Table 5
Best bysector linear fitting, Pearson correlation coefficients and dispersion perpendicolar to the best-fit for the radius vs. stellar mass and radius vs. Hi mass presented in Fig. 5.
Sample | Band | N | a | b | r | σ |
|
||||||
log (RISO) = a × log (M∗) + b | ||||||
All | i | 312 | 0.38 ± 0.01 | –2.83 ± 0.06 | 0.85 | 0.13 |
NUV | 299 | 0.42 ± 0.04 | –3.20 ± 0.10 | 0.47 | 0.24 | |
FUV | 265 | ... | ... | 0.11 | ... | |
E-S0a | i | 61 | 0.48 ± 0.02 | –4.04 ± 0.11 | 0.94 | 0.07 |
NUV | 58 | 0.43 ± 0.03 | –3.69 ± 0.19 | 0.80 | 0.11 | |
FUV | 43 | 0.59 ± 0.10 | –5.75 ± 0.42 | 0.59 | 0.18 | |
≥ Sa & DefHI < 0.5 | i | 156 | 0.41 ± 0.02 | –3.12 ± 0.10 | 0.80 | 0.13 |
NUV | 150 | 0.42 ± 0.03 | –3.04 ± 0.13 | 0.63 | 0.17 | |
FUV | 142 | 0.47 ± 0.05 | –3.55 ± 0.16 | 0.54 | 0.21 | |
≥ Sa & DefHI ≥ 0.5 | i | 89 | 0.41 ± 0.02 | –3.15 ± 0.11 | 0.87 | 0.12 |
NUV | 86 | 0.40 ± 0.04 | –3.11 ± 0.16 | 0.68 | 0.18 | |
FUV | 78 | 0.55 ± 0.10 | –4.68 ± 0.28 | 0.45 | 0.30 | |
|
||||||
log (RISO) = a × log (MHI) + b | ||||||
≥ Sa & DefHI < 0.5 | i | 156 | 0.56 ± 0.03 | –4.3 ± 0.2 | 0.69 | 0.16 |
NUV | 157 | 0.50 ± 0.02 | –3.6 ± 0.1 | 0.85 | 0.10 | |
FUV | 148 | 0.53 ± 0.02 | –4.0 ± 0.1 | 0.87 | 0.10 | |
|
||||||
log (R50) = a × log (MHI) + b | ||||||
≥ Sa & DefHI < 0.5 | i | 156 | 0.58 ± 0.04 | –4.9 ± 0.2 | 0.64 | 0.17 |
NUV | 156 | 0.66 ± 0.04 | –5.6 ± 0.1 | 0.72 | 0.17 | |
FUV | 147 | 0.67 ± 0.04 | –5.7 ± 0.2 | 0.74 | 0.16 |
Notes. The best linear fitting parameters are provided only when the Pearson correlation coefficient gives a probability higher than ~95% that the two variables are correlated.
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