TY - JOUR
T1 - Rotating Motion of the Outflow of IRAS 16293-2422 A1 at Its Origin Point near the Protostar
AU - Oya, Yoko
AU - Watanabe, Yoshimasa
AU - López-Sepulcre, Ana
AU - Ceccarelli, Cecilia
AU - Lefloch, Bertrand
AU - Favre, Cécile
AU - Yamamoto, Satoshi
N1 - Funding Information:
Original content from this work may be used under the terms of the . Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. a Grant-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technologies of Japan 18H05222 a Grant-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technologies of Japan 19H05069 a Grant-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technologies of Japan 19K14753 a Grant-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technologies of Japan 21K13954 yes � 2021. The Author(s). Published by the American Astronomical Society. Creative Commons Attribution 4.0 licence
Publisher Copyright:
© 2021. The Author(s). Published by the American Astronomical Society.
PY - 2021/11/1
Y1 - 2021/11/1
N2 - The Class 0 protostar IRAS 16293-2422 Source A is known to be a binary system (A1 and A2) or even a multiple system that processes a complex outflow structure. We have observed this source in the C34S, SO, and OCS lines at 3.1 mm with the Atacama Large Millimeter/submillimeter Array. A substructure of this source is traced by our high angular-resolution observation (0.″12; 20 au) of the continuum emission. The northwest-southeast (NW-SE) outflow on a 2″ scale is detected in the SO (J N = 22-11) 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) × 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.
AB - The Class 0 protostar IRAS 16293-2422 Source A is known to be a binary system (A1 and A2) or even a multiple system that processes a complex outflow structure. We have observed this source in the C34S, SO, and OCS lines at 3.1 mm with the Atacama Large Millimeter/submillimeter Array. A substructure of this source is traced by our high angular-resolution observation (0.″12; 20 au) of the continuum emission. The northwest-southeast (NW-SE) outflow on a 2″ scale is detected in the SO (J N = 22-11) 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) × 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.
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U2 - 10.3847/1538-4357/ac0a72
DO - 10.3847/1538-4357/ac0a72
M3 - Article
AN - SCOPUS:85119183720
SN - 0004-637X
VL - 921
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 12
ER -