Table 1.
Best-fit linear relations of the diagrams analyzed in this work.
| x | y | Redshift range | Best-fit bins | Best-fit pymc |
|---|---|---|---|---|
| z | log ΣSFR/(M⊙/yr/kpc2) | All | m = 0.21 ± 0.03 | m = 0.16 ± 0.06 |
| q = −0.7 ± 0.2 | q = −0.3 ± 0.4 | |||
| log M⋆/M⊙ | log SFR/(M⊙/yr) | Low-z | m = 0.65 ± 0.09 | m = 0.63 ± 0.07 |
| q = −4.9 ± 0.8 | q = −4.8 ± 0.7 | |||
| log M⋆/M⊙ | log SFR/(M⊙/yr) | High-z | m = 0.4 ± 0.3 | m = 0.63 ± 0.10 |
| q = −3 ± 2 | q = −4.8 ± 1.0 | |||
| log M⋆/M⊙ | log ΣSFR/(M⊙/yr/kpc2) | Low-z | m = 0.17 ± 0.13 | m = 0.2 ± 0.1 |
| q = −1.0 ± 0.9 | q = −1.3 ± 0.8 | |||
| log M⋆/M⊙ | log ΣSFR/(M⊙/yr/kpc2) | High-z | m = 0.2 ± 0.4 | m = 0.16 ± 0.11 |
| q = −1 ± 3 | q = −0.3 ± 1.1 | |||
Notes. The first two columns indicate the x and y axis quantities, while the last two columns highlight the best fit coefficients of the linear relations (y = m × x + q) obtained with two different approaches, as described in the text. The third column indicates whether the relation is derived with the subset at lower redshift (4 < z < 6), at higher redshift (6 < z < 10), or in the entire z range. Only galaxies above the 90% mass completeness limits are used for the fit.
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