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1972Apj...173...63E the Astrophysical Journal The Astrophysical Journal, 173:63-86,1972 April 1 © 1972. The University of Chicago. All rights reserved. Printed in U.S.A. 1972ApJ...173...63E NGC 2516 AND THE PLEIADES GROUP O. J. Eggen Mount Stromlo and Siding Spring Observatories, Research School of Physical Sciences, Australian National University Received 1971 July 19; revised 1971 November 5 ABSTRACT UBV observations to visual magnitude 16 are given for stars in NGC 2516 together with new UBV observations of members of IC 2602 and 2391 and intermediate-band results for the members of the ^ Sculptoris cluster. The clusters of the Pleiades group are found to represent a considerable age spread (1-8 X 107 years), and this is confirmed by both the luminous blue and red group members unattached to clusters. The B-type stars in the younger (a Persei) and older (Pleiades and NGC 2516) group clusters closely define the same relation between the H/3 intensities and the luminosities, but the young group cluster IC 2602 and the similar, non-group cluster IC 2391 give anomalous results both in the (My, j3)-relation of the hot stars and in the luminosities derived from the A-type and F- and G-type main-sequence stars from the intermediate-band indices. The early-type group members in the general field, including several of the brightest members of the Scorpius-Centaurus stream, appear to represent the same age spread as the clusters in the group and also define the same (Mv, /3)-relation as the B-type stars in the a Persei and Pleiades clusters. The clusters in the group contain several late-type high-luminosity stars, and the group members in the general field include such bright stars as a Car, a Sco, and several F- and G-type objects of luminosity class II. The distribution of group members in the (Mhoh l°g F«)-plane is understandable in terms of evolutionary tracks for stellar models of masses 5-15 30?©. The lower limit of the temperature of the luminous group stars is some 600° hotter than for the members of the older Hyades group, and this probably explains the apparent absence of “normal” red variables in the Pleiades group. However, the group probably contains the hotter, erratic N-type variables at Mho\ near —5 mag. I. INTRODUCTION It was previously noted (Eggen 1964, 1965) that several bright clusters of early-type stars had common space motion with the Pleiades cluster. The members of this Pleiades group include NGC 2516, IC 2602, and the a Persei cluster. The present paper presents UBV photometry, to V near 16 mag, for members of the cluster NGC 2516 and discusses the available broad- and intermediate-band photometry of the other clusters in the group, comparing the results with the available photometry of similar clusters that are not members of the group. II. NGC 2516 The cluster NGC 2516 {a = 7h58m, b = —60°40'; 1950) is located in Carina at a galactic latitude of 6 = —16°. Cox (1955) has published photometric results on the {PV) system for some of the brighter stars, and single observations on the UBV system were published by Dachs (1970) for 70 stars brighter than visual magnitude near 11. Com- paring his results with those of Cox, Dachs found the relation B — V = 0.955 (P — V) + 0.125 mag, which is close to that based on much more extensive data (Eggen 1955); P — F = 0.965 (P — F) + 0.12 mag. New results for 145 stars are listed in table 1. These stars are identified in figure 1 except for a few HD stars lying outside the area of the figure. The cluster is of particular interest because of the presence of three red giants, No. 42, B, and HD 65662 (Cox 1955; Evans et al. 1961), and of several peculiar A-type stars (Hyland 1967a, b; Abt and Morgan 1969), Nos. 21 (Mn n star), 63 © American Astronomical Society • Provided by the NASA Astrophysics Data System TABLE 1—Observations of Stars in NGC 2516 Fe B—V U-B Fe B—V U-B Eggen Cox (mag) (mag) (mag) N Eggen Cox (mag) (mag) (mag) N 1972ApJ...173...63E 1 14.55 +0.76 +0.14 1 74 +0.23 +0.12 2 47 9^67 2 +0.125 +0.12 2 75 +0.39 28 +0.109.94 1 46 10.39 3 +0.83 ... 