BOLOMETRIC STELLAR DISTRIBUTION MODEL IN THE GALAXY AND ITS APPLICATION TO BAADES WINDOW

We develop a very simple model for the distribution of the stellar com ponent in our Galaxy. This model is completely arbitrary and is utilis ed only as a description of the stellar distribution in the Galaxy. Th e model consists of a flat (disc) component with a radial Gaussian den sity profile and an exponential density decay in the direction perpend icular to the galactic plane; moreover, it also presents a spheroidal (bulge) component with a radial Gaussian density profile. At this stag e, the model is used for predicting the would-be-observed bolometric l uminosity functions (LF) of bright (M-bol less than or equal to 0.0) s tars. The main purpose of this paper is to check, using our simplified galactic model, whether the stellar population in Baade's Window (BW) , may consist of a combination of bulge and disc extending to the gala ctic centre populations. We show that this possibility is consistent w ith the data, and that the observed LF may be separated into two Gauss ian components which may consistently correspond to the bulge and disc contributions.