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The study of the development of structures on multiple scales in the coldinterstellar medium has experienced rapid expansion in the past decade, on boththe observational and the theoretical front. Spectral line studies at(sub-)millimeter wavelengths over a wide range of physical scales have providedunique probes of the kinematics of dense gas in star-forming regions, and havebeen complemented by extensive, high dynamic range dust continuum surveys ofthe column density structure of molecular cloud complexes, while dustpolarization maps have highlighted the role of magnetic fields. This has beenaccompanied by increasingly sophisticated numerical simulations including newphysics (e.g., supernova driving, cosmic rays, non-ideal magneto-hydrodynamics,radiation pressure) and new techniques such as zoom-in simulations allowingmulti-scale studies. Taken together, these new data have emphasized theanisotropic growth of dense structures on all scales, from giant ISM bubblesdriven by stellar feedback on $\sim$50-100 pc scales through parsec-scalemolecular filaments down to $<$0.1 pc dense cores and $<$1000 au protostellardisks. Combining observations and theory, we present a coherent picture for theformation and evolution of these structures and synthesize a comprehensivephysical scenario for the initial conditions and early stages of star and diskformation.

From Bubbles and Filaments to Cores and Disks: Gas Gathering and Growth of Structure Leading to the Formation of Stellar Systems