Hodge 301 - A Neglected Cluster Next to R 136 in 30 Doradus

Details Hodge 301 - A Neglected Cluster Next to R 136 in 30 Doradus Hodge 301 - A Neglected Cluster Next to R 136 in 30 Doradus

Aug 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996agab...12..215g&link_type=abstract

Astronomische Gesellschaft Abstract Series, 12, 215

Astronomy and Astrophysics

Astronomy

1

Large Magellanic Cloud, Star Clusters, Star Formation, 30 Doradus, Hodge 301

Scientific paper

At a distance of 50 kpc, 30 Doradus provides a unique opportunity to study the detailed star formation history in a giant starburst region. 30 Dor contains two prominent clusters: the compact, young R 136 cluster at its core, and the poorer, older cluster Hodge 301 approximately 3' to the northwest. Hodge 301 is very close to or contains R 132. While the R 136 cluster has been the focus of numerous studies, Hodge 301 has been neglected. Thus, our understanding of the starburst in 30 Dor is severely limited. We have obtained proprietary HST WFPC2 images of Hodge 301 in the F336W, F555W, F814W, and F656N filters, roughly corresponding to the U, V, I, and H alpha bands. The photometry reaches V ~ 24 mag and spans at least 12 mag. The colour-magnitude diagrams show an extended main sequence with a small number of supergiants. The H alpha and continuum images were used to identify stars with Balmer emission. We find a large fraction of Be star candidates. Isochrone fits yield a preliminary age of 20 Myr for Hodge 301, significantly older than the age of 3 to 4 Myr that was found for the R 136 cluster. Using star counts for Hodge 301 to extrapolate an IMF with Salpeter slope to higher masses, we find that the 5 most massive stars may have exploded as supernovae. This is in good agreement with the extremely violent motions in the interstellar medium surrounding Hodge 301 (see poster by Chu et al., this conference).

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