Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998larm.confe.159d&link_type=abstract
"IX Latin American Regional IAU Meeting, "Focal Points in Latin American Astronomy", held in Tonantzintla, Mexico, Nov 9-13, 199
Astronomy and Astrophysics
Astronomy
Scientific paper
Washington C, T1 CMDs are used to study LMC star clusters. Age estimates are based in the difference dT1 between the giant branch clump and the turnoff, calibrated using standard clusters, while metallicities are derived from the location of the giant and subgiant branches as compared to mean loci of fiducial star clusters. 25 candidates to old clusters, which were uncovered by menas of UBV integrated photometry and CaII triplet spectroscopy, where reanalized by means of this technique and turned out to be intermediate age (1-3 Gyr) clusters. We confirm previous indications that there was no cluster formation between 3 and 8 Gyr ago and there was a pronounced epoch of cluster formation beginning 3 Gyr ago that peaked 1.5 Gyr ago. We also analised clusters and surrounding fields in the outer LMC disk (well beyond 4 degrees). We found that in most cases the stellar population of each cluster is quite similar to that of the field where it is embedded, thus sharing its mean age and metallicity properties. On the other hand significant metallicity differences are found among clusters of similar age, indicating that the chemical enrichment was not homogeneous in the LMC. three regions deserve special attention: that of the so far unique cluster ESO121-SC03, the field surrounding the far eastern intermediate age cluster OHSC 37 and in the northern part of the LMC disk the field around SL388 and SL509. We detect LMC field stars out to 11 kpc, but not to 13 kpc, despite the presence of clusters at this distance. The mean metallicity derived for the intermediate age outer disk clusters is <[Fe/H]>=-0.7 and for the surrounding fields <[Fe/H]>=-0.6. These values are significantly lower than that found by Olszewsky et al. (1991, AJ 101, 515) for a sample of clusters of similar ages, but are in good agreement with several recent studies. A few clusters stand out in the age-metallicity relationship, in the sense that they are intermediate age clusters at relatively low metallicity ([Fe/H]~-1.
Bica Eduardo
Claria Juan J.
Dottori Horacio
Geisler Doug
Piatti Alberto
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