Population of VMS in our Milky Way model. Top panel: number of massive stars (8–120 M_⊙) and VMS (120–300 M_⊙) in rings with a width of 0.1 kpc as a function of galactocentric distance. We used a Salpeter IMF with α = 2.35 and the SFR from the middle panel of Fig. 4 in Kubryk et al. (2015). Bottom panel: number of VMS in a disk around the Sun as a function of the maximum distance to the Sun, following the same method.