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197Lapj...163..313E the Astrophysical Journal, 163 The Astrophysical Journal, 163:313-331, 1971 January 15 (c) 1971. The University of Chicago. All rights reserved. Printed in U S A 197lApJ...163..313E NARROW- AND BROAD-BAND PHOTOMETRY OF RED STARS. V LUMINOSITIES AND TEMPERATURES FOR YOUNG DISK- POPULATION RED STARS OF HIGH LUMINOSITY O. J. Eggen Mount Stromlo and Siding Spring Observatories, Research School of Physical Sciences, Australian National University Received 1970 July 23 ABSTRACT Most of the known high-luminosity red stars, including long-period Cepheids, in the young disk- population groups, clusters, and associations in the Galaxy have been observed in the (UBVRI) system. Also, a few Cepheids and supergiants in the Large Magellanic Cloud are included. No clues to possible differences between LMC and galactic stars were found. The simple relation between M(I) and Mhoi and the available temperature calibration of (R — I) make it possible to construct a composite (Mho], log 7U-diagram for luminous stars in the young disk population. This diagram may be useful in the con- struction of stellar models and in the understanding of the evolutionary state of these stars. I. INTRODUCTION Many bright red stars are now known as members of young clusters and associations. These objects therefore provide the means of calibrating the luminosities of such stars. Moreover, the simple relation between the infrared and bolometric luminosities of these stars, and the available temperature calibrations of (i?, I) indices, make it possible to construct (Mboh l°g Te)-diagrams with some confidence. The young disk population is defined as that population younger than the Hyades Cluster, or some 5 X 108 years, and with space-motion vectors, (U, F), falling in the restricted region of the (Z7, F)-plane populated by the bright A-type stars (e.g., Eggen 1969tf, Fig. 1). A list of young disk groups, associations, and clusters containing bright red giants is given in Table 1, with the moduli and reddening values taken from the listed sources. These clusters are listed in order of diminishing luminosity of the brightest red stars and\therefore, roughly, in the order of increasing age. II. OBSERVATIONS Most of the objects in Table 1 are in the southern hemisphere, and the (UBVRI) observations have been made with the 40-inch reflector at Siding Spring Observatory. The few northern objects were observed with Mount Wilson telescopes. The (R, I) observations are on the Kron system (Kron, Gascoigne, and White 1957 ; Eggen 1968a, 1971) and were obtained with an ITT FW 118(S1) photomultiplier with the use of the original filters kindly made available by Dr. Kron. A few of the brighter stars were observed in the narrow-band (102, 65, 62) system (Eggen 1967; Eggen and Stokes 1970) and transformed to the (R, I) system (Eggen 1969¿>). Unless otherwise specified, all values of R and R — I used here are on the Kron system. The observations of all but the periodic variables are listed in Table 2. The interpreta- tion of some of the numbering systems in clusters is given in the references in Table 1. The spectral types listed in Table 2 are also mainly from the references in Table 1. III. THE HYADES GROUP The Hyades stars represent the oldest objects in the young disk population. The red-giant members of the group are listed in Table 3, together with the (UBVRI) 313 © American Astronomical Society • Provided by the NASA Astrophysics Data System 314 O. J. EGGEN photometry; the reddening, E(B — F), obtained from early-type stars in the vicinity of the red stars; the space motions (UVW) and their correction (At/, AF, AfF) for a 10-pc increase in the star’s assumed distance; the group modulus, m — M, and resulting 197lApJ...163..313E group parallax, Trg; and the galactic latitude, and the spectral type, from various sources. The giants in the Hyades and Praesepe Clusters are listed in Table 4. The group giants are shown in the (Mj, R — /)-plane of Figure 1. The variability of the three reddest stars is indicated by boxes. The well-defined giant sequence in Figure 1 was noted previously in connection with the (Af[102], [102, 65])-plane (Eggen 19696; the present calibration of the relation between Mk0\ and — / is a slight revision of that tabulated in Table 5 of this reference). The mean giant sequence between R — I = +0.3 and +0.4 mag in Figure 1 is shown schematically in Figure 2 where the mean values of the four giants (K0 III) in both the Praesepe and Hyades Clusters (Table 4) are represented by filled circles. Also, the earlier-type giant in Praesepe (HD 72779, GO HI) listed in Table 4 is shown in Figure 2 as an open circle together with the appar- ently discordant star in Figure 1 (HD 71369, M(I) = —0.7 mag; R — I = +0.28 mag; G5 II-III). These two objects may be slightly more massive, or slightly older, TABLE 1 Clusters and Associations with High-Luminosity Red Stars Object Clustér (m—M)o E(B—V) Source LMC 18.45 -fO. 05 Sandage and Tammann 1968 Cr 121 9.0 -j-0.03 Feinstein 1967 h and x Per 11.90 4-0.36 Eggen 1967 D NGC4755 11.86 +0.48 Feast 1963 21 NGC3293 12.08 +0.38 Feast 1958 a Sco II Sco 6.1 4-0.06 Eggen 1967 HD 101712 IC 2944 11.50 -f-0.33 Thackeray and Wesselink 1965 TV Gem I Gem 10.2 4-0.40 Eggen 1957 T12, R NGC3766 11.4 +0.19 Sher 1965 l Car ... 8.8 +0.27 Fernie 1967 RS Pup Ill Pup 11.3 4-0.55 Sandage and Tammann 1969 ô Lyr ô Lyr 7.5 +0.05 Eggen 19686 NGC 2451 7.1 4-0.05 Feinstein 1966 a Per. a Per 6.25 4-0.05 Eggen 1964 HD 66342 NGC 2516 7.5 4-0.12 Evans et al. 1961 Pleiades Eggen 1965 (Table XVI) SNor NGC 6087 9.76 +0.23 Sandage and Tammann 1969 BM Sco NGC 6405 8.5 +0.13 Eggen 1961 USgr M25 8.98 -j-0.55 Sandage and Tammann 1969 NGC 2287 9.1 0.0 Cox 1954 NGC 6705 11.0 +0.42 Johnson et al. 1956 Fig. 1.—Hyades giants in the {MJyR — I) plane. 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