The AMIGA sample of isolated galaxies - IX. Molecular gas properties

U. Lisenfeld; D. Espada; L. Verdes-Montenegro; N. Kuno; S. Leon; J. Sabater; N. Sato; J. Sulentic; S. Verley; M. S. Yun

doi:10.1051/0004-6361/201117056

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	n_up	Slope	Intercept	Slope	Intercept	Corr. coeff
			(bisector)	(bisector)	(M_H₂ dep.)	(M_H₂ dep.)	r
(1)	(2)	(3)	(4)	(5)	(6 )	(7)	(8)

M_H₂ vs. L_B
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 (f_ap < 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


M_H₂ 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 (f_ap < 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

M_H₂ vs. L_K
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(f_ap < 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

M_H₂ vs. L_FIR
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 (f_ap < 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

Σ_SFR vs. Σ_H₂
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 (f_ap < 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 M_H₂ and/or L_FIR. 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 M_H₂ or Σ_H₂ and B is L_B, L_K, L_FIR, (D₂₅)² or Σ_SFR, 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 L_B, L_FIR, L_K, or Σ_SFR as independent variable. Column 8: spearman’s rho correlation coefficient, calculated with ASURV.

^(*)

Only galaxies for which the aperture correction factor, f_ap (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.