Cloud-scale Molecular Gas Properties in Nearby Galaxies
Molecular gas is believed to be the direct fuel of star formation in galaxies in the local universe. Quantifying the physical properties of molecular gas is a thus crucial step towards building up a successful star formation theory. By analyzing high resolution ALMA imaging data of nearby galaxies, we systematically studied the distribution of molecular gas surface density, velocity dispersion, dynamical state, and turbulent pressure at the scale of individual molecular cloud. This offers by far the most comprehensive view of molecular gas properties in nearby star forming disk galaxies.
This is part of the first round science results coming out of the PHANGS Collaboration.