Rotating Motion of the Outflow of IRAS 16293-2422 A1 at its Origin Point
  near the Protostar
  The Class 0 protostar IRAS 16293$-$2422 Source A is known to be a binary
system (A1 and A2) or even a multiple system, which processes a complex outflow
structure. We have observed this source in the C$^{34}$S, SO, and OCS lines at
3.1 mm with the Atacama Large Millimeter/submillimeter Array (ALMA). A
substructure of this source is traced by our high angular-resolution
observation (0\farcs12; 20 au) of the continuum emission. The
northwest-southeast (NW-SE) outflow on a 2\arcsec\ scale is detected in the SO
($J_N$ = $2_2$--$1_1$) line. Based on the morphology of the SO distribution,
this bipolar outflow structure seems to originate from the protostar A1 and its
circumstellar disk, or the circummultiple structure of Source A. The rotation
motion of the NW-SE outflow is detected in the SO and OCS emissions. We
evaluate the specific angular momentum of the outflowing gas to be $(8.6 -
14.3) \times 10^{-4}$ km s$^{-1}$ pc. If the driving source of this outflow is
the protostar A1 and its circumstellar disk, it can be a potential mechanism to
extract the specific angular momentum of the disk structure. These results can
be a hint for the outflow launching mechanism in this source. Furthermore, they
provide us with an important clue to resolve the complicated structure of IRAS
16293$-$2422 Source A.
