Volume 399, Number 2, February IV 2003
|Page(s)||543 - 551|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||07 February 2003|
Observatorio Astronómico, Universidad Nacional de Córdoba, Laprida 854, 5000 Córdoba, Argentina e-mail: firstname.lastname@example.org;email@example.com
2 Instituto de Astronomía y Física del Espacio, CC 67, Suc. 28, 1428 Buenos Aires, Argentina e-mail: firstname.lastname@example.org
3 Institut d'Astronomie de l'Université de Lausanne, 1290 Chavannes-des-Bois, Switzerland e-mail: Jean-Claude.Mermilliod@obs.unige.ch
Corresponding author: J. J. Clariá, email@example.com
Accepted: 10 December 2002
We present new UBV photoelectric observations of 119 stars in the field of the southern open cluster IC 2488, supplemented by DDO and Washington photometry and Coravel radial velocities for a sample of red giant candidates. Nearly 50% of the stars sampled – including three red giants and one blue straggler – are found to be probable cluster members. Photometric membership probabilities of the red giant candidates show good agreement with those obtained from Coravel data. A mean radial velocity of (-2.63 ± 0.06) km s-1 is derived for the cluster giants. The reddening across the cluster is found to be uniform, the mean value being = 0.24 ± 0.04. IC 2488, located at a distance of (1250 ± 120) pc from the Sun and 96 pc below the Galactic plane, is most probably not related to the planetary nebula ESO 166-PN21. A metal abundance [Fe/H] = 0.10 ± 0.06 relative to the Sun is determined from DDO data of the red giant members, in good agreement with the [Fe/H] values derived from five independent Washington abundance indices. An age of 180 Myr is determined from the fitting of isochrones computed with convective overshooting for 0.019. The isochrone for log t = 8.25 reproduces remarkably well not only the morphology of the upper main sequence but also the observed red giant pattern.
Key words: methods: observational / open clusters and associations: individual: IC2488 / star: abundances / stars: Hertzsprung-Russell (HR) diagram and C-M diagrams
Based on observations made at Las Campanas Observatory (Chile) and Cerro Tololo Inter-American Observatory (Chile), National Optical Astronomy Observatories, operated by the Association of the Universities for Research in Astronomy, Inc., under contract with the National Science Foundation and on observations collected with the Danish 1.54-m telescope at the European Southern Observatory, La Silla (Chile).
© ESO, 2003
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