Resumo:
With the publication of the Gaia catalogue, and with the existence of automated isochrone
fitting methods, the study of open clusters has undergone major advances in recent years.
Its fundamental parameters have been, consequently, getting estimated in a larger scale
and with better precision. However, important parameters such as the total masses of
these objects, the details about populations of individual stars and of binary stars, and
the existence of mass segregation are not adequately studied. Within this context, in this
work we introduce a new method to determinate individual masses, including of binary
stars. This method allows us to study the total mass of open clusters, as well as to study
details of binary populations through their mass functions. To validate the method and its
efficiency, we used synthetic clusters with predetermined parameters. With the validated
method, we applied the procedure to clusters from a recent catalogue of fundamental
parameters by our group, obtained from GAIA Early Data Release 3 (EDR 3). The
main results include the obtaining of the detailed mass function for the populations of
individual, primary, and secondary stars, in addition to the total masses for 895 clusters.
We also show the relation between the total masses and other fundamental parameters,
discussing its dynamic implications.