What I did: I am analysing some simulation snapshots of the Milky Way and it is modelled as a DM halo – bulge – disc system. I produced some mean line of sight velocity (LOSV) and dispersion of mean LOSV plots that I am attaching here. To produce these plots I simply extracted the vx,vy,vz components of the velocities of the stars and i picked z-axis as the line of sight. I overlaid a grid on the galaxy snapshot and at different inclinations(theta=0,45,90 degrees)of the galaxy I plotted the mean vz in the grid cells (vz is the z-component of the velocities). For dispersion, I just plotted the std deviation of the vz in the grid cells.
My question: I want to now understand and interpret my plots. What can I deduce from the plots for the different angles of inclinations? what can we deduce about the orbits the stars have at the bulge and disc? I mainly want to understand why the line of sight velocity distribution looks the way it does on my plots form a physics point of view..that is, due to gravity or mass distribution perhaps...please refer to equations if you want. Any help is much appreciated, thanks so much!