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We apply novel survival analysis techniques to investigate the relationshipbetween a number of the properties of galaxies and their atomic($M_\mathrm{HI}$) and molecular ($M_{\mathrm{H_2}}$) gas mass, with the aim ofdevising efficient, effective empirical estimators of the cold gas content ingalaxies that can be applied to large optical galaxy surveys. We find that dustattenuation, {\AV}, of both the continuum and nebular emission, showssignificant partial correlations with $M_{\mathrm{H_2}}$, after controlling forthe effect of star formation rate (SFR). The partial correlation between {\AV}and $M_\mathrm{HI}$, however, is weak. This is expected because in poorlydust-shielded regions molecular hydrogen is dissociated by far-ultravioletphotons. We also find that the stellar half-light radius, $R_{50}$, showssignificant partial correlations with both $M_{\mathrm{H_2}}$ and$M_\mathrm{HI}$. This hints at the importance of environment (e.g.,galactocentric distance) on the gas content of galaxies and the interplaybetween gas and SFR. We fit multiple regression to summarize the median, mean,and the $0.15/0.85$ quantile multivariate relationships among$M_{\mathrm{H_2}}$, {\AV}, metallicity, and/or $R_{50}$. A linear combinationof {\AV} and metallicity (inferred from stellar mass) or {\AV} and $R_{50}$,can estimate molecular gas masses within $\sim 2.5-3$ times the observedmasses. If SFR is used in addition, $M_\mathrm{{H_2}}$ can be predicted towithin a factor $\lesssim 2$. In this case, {\AV} and $R_{50}$ are the two bestsecondary parameters that improve the primary relation between$M_\mathrm{{H_2}}$ and SFR. Likewise, $M_\mathrm{HI}$ can be predicted towithin a factor $\lesssim 3$ using $R_{50}$ and SFR.

Dirt-cheap Gas Scaling Relations: Using Dust Absorption, Metallicity and Galaxy Size to Predict Gas Masses for Large Samples of Galaxies