Similar Scaling Relations for the Gas Content of Galaxies across Environments to z ~ 3.5 (1805.10291v2)

Abstract: We study the effects of the local environment on the molecular gas content of a large sample of log($M_{}$/$M_{\odot}$) $\gtrsim$ 10 star-forming and starburst galaxies with specific star-formation rates (sSFRs) on and above the main sequence (MS) to $z$ $\sim$ 3.5. ALMA observations of the dust continuum in the COSMOS field are used to estimate molecular gas masses at $z$ $\approx$ 0.5-3.5. We also use a local universe sample from the ALFALFA HI 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 $\Delta$ ($M_{ISM}$ $\propto$ $\Delta^{0.03}$). Similarly, gas mass fraction (f${gas}$) and depletion timescale ($\tau$) show no environmental dependence to $z$ $\sim$ 3.5. At $\langle z\rangle$ $\sim$ 1.8, the average $\langle M{ISM}\rangle$,$\langle$f${gas}\rangle$, and $\langle \tau \rangle$ in densest regions is (1.6$\pm$0.2)$\times$10$^{11}$ $M{\odot}$, 55$\pm$2%, and 0.8$\pm$0.1 Gyr, respectively, similar to those in the lowest density bin. Independent of the environment, f${gas}$ decreases and $\tau$ increases with increasing cosmic time. Cosmic molecular mass density ($\rho$) in the lowest density bins peaks at $z$ $\sim$ 1-2, and this peak happens at $z$ $<$ 1 in densest bins. This differential evolution of $\rho$ 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($M{*}$/$M_{\odot}$) $\gtrsim$ 10 star-forming and starburst galaxies is primarily driven by internal processes, and not by their local environment since $z$ $\sim$ 3.5.