1 76 +0.56 +0.0316.27 1 11.98 4 +0.67 +0.16 1 77 +1.035 +0.9215.67 2 13.10 5 +0.615 +0.04 1 78 +0.865 +0.6113.01 1 15.35 6 +0.86 +0.52 1 79 +0.885 +0.3714.86 2 14.04 7 +0.73 +0.21 1 80 +0.19 +0.1513.65 2 45 9.88 8 +1.19 +1.00 1 81 +0.105 +0.0114.00 2 43 9.40 9 +0.69 +0.14 1 82 +0.08 71 +0.04512.22 2 58 9.66 10 +0.94 +0.38 1 83 +0.815 +0.2014.34 1 15.40 11 +0.38 +0.07 2 84 44 10.90 +0.33 56 +0.17511.38 2 12 +0.82 +0.28 1 85 +0.615 +0.04513.77 2 12.74 13 +1.18 +0.36 1 86 +0.535 +0.0115.18 2 12.25 14 +0.245 +0.16 1 87 +0.16 35 +0.08510.52 1 50 10.12 15 +0.93 +0.605 1 88 +0.555 0.0013.99 2 Ill 11.41 16 +0.945 +0.42 2 89 49 9.83 +1.34 +1.4414.21 3 17 +0.715 +0.12 1 90 +0.66 +0.08514.30 1 12.87 18 +0.87 +0.405 1 91 +0.505 +0.05514.02 1 79 11.67 19 +0.80 +0.255 1 92 +0.73 +0.14516.29 2 13.43 20 +0.925 +0.48 1 93 +0.14 +0.1114.38 2 53 10.52 21 +0.01 -0.33 2 94 +0.615 B +0.0156.86 1 12.51 22 +0.07 +0.035 1 95 +0.935 +0.4359.48 1 14.33 23 -0.03 -0.31 2 96.. +0.685 +0.3756.75 1 15.29 24 -0.01 -0.21 2 97 12.93 +0.805 37 +0.398.22 1 25 +0.20 +0.15 2 98.. +0.675 38 +0.089.55 1 14.68 26 +0.475 +0.30 1 99 d 8.59 +0.035 -0.1814.55 2 27 +0.92 +0.46 3 100 +0.05 -0.10514.55 3 b 7.20 28 +1.15 +0.97 2 101 +0.045 -0.20512.74 1 83 8.40 29 +0.49 +0.17 1 102 +0.575 96 +0.01511.26 1 11.95 30 +0.325 +0.205 2 103 +0.61 97 +0.05510.86 1 12.05 31 +0.07 -0.07 2 104 +0.05 2 -0.228.82 2 c 8.95 32 +1.05 +0.65 1 105 +0.745 +0.0814.07 i 12.92 33 +0.68 +0.06 2 106 +0.80 +0.3014.48 1 13.35 34 +0.715 +0.175 2 107 +0.155 +0.13514.35 2 57 10.18 35 +0.79 +0.18 1 108..... ... 14.50 +1.015 +0.8513.46 1 36 +0.94 +0.55 1 109 +0.025 -0.2114.57 2 10 7.79 37 +1.06 +0.81 1 110 +0.72 +0.0814.06 2 12.86 38 +0.08 +0.04 1 111 +0.915 1 +0.269.05 1 14.08 39 +1.50 +1.68 2 112 +0.83 +0.3211.66 1 13.78 40 0.00 -0.14 4 113 +0.09 41 8.9-9.10.00 2 9 9.31 41 +0.63 +0.03 1 114 +0.70 +0.1013.44 1 13.09 42 +1.285 +1.175 2 115 +0.80 a +0.266.72 1 ... 14.53 43 +0.54 +0.05 2 116 +0.27 +0.1912.03 1 42 10.64 44 +1.20 +1.13 1 117 +0.77 +0.1512.21 1 14.27 45 +0.755 +0.15 1 118 +0.76 +0.2013.99 2 13.83 46 +0.335 +0.135 2 119 +0.50 55 +0.0610.96 2 95 11.76 47 +1.475 120 +0.415 +0.1013.99 1 11.14 48 +0.43 +0.07 1 121 +0.425 +0.19515.05 1 12.23 49 54 10.56 +0.29 +0.135 2 122 +0.09 +0.045 2 94 9.62 50 +0.61 +0.06 1 A 22 9.64 +0.20 +0.1611.74 2 51 +0.44 +0.19 1 B 110 5.16 +1.75 +1.8314.44 3 52 -0.10 -0.79 2 C 20 8.40 +0.02 A - 0.1955.79 3 53 +0.28 +0.14 4 D 17 9.79 +0.19 21 +0.0910.80 3 54 +0.66 +0.105 2 EA 9.53 +0.10 27 +0.0210.40 2 55 +0.615 +0.02 1 EB 9.52 +0.055 +0.0513.97 2 56 +1.02 +0.60 1 F 51 10.78 +0.29 +0.13514.71 2 57 +0.65 +0.15 1 G 18 9.60 +0.075 +0.07513.57 2 58 +0.70 +0.21 1 H 15 7.62 -0.06 -0.4213.79 3 59 0.00 -0.18 4 1 11 8.55 +0.055 26 -0.049.13 2 60 +1.055 +0.90 1 J 14 9.44 +0.04 +0.00514.95 2 61 +0.08 +0.06 2 K 91 8.39 -0.04 24 -0.3659.68 2 62 +0.525 +0.10 1 L 12 9.15 +0.105 25 +0.099.85 2 63 +0.96 +0.44 2 M 101 10.20 +0.16 +0.20514.36 1 64 +0.615 - 0.005 2 N 13 8.07 -0.04 73 -0.3212.38 3 65 +0.58 +0.005 2 0 8 9.69 +0.135 74 +0.0711.91 2 66 +0.63 +0.10 2 P 3 9.45 +0.075 -0.01514.48 1 67 +0.64 +0.045 1 Q 14.80 +0.59 75 +0.05512.06 2 68 +0.04 - 0.145 3 HD: 19 7.87 69 +0.41 +0.125 1 65599.
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