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Recent studies of the nearest star-forming clouds of the Galaxy atsubmillimeter wavelengths with the Herschel Space Observatory have provided uswith unprecedented images of the initial and boundary conditions of the starformation process. The Herschel results emphasize the role of interstellarfilaments in the star formation process and connect remarkably well with nearlya decade's worth of numerical simulations and theory that have consistentlyshown that the ISM should be highly filamentary on all scales and starformation is intimately related to self-gravitating filaments. In this review,we trace how the apparent complexity of cloud structure and star formation isgoverned by relatively simple universal processes - from filamentary clumps togalactic scales. We emphasize two crucial and complementary aspects: (i) thekey observational results obtained with Herschel over the past three years,along with relevant new results obtained from the ground on the kinematics ofinterstellar structures, and (ii) the key existing theoretical models and themany numerical simulations of interstellar cloud structure and star formation.We then synthesize a comprehensive physical picture that arises from theconfrontation of these observations and simulations.

From Filamentary Networks to Dense Cores in Molecular Clouds: Toward a New Paradigm for Star Formation