Aug 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jena.confe..77h&link_type=abstract
"JENAM-2007, "Our non-stable Universe", held 20-25 August 2007 in Yerevan, Armenia. Abstract book, p. 77-77"
Other
Scientific paper
The Initial Mass Function (IMF) of the bright end of the mass scale is a crucial parameter for determining the upper limit of stellar mass and its connection to the environment such as metallicity. The high mass stars, typically O- and B-type stars, are the luminous tracers of the young populations in galaxies. Although intrinsically few, their large fluxes make them easy to observe, both in our galaxy and other nearby galaxies. To determine the IMF it is necessary to know the mass of the stars (inferred from their position in colour-magnitude diagram) as well as their absolute magnitude, i.e. their exact distance and absorption. An efficient way of overcoming the problem of constraining the extinction as well as getting an exact estimation of the stars' distance is to consider the stars in stellar clusters. In order to address this science case using VO tools, we will suggest ways of selecting samples, construct the broad band spectral energy distribution of the selected stars and compare them to theoretical models available via the VO resources.
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