Example of fits of the observed (reddened) data to the (reddened) semi-empirical spectra for HIP 103598 (left) and HIP 50564 (right). The bolometric flux is calculated by integrating the un-reddened spectrum. The bottom panels illustrate the distribution of versus F_bol for the 400 simulations for the two stars with the 16th, 50th (median), and 84th percentiles indicated by the dashed lines. The continuous line is the derived F_bol without considering the simulations.