========================================================================== J/A+A/501/553 Equivalent widths of IC 2602 & IC 2391 stars (D'Orazi+, 2009) The following files can be converted to FITS (extension .fit or fit.gz) stars.dat tableew.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/A+A/501/553 ==========================================================================
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Beginning of ReadMe : J/A+A/501/553 Equivalent widths of IC 2602 & IC 2391 stars (D'Orazi+, 2009) ================================================================================ Chemical composition of the young open clusters IC 2602 & IC 2391. D'Orazi V., Randich S. <Astron. Astrophys. 501, 553 (2009)> =2009A&A...501..553D ================================================================================ ADC_Keywords: Clusters, open ; Abundances Keywords: stars: abundances - open clusters and associations: individual: IC 2602, IC 2391 Abstract: Galactic open clusters have been long recognized as one of the best tools to investigate the chemical content of Galactic disk and its time evolution. In the last decade, many efforts have been directed to chemically characterize the old and intermediate age population; surprisingly, the chemical content of the younger and close counterpart remains largely undetermined. In this paper we present the abundance analysis of a sample of 15 G/K members of the young pre-main sequence clusters IC 2602 and IC 2391. Along with IC 4665, these are the first pre-main sequence clusters for which a detailed abundance determination has been carried out so far. Description: We analyzed high-resolution, high S/N spectra acquired with different instruments (UVES and CASPEC at ESO, and the echelle spectrograph at CTIO), using MOOG and equivalent width measurements. Along with metallicity ([Fe/H]), we measured NaI, SiI, CaI, TiI and TiII, and NiI abundances. Stars cooler than 5500 show lower CaI, TiI, and NaI than warmer stars. By determining TiII abundances, we show that, at least for Ti, this effect is due to NLTE and over-ionization.