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Gravity drives the collapse of molecular clouds through which stars form, yetthe exact role of gravity in cloud collapse remains a complex issue. Studiespoint to a picture where star formation occurs in clusters. In a typical,pc-sized cluster-forming region, the collapse is hierarchical, and the starsshould be born from regions of even smaller sizes ($\approx 0.1\;\rm pc$). Theorigin of this spatial arrangement remains under investigation. Based on ahigh-quality surface density map towards the Perseus region, we construct a 3Ddensity structure, compute the gravitational potential, and derive eigenvaluesof the tidal tensor ($\lambda_{\rm min}$, $\lambda_{\rm mid}$, $\lambda_{\rmmax}$, $\lambda_{\rm min} < \lambda_{\rm mid} < \lambda_{\rm max}$), analyzethe behavior of gravity at every location and reveal its multiple roles incloud evolution. We find that fragmentation is limited to several isolated,high-density ``islands''. Surrounding them, is a vast amount of gas ($75 \%$ ofthe mass, $95 \%$ of the volume) that stays under the influence of extensivetides where fragmentation is suppressed. This gas will be transported towardsthese regions to fuel star formation. The spatial arrangement of regions underdifferent tides explains the hierarchical and localized pattern of starformation inferred from the observations. Tides were first recognized byNewton, yet this is the first time its dominance in cloud evolution has beenrevealed. We expect this link between cloud density structure and role gravityto be strengthened by future studies, resulting in a clear view of the starformation process.

Tides in clouds: control of star formation by long-range gravitational force