| dc.description.abstract | We use N-body simulations to study the evolution of the Fornax dwarf spheroidal galaxy. Specifically, we study the effects of tides on the internal structure of Fornax, and its globular clusters. We adopt a cuspy NFW and a cored Burkert halo, as well as a contracted Sersic bulge, extending out to about 2.65 kpc, and an extended Plummer bulge, extending out to about 6 kpc - while retaining 95$\%$ of its mass within 3 kpc. We find that the internal structure of Fornax is largely unaffected by tidal effects, with a extended bulge causing a maximum of 7% of its original stellar mass to become unbound, while a contracted bulge results in a maximum of 2$\%$ of its original stellar mass to become unbound. Our final to initial stellar mass ratio within 1.6 kpc was between 0.92 and 0.98 and between 0.82 and 0.89 for DM. Outside of the internal areas, there is significant DM stripping. For globular clusters, we find that both a cuspy and cored halo is consistent with observations, but a cored halo allows for more formation scenarios. A possible, and perhaps likely, reason for why GC 1,2,5, and perhaps GC4 as well, have not yet sunk is that their current distance from the center of Fornax is large enough that they have decayed very little over the last several Gyr while also being small enough to not have been stripped from Fornax. This solution could also explain why GC3 has not yet sunk, but would require an even larger initial radius. Alternatively it is possible GC3 has been accreted into Fornax. Furthermore, we show that the eccentricity of the GC orbit as well as the presence of the MW can all affect the decay time of a GC. Lastly, we were unable to replicate a previously reported effect where globular clusters placed inside the core radius of an halo with a large core increased its distance from the center of Fornax. | en |
