Extremely high excitation SiO lines in disk-outflow system in Orion
  Source I
  We present high-resolution images of the submillimeter SiO line emissions of
a massive young stellar object Orion Source I using the Atacama Large
Millimeter/ Submillimeter Array (ALMA) at band 8. We detected the 464 GHz SiO
v=4 J=11-10 line in Source I, which is the first detection of the SiO v=4 line
in star-forming regions, together with the 465 GHz 29SiO v=2 J=11-10 and the
428 GHz SiO v=2 J=10-9 lines with a resolution of 50 AU. The 29SiO v=2 J=11-10
and SiO v=4 J=11-10 lines have compact structures with the diameter of <80 AU.
The spatial and velocity distribution suggest that the line emissions are
associated with the base of the outflow and the surface of the edge-on disk. In
contrast, SiO v=2 J=10-9 emission shows a bipolar structure in the direction of
northeast-southwest low-velocity outflow with ~200 AU scale. The emission line
exhibits a velocity gradient along the direction of the disk elongation. With
the assumption of the ring structure with Keplerian rotation, we estimated the
lower limit of the central mass to be 7 solar mass and the radius of 12 AU< r
<26 AU.
