From Filamentary Networks to Dense Cores in Molecular Clouds: Toward a
  New Paradigm for Star Formation
  Recent studies of the nearest star-forming clouds of the Galaxy at
submillimeter wavelengths with the Herschel Space Observatory have provided us
with unprecedented images of the initial and boundary conditions of the star
formation process. The Herschel results emphasize the role of interstellar
filaments in the star formation process and connect remarkably well with nearly
a decade's worth of numerical simulations and theory that have consistently
shown that the ISM should be highly filamentary on all scales and star
formation is intimately related to self-gravitating filaments. In this review,
we trace how the apparent complexity of cloud structure and star formation is
governed by relatively simple universal processes - from filamentary clumps to
galactic scales. We emphasize two crucial and complementary aspects: (i) the
key observational results obtained with Herschel over the past three years,
along with relevant new results obtained from the ground on the kinematics of
interstellar structures, and (ii) the key existing theoretical models and the
many numerical simulations of interstellar cloud structure and star formation.
We then synthesize a comprehensive physical picture that arises from the
confrontation of these observations and simulations.
