Table 2
Typical flux-percentage error, offset
and C2 kpc values for the (U)LIRGs in the VIMOS
sample.
| IRAS | Percentage | Offset |
(6 kpc) |
(6 kpc) |
(all FOV) |
(all FOV) |
| error | (kpc) | |||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) |
|
|
||||||
| F01159−4443N | 5.8 | 0.0 | – | 0.72 ± 0.06 | – | 0.61 ± 0.05 |
| F01159−4443S | 5.8 | 0.1 | – | – | – | |
| F01341−3735N | 12.7 | 0.1 | 0.27 ± 0.05 | 0.52 ± 0.09 | 0.16 ± 0.03 | 0.39 ± 0.07 |
| F01341−3735S | 8.8 | 0.2 | 0.42 ± 0.05 | 0.81 ± 0.10 | 0.41 ± 0.05 | 0.81 ± 0.10 |
| F04315−0840 | 15.1 | 0.1 | 0.37 ± 0.08 | 0.61 ± 0.13 | 0.31 ± 0.07 | 0.62 ± 0.13 |
| F05189−2524 | 10.1 | 0.1 | 0.41 ± 0.06 | 0.56 ± 0.08 | 0.29 ± 0.04 | 0.56 ± 0.08 |
| F06035−7102E | 10.4 | 1.0 | 0.17 ± 0.03 | 0.24 ± 0.03 | 0.04 ± 0.01 | 0.06 ± 0.01 |
| F06035−7102W | 10.4 | 0.4 | – | – | – | |
| F06076−2139N | 6.9 | 0.0 | 0.24 ± 0.02 | 0.75 ± 0.07 | 0.10 ± 0.01 | 0.28 ± 0.03 |
| F06076−2139S | 6.9 | 0.0 | – | – | – | – |
| F06206−6135 | 7.6 | 0.8 | 0.11 ± 0.01 | 0.21 ± 0.02 | 0.06 ± 0.01 | 0.10 ± 0.01 |
| F06259−4708N | 11.6 | 0.2 | 0.25 ± 0.04 | 0.48 ± 0.08 | 0.17 ± 0.03 | 0.27 ± 0.04 |
| F06259−4708C | 11.6 | 0.7 | 0.28 ± 0.05 | 0.29 ± 0.05 | 0.22 ± 0.04 | 0.46 ± 0.08 |
| F06259−4708S | 11.6 | 0.8 | 0.27 ± 0.04 | 0.33 ± 0.05 | 0.17 ± 0.03 | 0.22 ± 0.04 |
| F06295−1735 | 9.6 | 1.1 | – | 0.30 ± 0.04 | – | 0.16 ± 0.02 |
| F06592−6313 | 18.0 | 0.0 | 0.40 ± 0.10 | 0.72 ± 0.14 | 0.37 ± 0.10 | 0.70 ± 0.17 |
| F07027−6011N | 9.6 | 0.0 | 0.42 ± 0.06 | 0.28 ± 0.15 | 0.33 ± 0.04 | 0.23 ± 0.03 |
| F07027−6011S | 14.5 | 0.2 | 0.37 ± 0.08 | 0.55 ± 0.04 | 0.33 ± 0.07 | 0.55 ± 0.11 |
| F07160−6215 | 17.7 | 0.2 | 0.29 ± 0.07 | 0.60 ± 0.11 | 0.29 ± 0.07 | 0.60 ± 0.15 |
| 08355−4944 | 14.0 | 0.1 | 0.36 ± 0.07 | 0.58 ± 0.15 | 0.29 ± 0.06 | 0.55 ± 0.11 |
| 08424−3130NE | 12.4 | 0.1 | – | – | – | – |
| 08424−3130SW | 12.4 | 0.1 | - | – | – | – |
| F08520−6850 | 12.0 | 1.1 | 0.17 ± 0.03 | 0.35 ± 0.06 | 0.06 ± 0.01 | 0.26 ± 0.04 |
| 09022−3615 | 14.4 | 0.1 | 0.22 ± 0.04 | 0.26 ± 0.05 | 0.14 ± 0.03 | 0.23 ± 0.05 |
| F09437 + 0317N | 17.4/8.7 | 6.3 | – | – | – | – |
| F09437 + 0317S | 19.0 | 4.1 | 0.17 ± 0.05 | 0.11 ± 0.03 | 0.11 ± 0.03 | 0.08 ± 0.02 |
| F10015−0614 | 3.7 | 0.1 | 0.29 ± 0.02 | 0.26 ± 0.01 | 0.23 ± 0.01 | 0.16 ± 0.01 |
| F10038−3338 | 21.0 | 0.1 | 0.19 ± 0.06 | 0.52 ± 0.15 | 0.15 ± 0.04 | 0.52 ± 0.15 |
| F10257−4339 | 6.3 | 0.0 | 0.26 ± 0.02 | 0.30 ± 0.03 | 0.26 ± 0.02 | 0.30 ± 0.03 |
| F10409−4556 | 15.8 | 0.2 | 0.26 ± 0.06 | 0.21 ± 0.05 | 0.26 ± 0.06 | 0.12 ± 0.03 |
| F10567−4310 | 9.4 | – | – | 0.53 ± 0.07 | – | 0.25 ± 0.03 |
| F11255−4120 | 8.0 | 0.0 | 0.25 ± 0.03 | 0.37 ± 0.04 | 0.16 ± 0.02 | 0.24 ± 0.03 |
| F11506−3851 | 18.6 | 0.8 | 0.54 ± 0.14 | 0.48 ± 0.12 | 0.54 ± 0.14 | 0.48 ± 0.12 |
| F12043−3140N | 8.2 | 0.1 | 0.39 ± 0.04 | 0.75 ± 0.08 | 0.35 ± 0.04 | 0.75 ± 0.08 |
| F12043−3140S | 8.2 | 2.2 | 0.19 ± 0.02 | 0.20 ± 0.02 | 0.18 ± 0.02 | 0.20 ± 0.02 |
| 12115−4656 | 7.1 | 0.6 | 0.28 ± 0.03 | 0.29 ± 0.03 | 0.23 ± 0.02 | 0.29 ± 0.03 |
