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Pub. Astron. Soc. Pacific, Volume 83, June 1971 the ARCTURUS GROUP O. J. EGGEN Mount Stromlo and Siding Spring Observatories, Re

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Pub. Astron. Soc. Pacific, Volume 83, June 1971 the ARCTURUS GROUP O. J. EGGEN Mount Stromlo and Siding Spring Observatories, Re Pub. Astron. Soc. Pacific, Volume 83, June 1971 THE ARCTURUS GROUP O. J. EGGEN Mount Stromlo and Siding Spring Observatories, Research School of Physical Sciences, The Australian National University Received 15 March 1971 Fifty-three probable members of a group of old disk population stars, moving with Arcturus, are discussed. The group includes the long period (250e1) variable RT Hydrae. The {My, B—V) and (Mboi, fí—/) diagrams of the group stars show the members to be among the oldest of the old disk population, similar in age, but not in chemical composition, to members of the old cluster NGC 188. Apogalactium for the group members is near the sun and there is some evidence for a nonrandom distribution of the U vectors of the space motions. The ultraviolet excess, 8(C/—ß)o.6' of the main-sequence members is +0Φ11 and spectroscopic analyses of three giant members give [Fe/H] near —0.5. The values of S{U— B)q q for seven groups of old disk population stars range from + 0Φ17 (σ Puppis group) to + 0^03 ( ε Indi group) with the old disk cluster M67 being similar to the latter. The value of E{B—V) = +0^06 for M67 is confirmed by early-type field stars in the vicinity of the cluster. The members of some of the old disk population groups that populate the (Μ^,Κ — Ι) plane near the clump of red giants (M^ol == 0m to + lm) are tabulated and discussed in connection with the suggested "supermetallicity" of some of these stars. It is concluded that the old disk popula- tion clusters and groups contain stars with values of [Fe/H] ranging from that of the Hyades to about 20 percent that of the sun. Available narrow-band photometric indices of early K-type giants are not directly useful for determining [Fe/H]. Key words: old disk stars — elemental abundances — photometry I. Introduction The (UBV) observations have been made in The large and well-determined parallax, several programs over many years. The (RI) σ/091 (weight 50), of Arcturus (HR 5340 = a results were mainly determined with the 40-inch Bootis) leads to space motion vectors of ((7, V, W) reflector at Siding Spring or with the Mount = ( — 25, —116, —3) km/sec. The common Wilson and Palomar Observatories' facilities. space motion of Arcturus and HR 7405 (a Vul- In a few cases, as noted, observations by others peculae has already been noted (Eggen 1969α), have been used. All {RI) results are on the Kron and recent studies of the motions of subgiants system (Kron, Gascoigne, and White 1957; Eggen and main-sequence stars have shown that among 1968α, 1971α). the relatively small number of objects near the The U vectors of the group members are dis- sun with space velocities of this size a significant tributed between —15 and —75 km/sec as percentage may be moving with Arcturus. These shown in Figure 1. A search for possible group stars are listed in Table I together with the (UBV) members with U vectors between 0 and —10 and {Rl) photometric results; the number (N, N) km/sec and between —75 and —85 km/sec of (UBV) and (RI) observations, respectively; yielded no additional members. the group parallax, ng, and the resulting modu- lus, m — M; the space motion vectors {U, V, W) II. (Mbob R—l) and (My, B—V) Relations and their change for a 100-parsec increase in The members of the Arcturus group listed in the distance (dU, dV, dW); the proper motions, Table I are shown as open circles in the (My, μ; the radial velocity, p, and spectral type; and B—V) plane of Figure 2. A few members of the either individual