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Table 2

Results from the integrated spectra analysis.

ID1 IS Q V B σ B V other σ other V adopted σ adopted
IRAS Å % km s-1 km s-1 km s-1 km s-1 km s-1 km s-1
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)

F01159-4443 (N) 1.4 ± 0.1 30 2 –237 ± 13 127 ± 18 13 ± 3 102 ± 16 –237 ± 13 127 ± 18
F01159-4443 (S) 1.2 ± 0.1 100 2 ··· ··· ··· ··· ··· ···
F01341-3735 (N) 0.9 ± 0.1 72 3 –278 ± 8 71 ± 3 –105 ± 4 76 ± 6 –192 ± 6 74 ± 5
F01341-3735 (S) 1.0 ± 0.2 49 2 ··· ··· 41 ± 4 80 ± 8 41 ± 4 80 ± 8
F04315-0840 0.6 ± 0.1 20 3 –186 ± 21 104 ± 11 –8 ± 5 109 ± 17 –186 ± 21 104 ± 11
F05189-2524 0.7 ± 0.1 38 2 –725 ± 26 150 ± 13 –451 ± 11 87 ± 7
F06035-7102 (0.6 ± 0.1) (77) 1 ··· ··· ··· ··· ··· ···
F06076-2139 (N) 0.7 ± 0.1 30 3 –172 ± 29 102 ± 9 ··· ···
F06076-2139 (S) 0.8 ± 0.1 64 2 –176 ± 16 139 ± 14 ··· ··· –176 ± 16 139 ± 14
F06206-6315 (1.9 ± 2.3) (100) 1 ··· ··· ··· ··· ··· ···
F06259-4780 (N) 0.9 ± 0.1 23 2 –234 ± 9 117 ± 2 –97 ± 3 91 ± 8 –166 ± 6 104 ± 6
F06259-4780 (C) 0.4 ± 0.1 39 2 –3 ± 4 92 ± 14 181 ±15 81 ± 24 93 ± 38 87 ±10
F06259-4780 (S) (1.0 ± 0.3) (72) 1 ··· ··· ··· ··· ··· ···
F06295-1735 (1.4 ± 0.7) (100) 1 ··· ··· ··· ··· ··· ···
F06592-6313 0.8 ± 0.1 25 3 –193 ± 11 148 ± 13 ··· ··· –193 ± 11 148 ± 13
F07027-6011 (N) 0.6 ± 0.1 21 2 –328 ± 18 92 ± 10 –140 ± 4 71 ± 4 –234 ± 12 87 ± 7
F07027-6011 (S) 0.9 ± 0.1 26 2 –202 ± 18 87 ± 4 –31 ± 4 112 ± 10 –202 ± 18 87 ± 4
F07160-6215 1.2 ± 0.3 39 2 ··· ··· –13 ± 2 132 ± 12 –13 ± 2 132 ± 12
08424-3130 (N) (1.0 ± 0.1) (42) 1 ··· ··· ··· ··· ··· ···
08424-3130 (S) (1.1 ± 0.1) (34) 1 ··· ··· ··· ··· ··· ···
F08520-6850 (1.0 ± 0.1) (100) 1 ··· ··· ··· ··· ··· ···
09022-3615 (1.2 ± 0.4) (100) 1 ··· ··· ··· ··· ··· ···
F09437+0317 (N) 1.3 ± 0.2 30 2 ··· ··· 54 ± 5 93 ± 14 54 ± 5 93 ± 14
F09437+0317 (S) (1.7 ± 0.2) (100) 1 ··· ··· ··· ··· ··· ···
F10015-0614 1.2 ± 0.1 48 2 –116 ± 5 135 ± 4 ··· ··· –116 ± 5 135 ± 4
F10038-3338 0.8 ± 0.1 50 2 –175 ± 5 131 ± 4 ··· ··· –175 ± 5 131 ± 4
F10257-4339 0.6 ± 0.1 28 2 –386 ± 11 97 ± 10 ··· ···
F10409-4556 1.3 ± 0.2 47 3 –180 ± 8 150 ± 6 ··· ··· –180 ± 8 150 ± 6
F10567-4310 1.5 ± 0.2 28 2 –146 ± 6 160 ± 4 ··· ··· –146 ± 6 160 ± 4
F11255-4120 0.8 ± 0.1 18 2 –405 ± 21 148 ± 26 –99 ±11 127 ± 15 –252 ± 21 138 ± 21
F11506-3851 1.2 ± 0.1 30 3 –88 ± 11 108 ± 8 173 ± 18 113 ± 14 –88 ± 11 108 ± 8
F12043-3140 (N) (0.7 ± 0.1) (79) 1 ··· ··· ··· ··· ··· ···
F12043-3140 (S) 0.9 ± 0.1 77 2 –152 ± 16 162 ± 13 ··· ··· –152 ± 16 162 ± 13
F12115-4656 1.5 ± 0.2 73 3 –65 ± 8 119 ± 6 ··· ··· –65 ± 8 119 ± 6
12116-5615 0.8 ± 0.1 22 2 –371 ± 21 98 ± 18 –156 ± 11 96 ± 16 –264 ± 16 97 ± 8
F12596-1529 (1.5 ± 0.2) (100) 1 ··· ··· ··· ··· ··· ···
F13001-2339 (1.2 ± 1.1) (63) 1 ··· ··· ··· ··· ··· ···
F13229-2934 0.5 ± 0.1 67 3 –140 ± 4 106 ± 3 ··· ··· –140 ± 4 106 ± 3
F14544-4255 (E) (0.9 ± 0.1) (41) 1 ··· ··· ··· ··· ··· ···
F14544-4255 (W) (1.9 ± 0.4) (100) 1 ··· ··· ··· ··· ··· ···
F17138-1017 (1.2 ± 0.5) (80) 1 ··· ··· ··· ··· ··· ···
F18093-5744 (N) 1.0 ± 0.1 65 2 –90 ± 14 152 ± 11 ··· ··· –90 ± 14 152 ± 11
F18093-5744 (C) (0.5 ± 0.1) (56) 1 ··· ··· ··· ··· ··· ···
F18093-5744 (S) 0.7 ± 0.1 41 2 ··· ··· –41 ± 4 103 ± 13 –41 ± 4 103 ± 13
F21453-3511 1.1 ± 0.1 97 2 ··· ··· ··· ··· ··· ···
F22132-3705 1.1 ± 0.1 47 3 ··· ··· 36 ± 3 109 ± 12 36 ± 3 109 ± 12
F22491-1808 (0.7 ± 0.1) (90) 1 ··· ··· ··· ··· ··· ···
F23128-5919 (N) 0.8 ± 0.1 99 2 ··· ··· ··· ··· ··· ···
F23128-5919 (S) (0.7 ± 0.1) (98) 1 ··· ··· ··· ··· ··· ···

