LAUSR

The density structure of the interstellar medium determines where stars form and release energy, momentum and heavy elements, driving galaxy evolution 1 – 4 . Density variations are seeded and amplified by gas motion, but the exact nature of this motion is unknown across spatial scales and galactic environments 5 . Although dense star-forming gas probably emerges from a combination of instabilities 6 , 7 , convergent flows 8 and turbulence 9 , establishing the precise origin is challenging because it requires gas motion to be quantified over many orders of magnitude in spatial scale. Here we measure 10 – 12 the motion of molecular gas in the Milky Way and in nearby galaxy NGC 4321, assembling observations that span a spatial dynamic range 10 −1 –10 3  pc. We detect ubiquitous velocity fluctuations across all spatial scales and galactic environments. Statistical analysis of these fluctuations indicates how star-forming gas is assembled. We discover oscillatory gas flows with wavelengths ranging from 0.3–400 pc. These flows are coupled to regularly spaced density enhancements that probably form via gravitational instabilities 13 , 14 . We also identify stochastic and scale-free velocity and density fluctuations, consistent with the structure generated in turbulent flows 9 . Our results demonstrate that the structure of the interstellar medium cannot be considered in isolation. Instead, its formation and evolution are controlled by nested, interdependent flows of matter covering many orders of magnitude in spatial scale. Statistical analysis of velocity fluctuations in the interstellar medium (ISM) of the Milky Way and NGC 4321 show that the motion of molecular gas over scales ranging from 0.1 to 1,000 pc is similar, and consistent with that generated by a combination of gravity and turbulence. ISM structure at one scale is therefore linked to structure at other scales.