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Table 2

Analysis of the dependencies of the CO(1–0) line luminosity on galaxy properties.

Model: y = α + βx, with
Total sample
x α β σ intr ρ
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
Low-M∗ sample (log M∗ [M⊙] < 10.0)
x α β σ intr ρ
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
High-M∗ sample (log M∗ [M⊙] ≥ 10.0)
x α β σ intr ρ
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.

(†)

Because of the large measurement errors on AV, of the order of ~ 0.5 mag, the regression analysis for the vs. AV relationships was performed without taking into account the errors on x, in order not to bias the results.

(‡)

In this case the regression analysis was performed by considering only the sources with an Hi line detection.

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