Table 5.
Best-fit values for the TFR fitted on the TFR sample.
| Sub-sample | Selec. | Number | Prop. (%) | αTFR | βTFR |
 |
 |
|---|---|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) |
| Small-5 | 87 (1) | 60 | 0.29 | 2.04 ± 0.01 | 0.32 | 2.00 ± 0.02 | |
| Large-5 | 58 (0) | 40 | 1.99 ± 0.01 | 1.97 ± 0.01 | |||
| Small-10 | 94 (1) | 65 | 2.03 ± 0.01 | 2.00 ± 0.02 | |||
| Large-10 | 51 (0) | 35 | 2.00 ± 0.02 | 1.97 ± 0.01 | |||
| Small-15 | 106 (1) | 73 | 2.02 ± 0.01 | 1.99 ± 0.01 | |||
| Large-15 | 39 (0) | 27 | 2.00 ± 0.02 | 1.98 ± 0.02 | |||
| Small-20 | 117 (1) | 81 | 2.02 ± 0.01 | 1.99 ± 0.01 | |||
| Large-20 | 28 (0) | 19 | 1.98 ± 0.02 | 1.97 ± 0.02 | |||
| Small-5 | (vi) | 80 (1) | 69 | 0.41 | 2.02 ± 0.02 | 0.49 | 1.98 ± 0.02 |
| Large-5 | 36 (0) | 31 | 1.98 ± 0.03 | 1.95 ± 0.03 | |||
| Small-10 | 85 (1) | 73 | 2.01 ± 0.02 | 1.98 ± 0.02 | |||
| Large-10 | 31 (0) | 27 | 1.99 ± 0.03 | 1.95 ± 0.03 | |||
| Small-15 | 89 (1) | 77 | 2.01 ± 0.02 | 1.98 ± 0.02 | |||
| Large-15 | 27 (0) | 23 | 2.00 ± 0.03 | 1.95 ± 0.03 | |||
| Small-20 | 98 (1) | 84 | 2.01 ± 0.02 | 1.98 ± 0.02 | |||
| Large-20 | 18 (0) | 16 | 1.97 ± 0.04 | 1.92 ± 0.04 | |||
| Small-5 | 27 (0) | 48 | 0.36 | 2.02 ± 0.03 | 0.47 | 1.98 ± 0.03 | |
| Large-5 | 29 (0) | 52 | 2.01s ± 0.03 | 1.96 ± 0.03 | |||
| Small-10 | 27 (0) | 48 | 2.02 ± 0.03 | 1.98 ± 0.03 | |||
| Large-10 | (vi) | 29 (0) | 52 | 2.01 ± 0.03 | 1.96 ± 0.03 | ||
| Small-15 | and | 29 (0) | 52 | 2.02 ± 0.03 | 1.98 ± 0.03 | ||
| Large-15 | (vii) | 27 (0) | 48 | 2.01 ± 0.03 | 1.95 ± 0.03 | ||
| Small-20 | 38 (0) | 68 | 2.03 ± 0.02 | 1.98 ± 0.03 | |||
| Large-20 | 18 (0) | 32 | 1.99 ± 0.04 | 1.93 ± 0.04 | |||
Notes. Optionally, we also apply a mass cut M⋆ ≤ 1010 M⊙ (vi) and a redshift cut 0.5 ≤ z ≤ 0.9 (vii). For each fit, the slope is fixed to the one from LTSFIT on the entire kinematics sample using the same selection criteria. Bold values correspond to those shown in Fig. 13. (1) Sub-sample name, (2) additional selection criteria applied, (3) number of galaxies in each sub-sample, with outliers in parentheses, (4) proportion of galaxies in each sub-sample (after removing outliers), (5) fixed slope for the TFR using the velocity computed from the mass models, (6) best-fit zero point (mass models), (7) fixed slope using the velocity computed from a flat model, and (8) best-fit zero point (flat model). Errors on fit parameters correspond to 1σ uncertainties.
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