Na-O Anticorrelation and HB. VII. The chemical composition of first and second-generation stars in 15 globular clusters from GIRAFFE spectra

Details Na-O Anticorrelation and HB. VII. The chemical composition of first and second-generation stars in 15 globular clusters from GIRAFFE spectra Na-O Anticorrelation and HB. VII. The chemical composition of first and second-generation stars in 15 globular clusters from GIRAFFE spectra

2009-09-16

arxiv.org/abs/0909.2938v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

25 pages, 20 figures,figs.3,5,15 degraded. Accepted for publication on Astronomy and Astrophysics

Scientific paper

We present abundances of Fe, Na, and O for 1409 red giant stars in 15 galactic globular clusters, derived from the homogeneous analysis of high resolution FLAMES/GIRAFFE spectra. Combining the present data with previous results, we obtained a total sample of 1958 stars in 19 clusters, the largest and most homogeneous database of this kind to date. Our GCs have [Fe/H] from -2.4 to -0.4, with a wide variety of global parameters (morphology of the horizontal branch, mass, concentration, etc). For all clusters we find the Na-O anticorrelation, the classical signature of proton-capture reactions in H-burning at high temperature in a previous generation of more massive stars, now extinct. Using quantitative criteria (from the morphology and extension of the Na-O anticorrelation), we can define 3 components of the stellar population in GCs: a primordial component (P) of first-generation stars, and 2 components of second-generation stars (intermediate I and extreme E populations from their different chemical composition). The P component is present in all GCs, and its fraction is almost constant at about one third. The I component represents the bulk of the cluster population. The E component is not present in all GCs, and it is more conspicuous in some (but not in all) of the most massive ones. We discuss the fractions and spatial distributions of these components in our sample and in two additional clusters (M3 and M13) from the literature. We also find that the slope of the anti-correlation (defined by the minimum O and maximum Na abundances) changes from cluster-to-cluster, a change that is represented well by a bilinear relation on cluster metallicity and luminosity. This second dependence suggests a correlation between average mass of polluters and cluster mass.

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