Volume 453, Number 1, July I 2006
|Page(s)||101 - 119|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||09 June 2006|
On the difference between nuclear and contraction ages
Cerro Tololo Interamerican Observatory, Casilla 603 La Serena, Chile
2 Observatório do Valongo/UFRJ, Ladeira do Pedro Antônio 43, 20080-090 Rio de Janeiro, Brazil
3 Department of Astronomy and Space Physics, Uppsala Astronomical Observatory, Box 515, 751 20 Uppsala, Sweden e-mail: firstname.lastname@example.org
4 Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisbon, Portugal
5 European Southern Observatory, Karl-Schwarzschild 2, 85748 Garching, Germany
Accepted: 20 February 2006
Context.Ages derived from low mass stars still contracting onto the main sequence often differ from ages derived from the high mass ones that have already evolved away from it.
Aims.We investigate the general claim of disagreement between these two independent age determinations by presenting photometry for the young galactic open clusters NGC 2232, NGC 2516, NGC 2547 and NGC 4755, spanning the age range ~10–150 Myr
Methods.We derived reddenings, distances, and nuclear ages by fitting ZAMS and isochrones to color–magnitudes and color–color diagrams. To derive contraction ages, we used four different pre-main sequence models, with an empirically calibrated color-temperature relation to match the Pleiades cluster sequence.
Results.When exclusively using the V vs. color–magnitude diagram and empirically calibrated isochrones, there is consistency between nuclear and contraction ages for the studied clusters. Although the contraction ages seem systematically underestimated, in none of the cases do they deviate by more than one standard deviation from the nuclear ages.
Key words: Galaxy: open clusters and associations: general / galaxies: star clusters / stars: formation / techniques: photometric / Hertzsprung-Russell (HR) and C-M diagrams
© ESO, 2006
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