Kavli Affiliate: Ke Wang
| First 5 Authors: Rong Liu, Tie Liu, Gang Chen, Hong-Li Liu, Ke Wang
| Summary:
To understand the nature of SiO emission, we conducted ACA observations of
the SiO (2-1) lines toward 146 massive star-forming regions, as part of the
ALMA Three-millimeter Observations of Massive Star-forming regions (ATOMS)
survey. We detected SiO emission in 128 (87.7$%$) sources and identified 171
SiO clumps, 105 of which are spatially separated from 3 mm continuum emission.
A large amount of the SiO line profiles (60$%$) are non-Gaussian. The velocity
dispersion of the SiO lines ranges from 0.3 to 5.43 km s$^{-1}$. In 63 sources
the SiO clumps are associated with H$_rm{II}$ regions characterized by
H40$alpha$ emission. We find that 68$%$ (116) of the SiO clumps are
associated with strong outflows. The median velocity dispersion of the SiO line
for outflow sources and non-outflow sources is 1.91 km s$^{-1}$ and 0.99 km
s$^{-1}$, respectively. These results indicate that outflow activities could be
connected to strongly shocked gas. The velocity dispersion and
[SiO]/[H$^{13}$CO$^+$] intensity ratio do not show any correlation with the
dust temperature and particle number density of clumps. We find a positive
correlation between the SiO line luminosity and the bolometric luminosity,
implying stronger shock activities are associated with more luminous
proto-clusters. The SiO clumps in associations with H$_rm{II}$ regions were
found to show a steeper feature in $L_rm{sio}$/$L_rm{bol}$. The SiO line
luminosity and the fraction of shocked gas have no apparent evidence of
correlation with the evolutionary stages traced by luminosity to mass ratio
($L_rm{bol}/M$).
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