Cosmological simulations of the same spiral galaxy: the impact of
  baryonic physics
  The interplay of star formation and supernova (SN) feedback in galaxy
formation is a key element for understanding galaxy evolution. Since these
processes occur at small scales, it is necessary to have sub-grid models that
recover their evolution and environmental effects at the scales reached by
cosmological simulations. We simulate the same spiral galaxy inhabiting a Milky
Way (MW) size halo in a cosmological environment changing the sub-grid models
for SN feedback and star formation. We test combinations of the Schmidt law and
a multi-freefall based star formation with delayed cooling feedback or
mechanical feedback. We reach a resolution of 35 pc in a zoom-in box of 36 Mpc.
For this, we use the code RAMSES with the implementation of gas turbulence in
time and trace the local hydrodynamical features of the star-forming gas.
Finally, we compare the galaxies at redshift 0 with global and interstellar
medium observations in the MW and local spiral galaxies. The simulations show
successful comparisons with observations. Nevertheless, diverse galactic
morphologies are obtained from different numerical implementations. We
highlight the importance of detailed modelling of the star formation and
feedback processes, especially when increasing the resolution of simulations.
Future improvements could alleviate the degeneracies exhibited in our simulated
galaxies under different sub-grid models.
