A model to determine the slope of the initial mass function in a cluster of young stars.

A simple theoretical model is presented which aimed at determining the slope of the IMF in a cluster of young stars embedded in a cloud of hydrogen. In the model the stellar and gaseous fluxes for this cluster are added and calculations are made for the ratio of line to continuum fluxes and continuum colors as a function of the slope of a power-law IMF and the age of the cluster. Predictions at far ultraviolet wavelengths are included. It is found that a determination of the slope of the IMF is possible if the cluster is older than about 2 x 10 to the 7th years or if the IMF is much steeper than in the solar neighborhood.