Notes. Column (1): IRAS name. Column (2): NaD Equivalent width as measured in the model stellar spectra (output of the pPXF routine). Column (3): the estimated percentage contribution to the NaD by old stars (Sect. 3.1). In brackets values obtained from poor fits (i.e., Q = 1, in Col. (4)). Column (4): index of the quality of the stellar modeling of the integrated spectra (after visually inspecting the results of the pPXF analysis). It is defined as follows: 1 doubtful results, 2 and 3 medium and highly reliable results, respectively. We assign Q = to both galaxies in the system 08424-3130, since only a part of the nuclear region of both galaxies is covered by our VIMOS FoV (Fig. A.15). In particular, the area covered by the NaD absorption (and Hα, Bellocchi et al. 2013) for the Northern galaxy is very small, so that its correction for the rotation pattern (Sect. 3.1) is rather inaccurate. Columns (58): velocity and velocity dispersion of the different components derived for the NaD line profiles seen in the decontaminated spectra (i.e., observed – stellar model). The different components are identified according to their velocities. Specifically, the superindex B stands for a blueshifted component (according to the criterion in Sect. 4.2), while “other” indicates a second kinematic component. Such a component is typically narrower with respect to the blueshifted component, and it is found at systemic velocity (i.e., −60 <V< 60km s-1) or redshifted (V> 60km s-1) with respect to the stars. When two blueshifted components are found for the same object, the component with the lowest velocity is in the column dedicated to the “other”-component. Columns (910): adopted values of velocity and velocity dispersion for the 1D-analysis (Sect. 4.2). When two blueshifted components are found, their average values is considered. The symbol indicates the galaxies excluded for the 1D analysis since the Gaussian modeling of the NaD absorption line profile leaves strong residual.

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