摘要：Using the line ratio between the SiO (5–4) and the SiO (2–1)
observed by Zhang et al. (2000) with a synthesized beam of
9.
?? 5×8. ?? 0, we derived the physical conditions of the gas in the
high-velocity clumps. For our analysis we selected the portion
of the high-velocity range that is less affected by the miss-
ing flux. The analysis was performed at the B0i and B1a po-
sitions, at which the SiO (5–4) emission was detected above the
5σ level. We note that an analysis using several SiO lines ob-
served with a single-dish telescope has been made by Nisini
et al. (2007). However, they used single-pointing observations,
which means that the data were taken with different beam sizes,
for instance ∼27 ?? for SiO (2–1) and ∼11 ?? for SiO (5–4). In addi-
tion, the line ratios used the total integrated intensity, including
the low-velocitycomponent,whereas we used higher-resolution
data and focused on the high-velocity component.
关键词：Shock waves;ISM: jets and outflows;Stars: formation;ISM: individual objects: L1157;errata, addenda
