CONICET | Buscador de Institutos y Recursos Humanos

We analyze age and metallicity estimates for an unprecedented database of some 5.5 millionstars distributed throughout the Large Magellanic Cloud (LMC) main body, obtained from CCD Washington $CT_1$ photometry, reported on in Piatti et al. 2012. We produce a comprehensive field star Age-Metallicity Relationship(AMR) from the earliest epoch until $sim$ 1 Gyr ago.This AMR reveals that the LMC has not evolved chemically as either a closed-box or bursting system, exclusively, but as a combination of both scenarios that have varied in relative strength over the lifetime of the galaxy, although the bursting model falls closer to the data in general.Furthermore, while old and metal-poor field stars have been preferentially formed in the outer disk, younger and more metal-rich stars have mostly been formed in the inner disk, confirming an outside-in formation. We provide evidence for the formation of stars between 5 and 12 Gyr, during the cluster age gap, although chemical enrichment during thisperiod was minimal. We find no significant metallicity gradient in the LMC. We also find that the range in the metallicity of an LMC field has varied during the lifetime of the LMC. In particular, we find only a small range of the metal abundance in the outer disk fields, whereas an average range of $Delta$[Fe/H] = +0.3 $pm$ 0.1 dexappears in the inner disk fields.Finally, the cluster and field AMRs show a satisfactory match only for the last 3 Gyr, while for the oldest ages ($>$ 11 Gyr) the cluster AMR is a remarkable lower envelope to the field AMR. Such a difference may be due to the very rapid early chemical evolution and lack of observed field stars in this regime, whereas the globular clusters are easily studied.This large difference is not easy to explain as coming fromstripped ancient Small Magellanic Cloud (SMC) clusters, although the field SMC AMR is on average $sim$ 0.4 dex more metal-poor at all ages than that of the LMC but otherwise very similar.

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