trigonometric parallax deter- very old, disk population cluster NGC 188 minations with their weights, designated by the (Eggen and Sandage 1969) are also shown in usual observatory abbreviations, or the mean Figure 2, as crosses. The cluster and the group parallax and its total weight, in parentheses. are probably of about the same age although the 271 © Astronomical Society of the Pacific · Provided by the NASA Astrophysics Data System 272 O. J. EGGEN TABLE I Members of the Arcturus Group HD Ve V-V U-B m-M U V W Ha Name R R-I Ν, Ν π. dU dV dW Sp. T. km/sec (O'/OOl) (o:'ooi) 3266A 8?43 +0^66 - 15 -116 - 72 + 180 - 52.0 2 8 A ( 2 0 ) ADS497A 4,- 0.017 + 11 -129 -167 -405 G2 V Β 9.25 +0.69 +0.14 4,- G5 V 4308 6.54 +0.655 +0.11 1.88 - 52 -116 - 26 + 160 + 98.4 40C(8) -66053 5.99 + 0.19 2.1 0.042 - 78 -276 +217 -741 G3 V 61Y (7) -53077 9. 84 + 0. 84 +0.44 4.16 - 25 -116 + 114 + 70 - 58.2 19C(6) LTT 195 9.47 +0.35 2.2 0.015 - 63 -198 + 92 -474 K3 V 0Y ( 8) 4744 7.60 + 1.06 +0.79 3.95 - 16 -116 + 87 +224 -162.8 -6A(20) +290141 7.15 +0.39 1.1 0.016 + 66 - 65 - 14 - 30 G8 IV 6497 6. 42 + 1.18 + 1.26 4.95 - 16 -116 - 42 + 107 - 95.5 HR 316 5. 86 + 0.42 2, A* 0.010 + 42 - 36 - 53 -116 K2 III 6734 6. 45 +0.85 +0. 47 3.30 - 50 -116 + 40 + 138 - 95.4 22Y(12) 29 Cet 6.02 +0.335 2.2 0.022 - 41 -186 + 94 -422 KO IV 12369 7.00 + 1.42 7.68 - 64 -116 + 70 + 27 - 68.6 -2507 89 0.003 - 13 - 36 + 1 - 76 Κ4 III +480739 9. 82 +0.96 + 0.68 3.68 - 48 -116 + 9 + 76 - 97.0 18M ( 8 ) LTT 10 887 9.31 +0.36 1,1 0.0185 + 50 100 -150 -398 dK6 64Yk(6) 17820 8. 40 +0.53 -0.06 4.20 - 23 -117 - 84 + 45 + 6.1 +10o380 0.0145 - 59 -169 -116 -439 GO 22225 7.52 + 1.50 8.24 - 18 -116 - 43 + 6 - 8.5 GC 4276 6. 40 +0.935 1,2 0.002 - 3 - 26 - 11 - 40 gM2 24002 8.59 +0.84 +0.42 2.91 - 47 -116 - 15 + 260 - 16.0 25 (52) +0o659 0.026 - 88 -307 - 65 -635 Kl V 31560 3.12 + 1.08 4.95 - 67 -116 + 40 + 192 + 12.5 24C(7) ~2801839 0.010 - 76 -112 + 49 -234 K5 50806 6.02 +0.715 +0.255 3.20 - 53 -116 0 + 177 +171.5 34Y(10) -2 803554 5.69 +0.235 2,2 0.023 -206 -133 + 34 -440 G5 IV 3 8C(7) + 330169 4 10.11 +1.02 +0.82 3.15 - 70 -116 - 68 0 - 78.0 30V(10) G51-10 9.69 + 0.42 2.1 0.0235 - 13 -302 - 61 -640 dK6 4 4M ( 7 ) 71250 5.56 + 1.61 +1. 88 7.30 35 -116 - 79 - 23 - 7.3 26W(8) 27 Cnc 4.26 + 1.08 2.2 0.0035 10 - 42 - 26 -106 gM3 71887 7. 40 + 1.62 + 1.05 8.35 60 -116 15 + 17 + 40.0 253d RT HYA 4. 85 + 1.74 MAX 0.002 20 - 19 - 55 gM6e 75530 9.19 +0.73 +0.215 3.80 28 -116 - 90 -166 + 35.0 14C(7) -402 46 8 8.94 +0.275 2.3 0.0175 80 - 50 -180 -492 G8 V +10o2122 9.92 +0. 88 +0.555 3.45 - 58 -116 - 70 - 50 - 16.6 -7V(12) G 43-34 9. 44 +0.325 2,2 0.0205 -105 -254 -119 -626 dK5 23Y(7) 233719 9.54 + 1.10 +0.94 2.61 - 29 -116 + 21 + 96 - 24.5 2 6M(7) +5301395 8. 83 +0.47 2,2 0.030 - 44 -334 + 120 -748 dMO 69Yk(6) 90508 6.46 +0.605 +0.04 2.33 25 -116 + 30 + 84 - 6.6 53A(28) +4901961 6.20 + 0.24 3.4 0.034 74 -395 + 122 -885 G1 V 40M (7) 94518 3. 35 +0.60 -0.03 3.53 27 -116 - 33 -100 + 92.5 37C(7) -30o8807 0.020 39 - 64 -143 -326 G2 V © Astronomical Society of the Pacific · Provided by the NASA Astrophysics Data THE ARCTURUS GROUP 273 TABLE I (C HP Ve B-V U-B m— M u V W μα 7r(tríg) Name R R-I Ν, Ν dU dV dW Μδ Sp. T. km/sec (orooi) (o':ooi) Wolf 397 + 1. 19 - 26 - 116 - 68 - 250 + 37.0 33(40) G 10-25 9.48 +0.525 3, 4 0.048 -148 - 480 -221 -1130 dMO 106516 6.12 + 0. 47 -0.14 2. 80 - 67 - 116 -101 + 33 + 6.4 28(25) HR 4657 5.99 + 0.14 2,1 0.0275 -334 - 306 -289 -1018 F6 V 111515 8. 13 +0.69 + 0.10 3.40 - 56 - 116 - 67 - 72 - 3.9 31(15) + 2025 85 7.99 +0.255 2, 1 0.021 -122 - 248 -134 - 646 G8 V 115577 6. 80 +0.98 +0.655 3.70 - 75 - 116 + 69 - 61 +152.5 -2 709145 6.47 +0.38 1.1 0.018 + 12 - 36 - 30 G8 IV 115062 6.94 +1.575 +1.875 8.20 - 11 - 116 - 34 30 + 273 56 Vir 5.90 +0.795 2.2 0.002 + 2 - 24 - 12 48 gM2 123598 7. 10 +1.595 + 1.
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