2022ApJ...925...49R

Many astrochemical models of observed CO isotopologue line emission, earlier considered a good proxy measure of H₂ and hence disk gas mass, favor large deviations in the carbon and oxygen gas phase abundances and argue that severe gas phase CO depletion makes it a poor mass tracer. Here, we show that C¹⁸O line emission is an effective measure of the gas mass, and despite its complex chemistry, a possibly better tracer than HD. Our models are able to reproduce C¹⁸O emission from recent Atacama Large Millimeter/submillimeter Array surveys and the TW Hya disk to within a factor of ∼2-3 using carbon and oxygen abundances characteristic of the interstellar medium (C/H = 1.4 x 10^–4; O/H = 3.2 x 10^–4) without having to invoke unusual chemical processing. Our gas and dust disk structure calculations considering hydrostatic pressure equilibrium and our treatment of the CO conversion on grains are primarily responsible for the very different conclusions on disk masses and CO depletion. As did previous studies, we find that a gas phase C/O of ∼1-2 can explain observed hydrocarbon emission from the TW Hya disk; but significantly, we find that CO isotopologue emission is only marginally affected by the C/O ratio. We therefore conclude that C¹⁸O emission provides estimates of disk masses that are uncertain only to within a factor of a few, and describe a simplified modeling procedure to obtain gas disk masses from C¹⁸O emission lines.