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1. Introduction 2. Hyades Supercluster

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1. Introduction 2. Hyades Supercluster THE ASTRONOMICAL JOURNAL, 116:284È292, 1998 July ( 1998. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE AGE RANGE OF HYADES STARS OLIN J. EGGEN Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatories,1 Casilla 603, La Serena, Chile; oeggen=noao.edu Received 1997 December 29; revised 1998 March 12 ABSTRACT On the basis of canonical models, the age of Hyades supercluster stars, whether in the Hyades and Praesepe clusters or the noncluster Ðeld, ranges from (5È6) ] 108 to 109 yr. The di†erence between the parallax derived from the supercluster motion and that obtained from Hipparcos observations has a dis- persion only twice that of the mean dispersion of the individual Hipparcos values. The supercluster appears not to contain red giants on the Ðrst ascent of the red giant branch, but only asymptotic giant branch (““ clump ÏÏ) stars. The masses obtained for individual components of binary stars in the super- cluster show a dispersion of less than 10% when compared with model predictions. Key words: open clusters and associations: individual (Hyades) È stars: evolution 1. INTRODUCTION where (t, q) are the components of the proper motion in the direction of the convergent point (a, d) and perpendicular to The Hyades cluster, because of its depth-to-distance that direction, respectively; and ratio, has become the basis for the universal metric. The lowest mass cluster members form a cluster halo, and the n \ 4.74t/(V sin j) , (3) cluster itself, together with its near-twin the Praesepe clus- clus tot whereV is total space motion of the supercluster relative ter, is part of the Hyades supercluster. This supercluster, to the Suntot and j is the angular distance between the star together with another, the NGC 1901 supercluster, forms and (a, d). The photometric luminosities have been derived the main constituent of star stream I, for which the apex of from the photometric calibrations listed in Eggen (1996). the proper motions is (a,d) \ (6h.4, 6¡.5) (B1950.0). Previous investigations of the cluster and superclusters have shown a 2. HYADES SUPERCLUSTER wider range of agesÈ8 ] 108 to 2 ] 109 yrÈthan can be 2.1. Upper Main Sequence easily explained as one, prolonged star birth event. The present discussion will be divided into two parts, The parameters for upperÈmain-sequence members of the with the upper main sequence of the supercluster discussed Hyades supercluster are listed inTable 1, where the stars in° 2.1 and red giants in° 2.2. The b photometry is mainly are identiÐed by HR, HD, and Hipparcos (ESA 1997) from the compilation byHauck & Mermilliod (1980), and numbers. Only stars not known to have photometrically the RI photometry is on the system deÐned in Eggen unresolved companions from 0.2 to 3.2 mag fainter are con- (1979). The proper motions are on the FK5 system and are sidered. The total space motion is from the references in the notes toTable 1. The observed V \ 43.5 ] 0.045X (4) radial velocities are mainly fromAbt & Biggs (1972) and tot (Eggen 1992b), where X is the distance in parsecs of the star Barbier-Brossat,Petit, & Figon (1994). For the upperÈ from the Sun in the direction opposite that of the Galactic main-sequence stars, the values oflog T are based on b. center. The computed values of the radial velocity are given A previous discussion(Eggen 1995) foundeff that by log T \ 3.881 ] 0.53(b [ 2.800) , (1) eff o \ V cos j . (5) derived from spectrophotometry(Smalley & Dworetsky comp tot The mean di†erence,, omitting the variable- 1993) for a range of Am, ultraÈshort-period Cepheid o [ o velocity stars, is 0.3 obs2.4 (1 compp)kms ,or 0.35 2.50 (USPC; d Scuti), and normal AF stars, as well as fundamen- [ ^ ~1 [ ^ km s if we include those with variable velocity. The dis- tal values ofT (Andersen 1991) derived