DETERMINATION OF BOLOMETRIC FLUXES FOR F-SUBDWARF, G-SUBDWARF AND K-SUBDWARF

Bolometric fluxes for 118 dwarfs and subdwarfs with 4000K < T-eff < 70 00K and +0.5 < [Fe/H] < -3.5 are derived by integrating UBVRIJHK photo metry. For these stars (typical of the galactic and globular cluster m ain sequences) at least 80% of the energy emitted is measured by those bands. A grid of theoretical model line-blanketed flux distributions (Kurucz 1991, 1993) was used in order to estimate the flux outside the se photometric bands. The method, based on the use of synthetic magnit udes, provides bolometric fluxes with an estimated uncertainty in the order of 2%. The results obtained have been used to calibrate the bolo metric flux versus K, (V-K) and [Fe/H], in order to derive an expressi on of general application. A by-product of this study is the bolometri c correction for main sequence stars, which is tabulated for different metallicities. Comparisons of these results with those obtained by ot her authors are presented and discussed.