Table B.1.
Spearman correlation coefficient ρS and p-values of the OCLs of all 4 methods divided into sub-samples of barred and unbarred galaxies and AGN-active and inactive galaxies.
| Method | ρall | pall | ρbar | pbar | ρno bar | pno bar | ρAGN | pAGN | ρno AGN | pno AGN |
|---|---|---|---|---|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) |
| Stellar mass correlated with | ||||||||||
| Spectrum 300 pc | 0.53 ± 0.05 | < 0.001 | 0.55 ± 0.06 | < 0.001 | 0.32 ± 0.15 | 0.10 | 0.33 ± 0.11 | 0.17 | 0.44 ± 0.08 | < 0.001 |
| Spectrum 2 kpc | 0.55 ± 0.06 | < 0.001 | 0.62 ± 0.07 | < 0.001 | 0.44 ± 0.12 | 0.02 | 0.68 ± 0.08 | 0.001 | 0.45 ± 0.09 | < 0.001 |
| pv–diagram | 0.53 ± 0.04 | < 0.001 | 0.57 ± 0.05 | < 0.001 | 0.30 ± 0.10 | 0.12 | 0.40 ± 0.10 | 0.09 | 0.45 ± 0.05 | < 0.001 |
| lwm | 0.44 ± 0.05 | < 0.001 | 0.46 ± 0.06 | 0.002 | 0.19 ± 0.11 | 0.34 | 0.18 ± 0.1 | 0.47 | 0.39 ± 0.06 | 0.002 |
| SFR correlated with | ||||||||||
| Spectrum 300 pc | 0.44 ± 0.05 | < 0.001 | 0.33 ± 0.06 | 0.03 | 0.19 ± 0.14 | 0.34 | 0.55 ± 0.09 | 0.015 | 0.3 ± 0.08 | 0.02 |
| Spectrum 2 kpc | 0.47 ± 0.06 | < 0.001 | 0.44 ± 0.08 | 0.003 | 0.28 ± 0.14 | 0.15 | 0.64 ± 0.09 | 0.003 | 0.35 ± 0.09 | 0.007 |
| pv–diagram | 0.38 ± 0.04 | 0.001 | 0.37 ± 0.06 | 0.01 | -0.04 ± 0.11 | 0.83 | 0.56 ± 0.08 | 0.01 | 0.22 ± 0.06 | 0.09 |
| lwm | 0.33 ± 0.05 | 0.003 | 0.26 ± 0.06 | 0.09 | 0.04 ± 0.12 | 0.82 | 0.46 ± 0.09 | 0.05 | 0.2 ± 0.06 | 0.12 |
Notes. Spearman rank correlation coefficient (ρ) and p-value (p) for all combinations between stellar mass and the individual method OCLs (top half) and SFR and the individual method OCLs used (bottom half). Columns (2) and (3) refer to the coefficients calculated for the full sample. Columns (4)–(7) present the Spearman coefficients for the sub-sample of barred galaxies (R, pbar) and unbarred galaxies (R, pno bar), as described in Section B. Columns (8)–(11) present the Spearman coefficients when dividing the full sample into sub-samples of active galaxies (R, pAGN) and inactive galaxies (R, pno AGN), see Section B. Uncertainties of ρ are achieved via the standard deviation when repeatedly (∼1000 times) perturbing the OCLs and re-calculating the Spearman coefficients.
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