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The star formation history of galaxies is a complex process usuallyconsidered to be stochastic in nature, for which we can only give averagedescriptions such as the color-density relation. In this work we followstar-forming gas particles in a hydrodynamical N-body simulation back in timein order to study their initial spatial configuration. By keeping record of thetime when a gas particle started forming stars we can produce gas-starisochrone surfaces delineating the surfaces of accreting gas that beginproducing stars at different times. These accretion surfaces are closely packedinside dense regions, intersecting each other, and as a result galaxies insideproto-clusters stop accreting gas early, naturally explaining the colordependence on density. The process described here has a purely gravitational /geometrical origin, arguably operating at a more fundamental level than complexprocesses such as AGN and supernovae, and providing a conceptual origin for thecolor-density relation.

Star Formation Isochrone Surfaces: Clues on Star Formation Quenching in Dense Environments