  In a recent paper, Smith and Tombleson (2015) state that the Luminous Blue
Variables (LBVs) in the Milky Way and the Magellanic Clouds are isolated; that
they are not spatially associated with young O-type stars. They propose a novel
explanation that would overturn the standard view of LBVs. In this paper we
test their hypothesis for the LBVs in M31 and M33 as well as the LMC and SMC.
In M31 and M33, the LBVs are associated with luminous young stars and
supergiants appropriate to their luminosities and positions on the HR Diagram.
Moreover, in the Smith and Tombleson scenario most of the LBVs should be
runaway stars, but the stars' velocities are consistent with their positions in
the respective galaxies. In the Magellanic Clouds, those authors' sample was a
mixed population. We reassess their analysis, removing seven stars that have no
clear relation to LBVs. When we separate the more massive classical and the
less luminous LBVs, the classical LBVs have a distribution similar to the late
O-type stars, while the less luminous LBVs have a distribution like the red
supergiants. None of the confirmed LBVs have high velocities or are candidate
runaway stars. These results support the accepted description of LBVs as
evolved massive stars that have shed a lot of mass, and are now close to their
Eddington limit.
