Table 1.
Best-fit parameters for the stellar TFR and the stellar FR in the SPARC sample using different methods of estimating M⋆.
TFR (68 galaxies),  , y = M⋆/M⊙ |
||||
|---|---|---|---|---|
| Method | a | b | σM⋆ | σ⊥ |
| dyn | 4.89 ± 0.21 | 10.20 ± 0.04 | 0.262 | 0.053 |
| phot | 5.21 ± 0.18 | 10.16 ± 0.03 | 0.274 | 0.052 |
| MSC | 3.97 ± 0.20 | 9.93 ± 0.04 | 0.302 | 0.074 |
| Υdisk = 0.5 | 4.90 ± 0.17 | 10.17 ± 0.03 | 0.259 | 0.052 |
| FR (55 galaxies), x = M⋆/1010.5 M⊙, y = j⋆/km s−1 kpc−1 | ||||
| Method | a | b | σj⋆ | σ⊥ |
| dyn | 0.62 ± 0.03 | 3.00 ± 0.02 | 0.183 | 0.155 |
| phot | 0.52 ± 0.03 | 3.04 ± 0.03 | 0.171 | 0.151 |
| MSC | 0.66 ± 0.04 | 3.27 ± 0.03 | 0.186 | 0.155 |
| Υdisk = 0.5 | 0.57 ± 0.03 | 3.04 ± 0.03 | 0.179 | 0.155 |
Notes.dyn–rotation curve decomposition, phot–SED modelling, MSC–marginal stability condition, Υdisc = 0.5 – Equation (1) with a constant Υdisc of 0.5. Fits are in the form log(y)=a log(x)+b, with x and y defined in the Table headers. σM⋆ (or σj⋆) and σ⊥ are the observed vertical and orthogonal scatter, respectively.
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