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Astron. Astrophys. 320, 74-78 (1997)

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4. Discussion and conclusion

The radial velocity observations and photometric data obtained for this new sample of stars in the wide surrounding of the Pleiades confirmed the membership of some 25 new stars. There are a few ambiguous cases: the membership evidences from radial velocity and photometry are contradictory. The rate of success (25/93) is much less than in the previous sample (56/83), which can be explained by two factors: (1) the first sample was selected on the basis of proper motions and photometric data, while the second one is based only on proper motions because no photometric data were available; (2) the data from Artjukhina & Kalinina (1970) have larger errors and many field stars appear (in their data) to have proper motions close to that of the Pleiades. The proper motion of the Pleiades represents usually a very selective criterion for membership (Schilbach et al. 1995). But because of the larger errors, it is also possible that real Pleiades members have not been selected in the member list due to their proper motion being beyond the limiting criterion, while many field stars have been considered erroneously in the candidate list. It is therefore quite probable that the sample of corona members is still not exhaustive.

Complementary radial-velocity observations are suggested for a few probable members that we cannot observe with CORAVEL because they are hotter than F5 and it would be useful to get independent observations of several stars with contradictory membership assignements from the kinematics and the photometry. It would be also very important for the study of the Pleiades and the understanding of the structure of the cluster to search for the Pleiades members in the magnitude range 9.5 [FORMULA] 15 (or even to fainter magnitudes, if possible), corresponding to the G- and K-type dwarfs out to about [FORMULA] from the cluster center.

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© European Southern Observatory (ESO) 1997

Online publication: July 3, 1998
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