Table 2
Parameters of the H iK-band and baryonic TFR.
| TFR | Slope a | Intercept b | σ | ρ |
|
|
||||
| K-band | ||||
| unconstrained | −4.67 ± 0.99 | −23.25 ± 0.12 | 0.43 | 0.74 |
| slope fixed | −8.38 (CO) | −23.31 ± 0.17 | 0.67 | |
| slope fixed | −8.78 (TP00) | −23.32 ± 0.18 | 0.69 | |
| slope fixed | −9.13 (WBC10) | −23.32 ± 0.19 | 0.72 | |
| slope fixed | −9.64 (NV07) | −23.33 ± 0.20 | 0.77 | |
|
|
||||
| Baryonic | ||||
| unconstrained (JAM) | 2.38 ± 0.25 | 10.71 ± 0.03 | 0.24 | 0.94 |
| unconstrained (SFH) | 2.51 ± 0.42 | 10.71 ± 0.05 | 0.47 | 0.80 |
| slope fixed (JAM) | 3.36 (NV07) | 10.72 ± 0.04 | 0.39 | |
| slope fixed (SFH) | 3.36 (NV07) | 10.72 ± 0.06 | 0.57 | |
| slope fixed (JAM) | 3.84 (McG12) | 10.73 ± 0.05 | 0.50 | |
Notes. The rows in the table present the best-fitting parameters for the K-band TFR (all inverse fits) and the JAM baryonic TFR for the 16 galaxies in Table 1. The slopes without uncertainties correspond to the cases where the slope has been fixed to a reference TFR: CO: Davis et al. (2011), TP00: Tully & Pierce (2000), WBC10: Williams et al. (2010), NV07: Noordermeer & Verheijen (2007) and McG: McGaugh (2012). The scatter σ in mass of the baryonic TFR has been converted into magnitudes by multiplying by 2.5. The last column gives the correlation coefficient of the data.
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