ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Deriving
  Inclination Angle and Velocity of the Protostellar Jets from their SiO Knots
  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.
