Cluster formation in the LMC

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dc.creatorVallenari, A.
dc.creatorMoretti, A.
dc.creatorHeld, E. V.
dc.creatorRizzi, L.
dc.creatorBettoni, D.
dc.date2002-10-02
dc.date.accessioned2026-07-07T02:05:33Z
dc.date.available2026-07-07T02:05:33Z
dc.descriptionIn this work we present preliminary results concerning the properties of about 50 clusters and associations located in a densely populated region at the Southern edge of the supershell LMC~4. The ages of the clusters and associations are derived. The cluster formation rate peaks at about 10-20 Myr ago corresponding to the age of the formation of LMC~4. Objects younger than 10 Myr are located close to CO clouds, indicating a possible trigger of the recent star formation by the interaction of the supershell with the interstellar medium. Isophotal analysis has been done for 50% of the clusters. A large number of objects present isophotal distortions commonly interpreted as sign of interaction. Cluster multiplets are coeval within 20 Myr, suggesting a common origin. This indicates that clusters possibly form in large groups. Our findings are in agreement with the unified view of multi-scale star formation, where a size-duration correlation is expected.
dc.description2 pages, Proceedings of the Conference : New Horizons in Globular Clusters
dc.identifierhttps://arxiv.org/abs/astro-ph/0210060
dc.identifierhttp://arxiv.org/abs/astro-ph/0210060
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/5135
dc.subjectAstrophysics
dc.titleCluster formation in the LMC
dc.typetext

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