  Mass loss bridges the gap between massive stars and supernovae (SNe) in two
major ways: (i) theoretically it is the amount of mass lost that determines the
mass of the star prior to explosion, and (ii) observations of the circumstellar
material around SNe may teach us the type of progenitor that made the SN. Here,
I present the latest models and observations of mass loss from massive stars,
both for canonical massive O stars, as well as very massive stars (VMS) that
show Wolf-Rayet type features.
