Kavli Affiliate: Ke Wang
| First 5 Authors: C. Zhang, Tie Liu, Sihan Jiao, Feng-Yao Zhu, Z. -Y. Ren
| Summary:
We report the observations of J=1-0 of HCN, HCO+, H13CO+, and H13CN, HC3N
(J=11-10) emission towards 135 massive star-forming clumps, as part of the
ATOMS (ALMA Three-millimeter Observations of Massive Star-forming regions)
Survey. We present the integrated intensity probability distribution function
for these molecular tracers, modeled as a combination of a log-normal
distribution and a power-law tail. The molecular line luminosities for the
power-law tail segment, Lmol(p), have been calculated. We have investigated the
correlation between the bolometric luminosity, Lbol, and the power-law part of
the molecular line luminosity, Lmol(p). Our findings suggest that the scaling
relationships between Lbol and Lmol(p) for HCN and HCO+ are sublinear,
indicating that these molecules might not be the most effective tracers for the
dense gas. In contrast, H13CN and HC3N exhibit a nearly linear relationship
between Lbol and Lmol(p), indicating that they can well trace gravitationally
bound dense gas. The ratios of Lbol-to-Lmol(p), serving as indicators of star
formation efficiency within massive star-forming clumps, exhibit a weak
anti-correlation with the power-law index in the I-PDF. In addition, the star
formation efficiency is also weakly anti-correlated with the exponent U of the
corresponding equivalent density distribution. Our results implie that clumps
with substantial gas accumulation may still display low star formation
efficiencies.
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