Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002a%26a...386..187m&link_type=abstract
Astronomy and Astrophysics, v.386, p.187-203 (2002)
Astronomy and Astrophysics
Astrophysics
23
Open Clusters And Associations: Ic 4651, Stars: Hr Diagram, Stars: Evolution, Stars: Kinematics, Stars: Fundamental Parameters
Scientific paper
We present multiple-epoch radial-velocity observations for 104 stars in a 10arcmin x 10arcmin field of the intermediate-age open cluster IC 4651 to V ~ 14.5. Only 13 stars (13%) of the full sample are field stars. From the 44 single member stars we find a mean radial velocity of -30.76+/-0.20 km s-1, and the 12 single red-giant members yield a true radial-velocity dispersion of 0.74 km s-1. Of the 19 giant members, 7 (37%) are spectroscopic binaries with periods up to 5000 days, while 35 (52%) of the 67 main-sequence and turnoff members are binaries with periods less than ~ 1000 days. Combined with our deep, accurate CCD Strömgren photometry in a ~ 21arcminx21 arcmin field of IC 4651 \citep{mei00}, these data substantially improve the definition of the cluster locus in the colour-magnitude diagram and the spatial structure of the cluster, although the photometry shows that IC 4651 contains at least twice as many stars on the upper main sequence as was believed when the radial-velocity survey was initiated. The single cluster members define a very tight sequence in the CMD, and two sets of isochrones from stellar models with convective overshooting (d/H_p = 0.2) have been fit to it. Our best estimate for the age of IC 4651 is 1.7 +/- 0.15 Gyr, assuming [Fe/H] = 0.12 (Hyades) and E(b-y) = 0.071. Including the ~ 650 stars newly discovered from the photometry, we estimate the present total mass of IC 4651 to be ~ 630 Msun, excluding any undetected stellar remnants. The corresponding tidal cutoff radius is ~ 22arcmin . IC 4651 shows evidence of moderate mass segregation: Most of the turn-off stars and nearly all the red giants are located at radii smaller than ~ 7arcmin , while the lower main-sequence stars are less centrally concentrated. The spatial distributions of cluster and field stars indicate that additional cluster stars are probably still to be found outside the fields studied so far. Comparison of the present mass function of IC 4651 with plausible initial mass functions indicates that the cluster initially contained at least ~ 8300 stars with a total mass of ~ 5300 Msun. Thus, of the original cluster stars only ~ 7%, containing ~ 12% of the initial mass, remain today. Of the initial cluster mass, ~ 35% has been lost due to evolution of the most massive stars into white dwarfs or other remnants while the remaining ~ 53%, comprising ~ 93% of the original low-mass stars, appear to have migrated out of the observed field or been lost from the cluster altogether. IC 4651 is currently 1 kpc closer to the Galactic center than its ``sister'' cluster NGC 3680 \citep{nordstrom97}, but their Galactic orbital parameters indicate that the mean orbital radius of IC 4651 is in fact larger by 0.7 kpc, providing a plausible reason why it is much less advanced in its dynamical evolution than the coeval cluster NGC 3680. Based on observations obtained with the Danish 1.5-m telescope at the European Southern Observatory, La Silla, Chile. Tables 1 and 2 are also, and Table A1 only, available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/386/187
Andersen Jeppe J.
Meibom Soeren
Nordstrom Birgita
No associations
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