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We use the IllustrisTNG cosmological hydrodynamical simulation to study theevolution of star formation rate (SFR)-density relation over cosmic time. Weconstruct several samples of galaxies at different redshifts from $z=2.0$ to$z=0.0$, which have the same comoving number density. The SFR of galaxiesdecreases with local density at $z=0.0$, but its dependence on local densitybecomes weaker with redshift. At $z\gtrsim1.0$, the SFR of galaxies increaseswith local density (reversal of the SFR-density relation), and its dependencebecomes stronger with redshift. This change of SFR-density relation withredshift still remains even when fixing the stellar masses of galaxies. Thedependence of SFR on the distance to a galaxy cluster also shows a change withredshift in a way similar to the case based on local density, but the reversalhappens at a higher redshift, $z\sim1.5$, in clusters. On the other hand, themolecular gas fraction always decreases with local density regardless ofredshift at $z=0.0-2.0$ even though the dependence becomes weaker when we fixthe stellar mass. Our study demonstrates that the observed reversal of theSFR-density relation at $z\gtrsim1.0$ can be successfully reproduced incosmological simulations. Our results are consistent with the idea thatmassive, star-forming galaxies are strongly clustered at high redshifts,forming larger structures. These galaxies then consume their gas faster thanthose in low-density regions through frequent interactions with other galaxies,ending up being quiescent in the local universe.

Evolution of star formation rate-density relation over cosmic time in a simulated universe: the observed reversal reproduced