Table 1.
Results from Bayesian linear regression.
| x | y | Intercept | Slope | σ [dex] | ρcorr | τKendall |
|---|---|---|---|---|---|---|
| log(M*/[M⊙]) | log(Mmol/[M⊙]) | −0.04 ± 0.38 | 0.91 ± 0.04 | 0.36 | 0.84 | 0.66 |
| log(SFR/[M⊙ yr−1]) | log(Mmol/[M⊙]) | 8.90 ± 0.02 | 1.02 ± 0.04 | 0.29 | 0.89 | 0.71 |
| log(M*/[M⊙]) | log fmol | −0.38 ± 0.38 | −0.11 ± 0.04 | 0.36 | −0.19 | −0.11 |
| log(M*/[M⊙]) | log(τmol/[yr]) | 7.29 ± 0.32 | 0.16 ± 0.03 | 0.28 | 0.33 | 0.21 |
| log(M*/[M⊙]) | log fHI | 6.16 ± 0.36 | −0.65 ± 0.04 | 0.38 | −0.73 | −0.54 |
Notes. Values quoted are best-fit intercept and slope with 1σ uncertainties from the Bayesian linear fit to the molecular and neutral gas scaling relations of the star-forming sample. Also listed are the intrinsic scatter σ and the linear correlation coefficient ρcorr returned by the fitting procedure. The final column contains an estimate for Kendall’s τ correlation measure obtained taking into account the presence of upper limits.
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