Fundamental parameters of the LMC clusters NGC 1836, NGC 1860, NGC 1865, SL 444, LW 224 and SL 548

• Autor(a) principal: Piatti, Andres E.
• Data de Publicação: 2003
• Outros Autores: Bica, Eduardo Luiz Damiani, Geisler, Doug, Claria Olmedo, Juan Jose
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Institucional da UFRGS
• Texto Completo: http://hdl.handle.net/10183/89983
• topic: Grande Nuvem de Magalhães; Composicao estelar; Evolucao estelar; Fotometria estelar; Techniques: photometric; Galaxies: individual: large magellanic cloud; Magellanic clouds; Galaxies: star clusters

Complementing our recent Washington photometric studies on intermediate age and young Large Magellanic Cloud (LMC) clusters, we now turn our attention to six previously unstudied star clusters in the transition range 200–700 Myr.We study NGC 1836, 1860 and 1865, which are projected on theLMCbar;SL444, also located in the central disc but outside the bar; andLW 224 and SL 548, both located in the outer disc.We derive ages and metallicities from extracted T1 versus C–T1 colour–magnitude diagrams (CMDs), using theoretical isochrones recently computed for the Washington photometric system. For the metallicity determinations, these CMDs are particularly sensitive. We also estimate ages and metallicities of the surrounding fields of NGC 1860 and 1865 by employing the δT 1 index defined in Geisler et al. (1997, AJ, 114, 1920) and theoretical isochrones. By adding the present cluster sample to those of our previous studies, we nowgather 37LMCclusters with homogeneous parameter determinations, which are employed to probe the chemical enrichment of the LMC and its spatial distribution. On average, inner disc clusters turned out to be not only younger than the outer ones, but also more metal-rich; some have solar metal content. Furthermore, inner clusters located to the west of the LMC centre are younger and more metal-rich than their eastern counterparts. We propose that a bursting formation mechanism, with an important formation event centred at ~ 2.0 Gyr, provides a better description of the cluster age–metallicity relation than a closed-box chemical evolution model. In the outer disc, the field star formation seems to have lasted until 2 Gyr ago while it continued in the inner disc for almost 1 Gyr longer.