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As the recent publication by Breen et al (2013) found Class II methanolmasers are exclusively associated with high mass star forming regions. Based onthe positions of the Class I and II methanol and H$_{2}$O masers, UC H IIregions and 4.5 $\mu$m infrared sources, and the center velocities($v_{\text{LSR}}$) of the Class I methanol and H$_{2}$O masers, compared to the$v_{\text{LSR}}$ of the Class II methanol masers, we propose three disk-outflowmodels that may be traced by methanol masers. In all three models, we havelocated the Class II methanol maser near the protostar, and the Class Imethanol maser in the outflow, as is known from observations during the lasttwenty years. In our first model, the H$_{2}$O masers trace the linear extentof the outflow. In our second model, the H$_{2}$O masers are located in acircumstellar disk. In our third model, the H$_{2}$O masers are located in oneor more outflows near the terminating shock where the outflow impacts theambient interstellar medium. Together, these models reiterate the utility ofcoordinated high angular resolution observations of high mass star formingregions in maser lines and associated star formation tracers.

Disk-outflow models as applied to high mass star forming regions through methanol and water maser observations