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Many questions remain regarding the properties of disks around massiveprototstars. Here we present the observations of a high mass protostellarobject including an elongated dust continuum structure perpendicular to theoutflow. Submillimeter Array 230 GHz line and continuum observations of thehigh mass protostellar object IRAS 18151-1208 along with single dish IRAM 30mobservations afford us high spatial resolution (0.8") as well as recovery ofthe extended emission that gets filtered out by the interferometer. Theobservations of 12CO confirm the outflow direction to be in thesoutheast-northwest direction, and the 1.3 mm continuum exhibits an elongationin the direction perpendicular to the outflow. We model the physical parametersof the elongated structure by simultaneously fitting the observed spectralenergy distribution (SED) and the brightness profile along the major axis usingthe 3D Radiative Transfer code MC3D. Assuming a density profile similar to thatof a low mass disk, we can also reproduce the observations of this high massprotostellar object. This is achieved by using the same density distributionand flaring parameters as were used in the low mass case, and scaling up thesize parameters that successfully modeled the circumstellar disk of several TTauri stars. We also calculate that a region within the inner 30 AU of such ahigh mass disk is stable under the Toomre criterion. While we do not rule outother scenarios, we show here that the observations in the high mass regime areconsistent with a scaled up version of a low mass disk. Implications on highmass star formation are discussed.

A High Mass Dusty Disk Candidate: The Case of IRAS 18151-1208