EDP Sciences logo
Subscriber Authentication Point
Search
Menu
Home All issues Volume 534 (October 2011) A&A, 534 (2011) A102 Full HTML
Free Access

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.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.