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The cloud-scale density, velocity dispersion, and gravitational boundednessof the interstellar medium (ISM) vary within and among galaxies. In turbulentmodels, these properties play key roles in the ability of gas to form stars.New high fidelity, high resolution surveys offer the prospect to measure thesequantities across galaxies. We present a simple approach to make suchmeasurements and to test hypotheses that link small-scale gas structure to starformation and galactic environment. Our calculations capture the key physics ofthe Larson scaling relations, and we show good correspondence between ourapproach and a traditional "cloud properties" treatment. However, we argue thatour method is preferable in many cases because of its simple, reproduciblecharacterization of all emission. Using, low-J 12CO data from recent surveys,we characterize the molecular ISM at 60pc resolution in the Antennae, the LargeMagellanic Cloud, M31, M33, M51, and M74. We report the distributions ofsurface density, velocity dispersion, and gravitational boundedness at 60pcscales and show galaxy-to-galaxy and intra-galaxy variations in each. Thedistribution of flux as a function of surface density appears roughly lognormalwith a 1sigma width of ~0.3 dex, though the center of this distribution variesfrom galaxy to galaxy. The 60pc resolution line width and molecular gas surfacedensity correlate well, which is a fundamental behavior expected for virializedor free-falling gas. Varying the measurement scale for the LMC and M31, we showthat the molecular ISM has higher surface densities, lower line widths, andmore self-gravity at smaller scales.

astrophysical journal/the astrophysical journal

A Portrait of Cold Gas in Galaxies at 60pc Resolution and a Simple  Method to Test Hypotheses That Link Small-Scale ISM Structure to Galaxy-Scale  Processes