========================================================================== J/ApJ/647/1075 Age-metallicity relation of omega Cen (Stanford+, 2006) The following files can be converted to FITS (extension .fit .fgz or .fiZ) table2.dat table3.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/ApJ/647/1075 ==========================================================================
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Beginning of ReadMe : J/ApJ/647/1075 Age-metallicity relation of omega Cen (Stanford+, 2006) ================================================================================ The age and metallicity relation of omega Centauri. Stanford L.M., Da Costa G.S., Norris J.E., Cannon R.D. <Astrophys. J., 647, 1075-1092 (2006)> =2006ApJ...647.1075S ================================================================================ ADC_Keywords: Clusters, globular ; Photometry, UBV ; Radial velocities ; Abundances, [Fe/H] Keywords: globular clusters: general - globular clusters: individual (omega Centauri) Abstract: We present a metallicity distribution based on photometry and spectra for 442 Omega Centauri cluster members that lie at the main-sequence turnoff region of the color-magnitude diagram. This distribution is similar to that found for the red giant branch. The distribution shows a sharp rise to a mean of [Fe/H]=-1.7 with a long tail to higher metallicities. Ages have then been determined for the stars using theoretical isochrones enabling the construction of an age-metallicity diagram. Interpretation of this diagram is complicated by the correlation of the errors in the metallicities and ages. Nevertheless, after extensive Monte Carlo simulations, we conclude that our data show that the formation of the cluster took place over an extended period of time: the most metal-rich stars in our sample ([Fe/H] -0.6) are younger by 2-4Gyr than the most metal-poor population. Description: Photometry for the cluster was obtained with the 1m telescope + Tektronix CCD combination at Siding Spring Observatory, in the V and B bands.