Quantitative analysis of the molecular gas morphology in nearby disk galaxies
arxiv(2024)
Abstract
We present a quantitative and statistical analysis of the molecular gas
morphology in 73 nearby galaxies using high spatial resolution CO (J=2-1) data
obtained from the Atacama Large Millimeter/submillimeter Array (ALMA) by the
PHANGS large program. We applied three model-independent parameters:
Concentration (C), Asymmetry (A), and Clumpiness (S) which are commonly used to
parameterize the optical and infrared morphology of galaxies. We find a
significant correlation between A and S, with a Spearman's rank correlation
coefficient of 0.62 with a p-value of 4 × 10^-9. This suggests a
higher abundance of molecular clumps (i.e. giant molecular cloud associations)
in galaxies that display stronger distortion or biased large-scale molecular
gas distribution. In addition, the analysis of the C parameter suggests high
central molecular concentration in most barred spiral galaxies investigated in
this study. Furthermore, we found a positive correlation between the length of
the bar structure (R_bar/R_25) and the C parameter, with a
Spearman's rank correlation coefficient of 0.63 with a p-value of 3.8 ×
10^-5 suggesting that larger bar structure can facilitate overall molecular
gas transport and yield higher central concentration than galaxies with shorter
bars. Finally, we offer a possible classification scheme of nearby disk
galaxies which is based on the CAS parameters of molecular gas.
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