SIMBAD references

We study the effects of the local environment on the molecular gas content of a large sample of log(M_*/M_☉) >= 10 star-forming and starburst galaxies with specific star formation rates (sSFRs) on and above the main sequence (MS) to z ∼ 3.5. ALMA observations of the dust continuum in the COSMOS field are used to estimate molecular gas masses at z ≃ 0.5-3.5. We also use a local universe sample from the ALFALFA H I survey after converting it into molecular masses. The molecular mass (M_ISM) scaling relation shows a dependence on z, M_*, and sSFR relative to the MS, but no dependence on environmental overdensity Δ(M_ISM ∝ Δ^0.03). Similarly, gas mass fraction (f_gas) and depletion timescale (τ) show no environmental dependence to z ∼ 3.5. At <z>∼ 1.8, the average <M_ISM>, <f_gas>, and <τ>in densest regions is (1.6 ± 0.2) x 10¹¹ M_☉, 55 ± 2%, and 0.8 ± 0.1 Gyr, respectively, similar to those in the lowest density bin. Independent of the environment, f_gas decreases and τ increases with increasing cosmic time. Cosmic molecular mass density (ρ) in the lowest density bins peaks at z ∼ 1-2, and this peak happens at z < 1 in densest bins. This differential evolution of ρ across environments is likely due to the growth of the large-scale structure with cosmic time. Our results suggest that the molecular gas content and the subsequent star formation activity of log(M_*/M_☉) >= 10 star-forming and starburst galaxies is primarily driven by internal processes, and not by their local environment since z ∼ 3.5.