0— — — — — —O — — — — «NWW^NMCSCSN CSCSCSCSCSCSCSCSCSCS ÛÛÛÛÛÛÛÛÛÛ QQÛÛÛÛDÛÛQ QQQQQQPPQQ X X X X X X S X X Xïïïïïïïïï ï XIXXXXXXXX ¡c^có^fictfit^oooiò fHMcô^wœsoÔÂd — escó^-indt-'oooid OlOCiOlwOlÂQO t-t-t-t-Nt-t-i-i-i000000000—- — — — — — — — — — CS Classification of Population II Stars