Evolution of Stars and Stellar Systems. I. The Initial Size Distribution of Clusters

Details Evolution of Stars and Stellar Systems. I. The Initial Size Distribution of Clusters Evolution of Stars and Stellar Systems. I. The Initial Size Distribution of Clusters

Jul 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004hst..prop10281c&link_type=abstract

HST Proposal ID #10281

Physics

Hst Proposal Id #10281 Stellar Populations

Scientific paper

There are three fundamental properties which define a star cluster - age, mass, and size. While much attention has been focused on the first two parameters, significantly less is known concerning not only actual cluster sizes and structures, but the initial distribution of stellar clustering which occurs in different environments. For example, NGC 1569 has formed three compact, massive young clusters in the last 10 Myr, while IZw18 appears to have only formed more diffuse, "scaled up" OB associations {SOBAs}. The HST archive now contains sufficient observations of nearby star-forming galaxies to allow a quantitative measure of the initial clustering of star formation. We propose to measure the distribution of the physical scales of cluster formation, from the most compact clusters to diffuse SOBAs in 30 nearby galaxies. Local variations in the star formation rate may manifest themselves in the fraction of star formation occuring in compact clusters vs. that occurring in more diffuse OB associations. Because our galaxy sample covers a large range in environment, mass, and star formation rate density, we will take the next step, and use our size distributions to place constraints on the processes responsible for setting the scales of star formation in the local universe. A complementary proposal aims to study the isolated red supergiant population in nearby star-forming galaxies {PI: Dr. C. Leitherer}.

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