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This article has an erratum: [https://doi.org/10.1051/0004-6361/201117056e]


Table 7

Correlation analysis.

Sample n nup Slope Intercept Slope Intercept Corr. coeff
(bisector) (bisector) (MH2 dep.) (MH2 dep.) r
(1) (2) (3) (4) (5) (6 ) (7) (8)

MH2 vs. LB
E-Im (T = (−5)–10) 173 79 1.45  ±   0.08  −5.61 ± 0.77 1.12  ±   0.08  −2.43 ± 0.83 0.66
E-Im (fap < 1.5)* 76 42 1.32  ±  0.10  −4.27 ± 0.94 1.06  ±  0.10  −1.79 ± 0.98 0.63
Sb-Sc (T = 3–5 ) 88 21 1.41  ±  0.10  −5.12 ± 0.97 1.06  ±  0.10  −1.69 ± 1.02 0.65

MH2 vs.
E-Im (T = (−5)–10) 173 79 1.41  ±  0.05 5.10  ±  0.50 0.88  ±  0.09 6.36  ±  0.23 0.52
E-Im (fap < 1.5)* 76 42 1.32  ±  0.08 5.47  ±  0.71 0.91  ±  0.11 6.38  ±  0.26 0.47
Sb-Sc (3-5) 88 21 1.31  ±  0.09 5.50  ±  0.93 0.79  ±  0.10 6.82  ±  0.27 0.53

MH2 vs. LK
E-Im (T = (−5)–10) 157 65 1.05  ±  0.07  −2.27 ± 0.72 0.72  ±  0.07 1.13  ±  0.74 0.64
E-Im(fap < 1.5)* 65 33 0.99  ±  0.09  −1.54 ± 0.96 0.69  ±  0.09 1.41  ±  0.95 0.66
Sb-Sc (T = 3–5) 87 20 1.18  ±  0.07  −3.49 ± 0.78 0.95  ±  0.08  −1.14 ± 0.85 0.74

MH2 vs. LFIR
E-Im (T = (−5)–10) 172 97 1.16  ±  0.08  −2.14 ± 0.72 0.98  ±  0.06  −0.46 ± 0.61 0.80
E-Im (fap < 1.5)* 75 48 1.15  ±  0.13  −2.09 ± 1.23 0.89  ±  0.11 0.28  ±  1.04 0.71
Sb-Sc (T = 3–5) 88 30 1.04  ±  0.06  −1.00 ± 0.55 0.90  ±  0.06 0.29  ±   0.58 0.82

ΣSFR vs. ΣH2
E-Im (T = (−5)–10) 172 97 0.89  ±  0.07  −2.78 ± 0.20 0.82  ±  0.07 2.25  ±  0.20 0.65
E-Im (fap < 1.5)* 75 48 1.00  ±  0.14  −2.77 ± 0.38 0.57  ±  0.10 1.53  ±  0.31 0.56
Sb-Sc (T = 3–5) 88 30 0.88  ±  0.07  −2.82 ± 0.21 0.84  ±  0.08 2.39  ±   0.22 0.71

Notes. The entries are: Column 1: subsample considered. Column 2: total number of galaxies in the respective samples. Column 3: number of galaxies with upper limits in MH2 and/or LFIR. Column 4: bisector slope and its error of the best-fit regression line derived with the Schmitt binning method in the ASURV package. The slope and intercept are defined as log(A) = intercept + log(B)  ×  slope, where A is MH2 or ΣH2 and B is LB, LK, LFIR, (D25)2 or ΣSFR, respectively. Column 5: bisector intercept and its error. Column 6 and 7: slope and intercept and their errors of the best-fit regression line derived with the Schmitt binning method in the ASURV package adopting LB, LFIR, LK, or ΣSFR as independent variable. Column 8: spearman’s rho correlation coefficient, calculated with ASURV.

(*)

Only galaxies for which the aperture correction factor, fap (see Sect. 3.5.1), is less than 1.5.

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