Table 2
Analysis of the dependencies of the CO(1–0) line luminosity on galaxy properties.
Model: y = α + βx, with  |
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| Total sample | ||||
| x | α | β | σ intr | ρ |
|
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| log M∗ [M⊙] | −2.5 ± 0.5 | 1.10 ± 0.05 | 0.31 ± 0.02 | 0.926 ± 0.012 |
| log SFR [M⊙ yr-1] | 8.16 ± 0.04 | 1.34 ± 0.07 | 0.21 ± 0.04 | 0.964 ± 0.013 |
| log SSFR [yr-1] | 1.0 ± 3.0 | −0.7 ± 0.3 | 0.83 ± 0.06 | −0.25 ± 0.09 |
| AV [mag]† (CCM89) | 7.13 ± 0.09 | 1.02 ± 0.07 | 0.49 ± 0.03 | 0.80 ± 0.03 |
| AV [mag]† (Calzetti) | 7.13 ± 0.09 | 0.92 ± 0.06 | 0.49 ± 0.03 | 0.80 ± 0.03 |
| 12 + log (O/H) (Tremonti+04) | −25 ± 2 | 3.8 ± 0.2 | 0.39 ± 0.03 | 0.890 ± 0.016 |
| 12 + log (O/H) N2 PP04 | −54 ± 5 | 7.2 ± 0.6 | 0.50 ± 0.04 | 0.84 ± 0.03 |
| 12 + log (O/H) N2 M13 | −68 ± 6 | 9.0 ± 0.7 | 0.51 ± 0.03 | 0.84 ± 0.03 |
| 12 + log (O/H) O3N2 PP04 | −30 ± 3 | 4.4 ± 0.3 | 0.48 ± 0.03 | 0.84 ± 0.02 |
| 12 + log (O/H) O3N2 M13 | −47 ± 4 | 6.6 ± 0.5 | 0.48 ± 0.03 | 0.84 ± 0.02 |
‡
|
−5.6 ± 1.7 | 1.41 ± 0.18 | 0.67 ± 0.05 | 0.64 ± 0.06 |
|
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| Low-M∗ sample (log M∗ [M⊙] < 10.0) | ||||
| x | α | β | σ intr | ρ |
|
|
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| log M∗ [M⊙] | −4.5 ± 1.2 | 1.31 ± 0.13 | 0.29 ± 0.05 | 0.90 ± 0.03 |
| log SFR [M⊙ yr-1] | 8.20 ± 0.07 | 1.56 ± 0.17 | 0.18 ± 0.08 | 0.96 ± 0.04 |
| log SSFR [yr-1] | −6 ± 14 | −1.4 ± 1.5 | 0.71 ± 0.11 | −0.3 ± 0.3 |
| AV [mag]† (CCM89) | 6.85 ± 0.16 | 1.10 ± 0.17 | 0.54 ± 0.07 | 0.66 ± 0.08 |
| AV [mag]† (Calzetti) | 6.86 ± 0.16 | 0.98 ± 0.15 | 0.54 ± 0.07 | 0.66 ± 0.07 |
| 12 + log (O/H) (Tremonti+04) | −21 ± 3 | 3.2 ± 0.3 | 0.30 ± 0.05 | 0.88 ± 0.03 |
| 12 + log (O/H) N2 PP04 | −41 ± 7 | 5.7 ± 0.8 | 0.44 ± 0.06 | 0.80 ± 0.05 |
| 12 + log (O/H) N2 M13 | −52 ± 8 | 7.1 ± 1.0 | 0.45 ± 0.07 | 0.80 ± 0.05 |
| 12 + log (O/H) O3N2 PP04 | −23 ± 4 | 3.6 ± 0.4 | 0.41 ± 0.06 | 0.81 ± 0.04 |
| 12 + log (O/H) O3N2 M13 | −37 ± 5 | 5.3 ± 0.6 | 0.40 ± 0.06 | 0.81 ± 0.05 |
|
‡
|
−3 ± 3 | 1.1 ± 0.3 | 0.59 ± 0.09 | 0.56 ± 0.10 |
|
|
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| High-M∗ sample (log M∗ [M⊙] ≥ 10.0) | ||||
| x | α | β | σ intr | ρ |
|
|
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| log M∗ [M⊙] | −0.5 ± 1.5 | 0.91 ± 0.15 | 0.32 ± 0.03 | 0.60 ± 0.08 |
| log SFR [M⊙ yr-1] | 8.30 ± 0.09 | 1.03 ± 0.15 | 0.24 ± 0.03 | 0.80 ± 0.07 |
| log SSFR [yr-1] | 12.0 ± 1.5 | 0.32 ± 0.15 | 0.39 ± 0.03 | 0.28 ± 0.13 |
| AV [mag]† (CCM89) | 8.26 ± 0.14 | 0.39 ± 0.09 | 0.36 ± 0.03 | 0.46 ± 0.09 |
| AV [mag]† (Calzetti) | 8.27 ± 0.14 | 0.35 ± 0.08 | 0.36 ± 0.03 | 0.45 ± 0.09 |
| 12 + log (O/H) (Tremonti+04) | −2 ± 6 | 1.1 ± 0.7 | 0.39 ± 0.03 | 0.20 ± 0.12 |
| 12 + log (O/H) N2 PP04 | 10 ± 11 | −0.1 ± 1.3 | 0.40 ± 0.03 | −0.01 ± 0.11 |
| 12 + log (O/H) N2 M13 | 10 ± 13 | −0.1 ± 1.6 | 0.40 ± 0.03 | −0.01 ± 0.11 |
| 12 + log (O/H) O3N2 PP04 | 16 ± 7 | −0.8 ± 0.8 | 0.40 ± 0.03 | −0.11 ± 0.12 |
| 12 + log (O/H) O3N2 M13 | 19 ± 11 | −1.2 ± 1.3 | 0.40 ± 0.03 | −0.11 ± 0.12 |
|
‡
|
3.3 ± 1.2 | 0.57 ± 0.13 | 0.34 ± 0.03 | 0.53 ± 0.10 |
Notes. (α,β) are the best-fit linear regression coefficients, σintr is the intrinsic scatter about the best-fit regression line, and ρ is the correlation coefficient. The analysis has been executed using the IDL code linmix_err.pro developed by Kelly (2007), which employes a Bayesian approach to perform a linear regression on a dataset that includes upper limits in y as well as measurement errors on both x and y. For each parameter of interest, the value and the associated error reported in the table correspond respectively to the median and to a robust estimate of the standard deviation of the posterior distribution returned by the code.
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