| 12116−5615 | 18.8 | 0.2 | 0.32 ± 0.08 | 0.75 ± 0.18 | 0.29 ± 0.07 | 0.75 ± 0.18 |
| F12596−1529E | 9.6 | 0.5 | – | – | – | – |
| F12596−1529W | 9.6 | 0.0 | – | – | – | – |
| F13001−2339 | 9.3 | 0.2 | 0.20 ± 0.03 | 0.51 ± 0.06 | 0.13 ± 0.02 | 0.48 ± 0.06 |
| F13229−4255 | 9.8 | 0.1 | 0.45 ± 0.06 | 0.69 ± 0.10 | 0.45 ± 0.06 | 0.69 ± 0.10 |
| F14544−4255E | 17.2 | 2.4 | 0.33 ± 0.08 | 0.51 ± 0.12 | 0.28 ± 0.07 | 0.18 ± 0.04 |
| F14544−4255W | 10.8 | 0.3 | 0.28 ± 0.04 | 0.70 ± 0.11 | 0.19 ± 0.03 | 0.70 ± 0.11 |
| F17138−1017 | 16.1 | – | – | 0.64 ± 0.14 | – | 0.64 ± 0.14 |
| F18093−5744N | 10.5 | 0.5 | 0.27 ± 0.04 | 0.32 ± 0.05 | 0.24 ± 0.03 | 0.32 ± 0.05 |
| F18093−5744C | 15.1 | 1.5 | – | 0.80 ± 0.17 | – | 0.79 ± 0.17 |
| F18093−5744S | 9.4 | 0.1 | 0.28 ± 0.04 | 0.39 ± 0.05 | 0.27 ± 0.03 | 0.39 ± 0.05 |
| F21130−4446 | 10.6 | 4.2 | 0.15 ± 0.02 | 0.26 ± 0.04 | 0.06 ± 0.01 | 0.05 ± 0.01 |
| F21453−3511 | 11.2 | 0.0 | 0.21 ± 0.03 | 0.27 ± 0.04 | 0.21 ± 0.03 | 0.27 ± 0.04 |
| F22132−3705 | 5.0 | 2.0 | 0.17 ± 0.01 | 0.16 ± 0.01 | 0.11 ± 0.01 | 0.15 ± 0.01 |
| F22491−1808 | 20.4 | 0.4 | 0.17 ± 0.05 | 0.17 ± 0.05 | 0.06 ± 0.02 | 0.12 ± 0.03 |
| F23128−5919N | 8.7 | 0.4 | 0.18 ± 0.02 | 0.30 ± 0.04 | 0.08 ± 0.01 | 0.17 ± 0.02 |
| F23128−5919S | 8.7 | 0.1 | – | – | – | – |
Notes. Column (1): IRAS name. Column (2): typical flux percentage error for all the galaxies in our sample. Note that for some multiple systems two or even three VIMOS pointings were used to cover the emission from each individual galaxy of the system (see Sect. 3 and Fig. 1 for details). For these objects, typical flux percentage errors were estimated for each individual pointing (e.g. IRAS F18093-5744). In the case of IRAS F09437+0317 two pointings were used to cover most of the emission from the northern source. The typical percentage error for each pointing is indicated in the table for this source. Column (3): the offsets in kpc between the peaks of the continuum and the Hα emissions. Column (4): the concentration C2 kpc of the continuum emission for the galaxies in our sample defining as “total flux” the flux within the same physical region (6 kpc × 6 kpc) for all galaxies in our sample. Column (5): same as Col. (4) but for the Hα images. Column (6): same as Col. (4) but using the entire FOV of our VIMOS images. Column (7): same as Col. (5) but using the entire FOV of our VIMOS images. The formal error associated to the C2 kpc values in the table has been calculated using the typical percentage errors given in Col. (2). For IRAS F08424-3130, IRAS F12596-1529 and IRAS F09437 + 0317 (IC 564) it is not possible to adequately measure C2 kpc (see text for details). In addition, the low S/N of the continuum images in the cases of IRAS F01159-4443 and IRAS F06295-1735, important contamination by a bright star in the field for the central system of IRAS F18093-5744 and the presence of vertical patterns in the cases of IRAS F10567-4310 and IRAS F17138-1017, prevents any attempt to measure C2 kpc for the continuum images of these five sources.
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