Stellar Phoenix Jpeg Repair Activation Code

Although the masses of the observed stars suggest several bursts of star formation from 30 to 1 Myr ago, the spectra cannot be reproduced by evolutionary models for low- and intermediate-mass stars and a compromise between evolutionary modeling and observed spectra must be adopted. We describe this compromise as a modified version of the Bonnsai code based on the models of Ekström et al. (2008, in prep.). We fit the observed spectrum to the evolutionary models within the synthetic grid of Boettiger et al. (2013, in prep.) to infer the stellar parameters. To disentangle the effects of binarity from those of the derived stellar parameters, we then add the parameters of a putative binary to the model and redo the fit. This iterative process allows us to estimate the effect of a putative companion on the derived parameters. We discuss a possible binarity rate of 0.4% for the observed sample of apparently single VFTS stars.

SSP: Simple Stellar Population: A tool for computing the properties of a stellar population based on its (single-age) star formation history and star formation rate. The input star formation rate is assumed to be constant over a given time period, and to be zero outside this period. When the star formation in the population ceases, the evolution of each is calculated with the synthesis code, and the properties of the population at the present time are computed. The properties of the population include luminosity, mass, and metallicity distributions, and stellar populations can be compared with observations, or the light or colours of the population can be used as a star formation history. The package contains routines for the transformation of the star formation rate to the IMF and the synthesis code, both based on the method of Bruzual & Charlot (1993). The user interface of the code is based on the Starburst99 (Leitherer et al. 1999, Vazquez et al. 2005) package.

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