학술논문
ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Deriving Inclination Angle and Velocity of the Protostellar Jets from their SiO Knots
Document Type
Working Paper
Author
Jhan, Kai-Syun; Lee, Chin-Fei; Johnstone, Doug; Liu, Tie; Liu, Sheng-Yuan; Hirano, Naomi; Tatematsu, Kenichi; Dutta, Somnath; Moraghan, Anthony; Shang, Hsien; Lee, Jeong-Eun; Li, Shanghuo; Liu, Chun-Fan; Hsu, Shih-Ying; Kwon, Woojin; Sahu, Dipen; Liu, Xun-Chuan; Kim, Kee-Tae; Luo, Qiuyi; Qin, Sheng-Li; Sanhueza, Patricio; Bronfman, Leonardo; Qizhou, Zhang; Eden, David; Traficante, Alessio; Lee, Chang Won
Source
Subject
Language
Abstract
We have selected six sources (G209.55-19.68S2, G205.46-14.56S1$_{-}$A, G203.21-11.20W2, G191.90-11.21S, G205.46-14.56S3, and G206.93-16.61W2) from the Atacama Large Millimeter/submillimeter Array Survey of Orion Planck Galactic Cold Clumps (ALMASOP), in which these sources have been mapped in the CO (J=2-1), SiO (J=5-4), and C$^{18}$O (J=2-1) lines. These sources have high-velocity SiO jets surrounded by low-velocity CO outflows. The SiO jets consist of a chain of knots. These knots have been thought to be produced by semi-periodical variations in jet velocity. Therefore, we adopt a shock-forming model, which uses such variations to estimate the inclination angle and velocity of the jets. We also derive the inclination angle of the CO outflows using the wide-angle wind-driven shell model, and find it to be broadly consistent with that of the associated SiO jets. In addition, we apply this shock-forming model to another three protostellar sources with SiO jets in the literature -- HH 211, HH 212, and L1448C(N) -- and find that their inclination angle and jet velocity are consistent with those previously estimated from proper motion and radial velocity studies.