Dynamical estimate of post main sequence stellar masses in 47 Tucanae
  We use the effects of mass segregation on the radial distribution of
different stellar populations in the core of 47 Tucanae to find estimates for
the masses of stars at different post main sequence evolutionary stages. We
take samples of main sequence (MS) stars from the core of 47 Tucanae, at
different magnitudes (i.e. different masses), and use the effects of this
dynamical process to develop a relation between the radial distance (RD) at
which the cumulative distribution reaches the 20th and 50th percentile, and
stellar mass. From these relations we estimate the masses of different post MS
populations. We find that mass remains constant for stars going through the
evolutionary stages between the upper MS up to the horizontal branch (HB). By
comparing RDs of the HB stars with stars of lower masses, we can exclude a mass
loss greater than 0.09M during the red giant branch (RGB) stage at nearly the
3{\sigma} level. The slightly higher mass estimates for the asymptotic giant
branch (AGB) are consistent with the AGB having evolved from somewhat more
massive stars. The AGB also exhibits evidence of contamination by more massive
stars, possibly blue stragglers (BSS), going through the RGB phase. We do not
include the BSS in this paper due to the complexity of these objects, instead,
the complete analysis of this population is left for a companion paper. The
process to estimate the masses described in this paper are exclusive to the
core of 47 Tuc.
