Limits on the significant mass-loss scenario based on the globular
  clusters of the Fornax dwarf spheroidal galaxy
  Many of the scenarios proposed to explain the origin of chemically peculiar
stars in globular clusters (GCs) require significant mass-loss ($\ge95\%$) to
explain the observed fraction of such stars. In the GCs of the Fornax dwarf
galaxy significant mass-loss could be a problem. Larsen et al. (2012) showed
that there is a large ratio of GCs to metal-poor field stars in Fornax and
about $20-25\%$ of all the stars with ${\rm [Fe/H]}<-2$ belong to the four
metal-poor GCs. This imposes an upper limit of $\sim80\%$ mass-loss that could
have happened in Fornax GCs. In this paper, we propose a solution to this
problem by suggesting that stars can leave the Fornax galaxy. We use a series
of $N$-body simulations, to determine the limit of mass-loss from Fornax as a
function of the initial orbital radii of GCs and the speed with which stars
leave Fornax GCs. We consider a set of cored and cuspy density profiles for
Fornax. Our results show that with a cuspy model for Fornax, the fraction of
stars which leave the galaxy, can be as high as $\sim90\%$, when the initial
orbital radii of GCs are $R=2-3\,\rm{kpc}$ and the initial speed of stars is
$v>20\,\rm{km\,s^{-1}}$. We show that such large velocities can be achieved by
gas expulsion induced mass-loss but not stellar evolution induced mass-loss.
Our results imply that one cannot interpret the metallicity distribution of
Fornax field stars as evidence against significant mass-loss in Fornax GCs, if
mass-loss is due to gas expulsion.