from eclipsing ~1 persion in the mean peculiar velocity is higher, as expected, binaries. The meaneff dispersion of the di†erence between the from the supercluster members, 0.27 2.50 km s , than spectrophotometric values and those from equation (1) is [ ^ ~1 it is for the members of the Hyades cluster, 0.26 0.66 100 K. The temperatures for the red giants are from ] ^ ^ km s . BessellÏs (1979)calibration of the [(R I) , log T ] rela- ~1 [ The mean modulus for the Hyades cluster members in tion. C eff Table 1 is 3.29 mag from the cluster motion and 3.37 mag The convergent point of the proper motion of stars in from the Hipparcos parallaxes. The motion parallaxes from stream I is at (a,d) (6.4, 6¡.5) (Eggen 1996). The stars \ h the Hipparcos convergent point(Perryman et al. 1998) yield discussed here are mainly of magnitude V \ 7 and peculiar a mean modulus of 3.33 mag, andSchwan (1991) found 3.40 velocityP.V. ¹ 0.1V , with M (clus) M (phot) \ 0.25 V [ V mag. The comparison between the cluster parallaxes in mag. Here tot Table 1 and the Hipparcos results is almost identical to that P.V. \ 4.74qD(pc) , (2) discussed by Perryman et al. The overall comparison for the supercluster stars in Table 1 yields n n 0.13 1.84 mas. Four stars are omitted from ÈÈÈÈÈÈÈÈÈÈÈÈÈÈÈ [ \ ^ thisclus comparison,Hip listed inTable 2. The convergent point of 1 The National Optical Astronomy Observatories are operated by the Association of Universities for Research in Astronomy, Inc., under co- the proper motions of a critically selected 20 cluster operative agreement with the National Science Foundation. members(Perryman et al. 1998) is (a,d) \ (6h.52, 6¡.66), com- 284 TABLE 1 MEMBERS OF THE HYADES SUPERCLUSTER o (km s~1) n (mas) k XV P.V. SPECTRAL tot HR (HD) REFERENCEa (pc) (km s~1) Obs. Comp. (km s~1) M log T Cluster Hip. p TYPE NOTES HIP V eff 125.......... 1 [15 42.8 [2V [2.9 ]1.2 ]0.79 3.936 16.0 18.97 0.64 A1 E 2472 238.......... 2 30 45.1 ]2.3 ]1.4 ]0.8 ]2.15 3.865 14.9 15.00 0.72 F3 IV 1 3865 343.......... 2 23 44.55 ]9.4 ]9.1 ]0.5 ]1.28 3.905 24.8 23.73 0.68 A7 V 2 5542 (8391) ....... 2 [5 43.25 ]4.2 ]4.2 ]1.4 ]2.83 3.843 14.4 12.70 0.80 F1 V 2 6418 403.......... 1 18 44.3 ]7V ]10.0 ]0.2 ]0.28 3.896 33.1 32.81 0.41 A5 IV 3 6686 520.......... 3 [8 43.1 ]8.0 ]4.6 ]2.9 ]0.97 3.934 15.3 17.54 0.62 A1 V 8241 607.......... 3 54 45.95 ]15.0 ]18.5 ]4.0 ]0.30 3.902 9.1 11.31 0.85 A5 III 9589 733.......... 2 31 44.9 ]24V ]18.4 ]1.3 ]2.27 3.859 10.0 9.39 0.92 F0 III 4 11644 878.......... 1 25 44.55 ]28.5 ]27.0 ]0.2 ]3.28 3.820 31.2 31.40 0.84 F5 IV 13834 1036 ........ 3 144 50.0 ]34.5 ]31.3 ]0.9 ]1.06 3.889 5.8 7.78 1.66 A3 Vp 5, 6 16077 1125 ........ 2 30 45.75 ]30.0 ]32.2 [1.0 ]2.06 3.830 12.7 10.98 0.90 F2 V 17214 1201 ........ 1 35 45.1 ]35.0 ]35.1 [0.3 ]2.92 3.836 24.3 24.14 0.90 F4 V 7 18170 1233 ........ 2 37 45.15 ]36: ]34.6 ]0.5 ]3.30 3.812 23.6 25.42 1.05 F5 V 7 18658 1279 ........ 2 38 45.2 ]36.4 ]36.7 [0.1 ]2.84 3.824 23.2 21.27 1.03 F3 V 7 19261 (26345) ...... 2 40 45.3 ]35.0 ]36.8 ]0.1 ]3.44 3.815 22.7 23.22 0.92 F6 V 7 19504 1292 ........ 3 30 44.85 ]36.8 ]37.4 [0.6 ]3.07 3.829 28.5 25.89 0.95 F4 V 7 19554 1319 ........ 2 43 45.45 ]36.4 ]37.5 ]2.2 ]3.06 3.827 22.4 22.51 0.82 F5 V 7 19877 (26737) ...... 2 51 45.8 ]3.75 ]38.4 ]0.8 ]3.42 3.814 18.0 18.12 0.82 F5 V 7 19789 1351 ........ 2 40 45.3 ]42.0 ]38.4 ]0.1 ]2.48 3.864 23.9 22.31 0.92 F0 V 7, 8 20219 1354 ........ 4 41 45.35 ]42.0 ]38.0 [0.8 ]2.97 3.824 22.7 21.12 0.77 F2 V 7 20255 1356 ........ 2 41 45.35 ]36.2 ]38.4 [0.6 ]2.07 3.887 22.4 21.20 0.99 F0 IV 7, 9 20261 (27534) ...... 2 43 45.45 ]3.1 ]37.8 ]0.4 ]3.55 3.815 21.6 19.83 0.89 F5 V 7 20350 1368 ........ 2 40 45.3 ]41.2 ]38.5 [0.6 ]2.54 3.858 22.4 21.87 0.66 Am 7, 10 20400 1380 ........ 2 41 45.35 ]37.5 ]38.1 [0.3 ]1.62 3.910 22.7 22.36 0.88 A8 V 7 20542 (27848) ...... 2 43 45.45 ]37.1 ]37.8 ]0.4 ]3.54 3.804 20.3 18.74 1.17 F6 V 7 20567 1385 .......
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