Heavy elements and chemical enrichment in globular clusters^*

¹ Observatoire de Paris – GEPI, 61 avenue de l'Observatoire, 75014 Paris, France e-mail: Gael.James@obspm.fr
² INAF – Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, 34131 Trieste, Italy
³ INAF – Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy

Received: 22 June 2004
Accepted: 5 August 2004

Abstract

High resolution () and high spectra have been acquired with UVES on the VLT-Kueyen (Paranal Observatory, ESO Chile) for several main sequence turnoff stars ( mag) and subgiants at the base of the Red Giant Branch ( mag) in three globular clusters (NGC 6397, NGC 6752 and 47 Tuc/NGC 104) at different metallicities (respectively ). Spectra for a sample of 25 field halo subdwarves have also been taken with equal resolution, but higher . These data have been used to determine the abundances of several neutron-capture elements in these three clusters: strontium, yttrium, barium and europium. This is the first abundance determination of these heavy elements for such unevolved stars in these three globular clusters. These values, together with the [Ba/Eu] and [Sr/Ba] abundance ratios, have been used to test the self-enrichment scenario. A comparison is done with field halo stars and other well known Galactic globular clusters in which heavy elements have already been measured in the past, at least in bright giants (–12 mag). Our results show clearly that globular clusters have been uniformly enriched by r- and s-process syntheses, and that most of them seem to follow exactly the same abundance patterns as field halo stars, which discards the “classical” self-enrichment scenario for the origin of metallicities and heavy elements in globular clusters.