Resolution of the Upper IMF in the Magellanic CLOUDS:CYCLE4

Details Resolution of the Upper IMF in the Magellanic CLOUDS:CYCLE4 Resolution of the Upper IMF in the Magellanic CLOUDS:CYCLE4

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5678w&link_type=abstract

HST Proposal ID #5678

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Hst Proposal Id #5678 Hot Stars Young Clusters

Scientific paper

Determination of the highly significant upper end of the initial mass function in extragalactic systems is subject to serious systematic error due to the combination of limited spatial resolution and the tendency of the most massive stars to occur in compact groups. These effects cause the luminosities to be overestimated and the numbers underestimated. The Magellanic Clouds provide the most favorable case, but even there compact systems remain a challenge. GTO observations of the 30 Doradus central cluster have demonstrated the substantial contribution which HST can make to the problem. This program will obtain UBV images with WF/PC of 5 important fields in the Magellanic Clouds other than the 30 Doradus cluster, in which recent ground-based and HST spectroscopy of extremely massive stars has been performed. It is absolutely vital to ascertain the multiplicity status of these images, even at the 0.1 arc sec level, for useful interpretation of the spectroscopic data. The use of 3 colors will enable reddening estimates to be made, and corrected color-magnitude diagrams and IMFs to be constructed, the latter with consultation of the spectroscopic results. The analysis of these images will provide a substantial advance over current knowledge of the upper IMF, and they represent an optimum use of HST in its present optical state, which would not be significantly enhanced by the refurbishment.

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