Observations of Orion Source I Disk and Outflow Interface
  We imaged the continuum and molecular line emission from Orion Source I
(SrcI) with up to 30 mas (12 AU) resolution at 43, 99, 223, and 340 GHz in an
attempt to probe the structure and chemistry of the circumstellar disk and
bipolar outflow associated with this high mass protostar. The continuum
spectral index ranges from $\sim$2 along the midplane of the disk to $\sim$3
along the edges, consistent with dust that is optically thick in the midplane
but becomes optically thin at the periphery. Salt (NaCl) emission is visible
where the dust is optically thin; it provides a unique tracer of the velocity
field within the disk. All other molecules that we have mapped - H$_2$O, AlO,
SiO, SiS, SO, and SO$_2$ - appear to originate primarily in the bipolar
outflow. The base of the outflow is corotating with the disk. SiS shows a
filamentary structure that is most prominent along the edges of the outflow.
The molecular distributions suggest that Si and Al released from dust grains in
the disk react with oxygen derived from H$_2$O to form SiO and AlO, and with SO
and SO$_2$ to form SiS.
