  Methanol masers are often found in linear distributions, and it has been
hypothesized that these masers are tracing circumstellar accretion disks around
young massive stars. However, recent observations in H2 emission have shown
what appear to be outflows at similar angles to the maser distribution angles,
not perpendicular as expected in the maser-disk scenario. The main motivation
behind the observations presented here is to determine from the presence and
morphology of an independent outflow tracer, namely SiO, if there are indeed
outflows present in these regions and if they are consistent or inconsistent
with the maser-disk hypothesis. For ten sources with H2 emission we obtained
JCMT single dish SiO (6-5) observations to search for the presence of this
outflow indicator. We followed up those observations with ATCA interferometric
mapping of the SiO emission in the (2-1) line in six sources. The JCMT
observations yielded a detection in the SiO (6-5) line in nine of the ten
sources. All of the sources with bright SiO lines display broad line wings
indicative of outflow. A subset of the sources observed with the JCMT have
methanol maser velocities significantly offset from their parent cloud
velocities, supporting the idea that the masers in these sources are likely not
associated with circumstellar disks. The ATCA maps of the SiO emission show
five of the six sources do indeed have SiO outflows. The spatial orientations
of the outflows are not consistent with the methanol masers delineating disk
orientations. Overall, the observations presented here seem to provide further
evidence against the hypothesis that linearly distributed methanol masers
generally trace the orientations of circumstellar disks around massive young
stars.
