Table 2
Integrated star-forming properties of the sample.
| Object | Reff |
|
|
L24 μm |
|
|
AV | |
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | |
|
|
||||||||
| IRAS06206-6315 | 2.5 | 4.1 ± 0.6 | 11.0 ± 1.7 | ··· | 0.53 ± 0.08 | 1.42 ± 0.22 | 7.4 ± 2.2 | |
| NGC 2369 | 0.5 | 0.73 ± 0.11 | 4.9 ± 0.8 | 1.7 ± 0.3 | 2.0 ± 0.3 | 13.9 ± 2.1 | 21 ± 6 | |
| NGC 3110† | 1.9 | 2.4 ± 0.4 | 5.0 ± 0.8 | 2.4 ± 0.4 | 0.93 ± 0.14 | 2.0 ± 0.3 | 8 ± 2 | |
| NGC 3256‡ | 1.0 | 3.7 ± 0.6 | 6.7 ± 1.0 | 10.1 ± 1.5 | 3.0 ± 0.5 | 5.4 ± 0.8 | 6.6 ± 2.0 | |
| ESO320-G030 | 0.7 | 0.93 ± 0.14 | 1.58 ± 0.24 | 1.8 ± 0.3 | 1.7 ± 0.3 | 2.8 ± 0.4 | 6.1 ± 1.8 | |
| IRAS12112+0305 | 2.6 | 3.8 ± 0.6 | 11.0 ± 1.7 | 14.5 ± 0.5 | 0.46 ± 0.07 | 1.35 ± 0.20 | 8.0 ± 2.4 | |
| IRASF12115-4656 | 1.3 | 1.9 ± 0.3 | 5.1 ± 0.8 | 1.40 ± 0.05 | 0.87 ± 0.13 | 2.4 ± 0.4 | 11 ± 3 | |
| NGC 5135 | 0.5 | 1.35 ± 0.20 | 3.1 ± 0.5 | 3.2 ± 0.5 | 4.1 ± 0.6 | 9.4 ± 1.4 | 9 ± 2 | |
| IRAS14348-1447 | 3.8 | 7.8 ± 1.2 | 18 ± 3 | 20.2 ± 0.7 | 0.44 ± 0.07 | 1.06 ± 0.16 | 6.5 ± 2.0 | |
| IRASF17138-1017 | 0.6 | 1.7 ± 0.3 | 3.3 ± 0.5 | 3.60 ± 0.09 | 4.5 ± 0.7 | 8.9 ± 1.3 | 7.6 ± 2.3 | |
| IRAS17208-0014 | 0.9 | 4.9 ± 0.7 | 13.2 ± 2.0 | 15.2 ± 0.4 | 5.1 ± 0.8 | 13.7 ± 2.1 | 7.3 ± 2.2 | |
| IC 4687 | 1.1 | 4.4 ± 0.7 | 8.3 ± 1.3 | 3.7 ± 0.6 | 3.1 ± 0.5 | 5.8 ± 0.9 | 7.2 ± 2.2 | |
| IRAS21130-4446 | 1.6 | 3.9 ± 0.6 | 8.3 ± 1.3 | ··· | 1.23 ± 0.19 | 2.6 ± 0.4 | 5.7 ± 1.8 | |
| NGC 7130 | 1.0 | 1.62 ± 0.25 | 5.4 ± 0.8 | 3.3 ± 0.5 | 1.24 ± 0.19 | 4.1 ± 0.6 | 13 ± 4 | |
| IC5179† | 1.6 | 1.7 ± 0.3 | 3.2 ± 0.5 | 1.56 ± 0.23 | 0.66 ± 0.10 | 1.25 ± 0.19 | 7.2 ± 2.2 | |
| IRAS22491-1808 | 1.7 | 2.3 ± 0.4 | 5.6 ± 0.9 | 17.7 ± 0.4 | 0.65 ± 0.10 | 1.56 ± 0.24 | 6.6 ± 2.0 | |
| IRAS23128-5919 | 2.0 | 11.6 ± 1.7 | 30 ± 4 | 18.6 ± 0.5 | 2.4 ± 0.4 | 6.3 ± 0.9 | 7.2 ± 2.2 | |
Notes. Integrated star-forming properties of the sample. Column (2): Hα effective radius in [kpc] from Arribas et al. (2012). Columns (3) and (4): observed (3) and extinction-corrected (4) Paα luminosities measured within Reff, expressed in [×107 L⊙]. The Paα luminosities for the LIRGs are obtained from the Brγ fluxes using the case B recombination factor at T = 10 000 K and ne = 104 cm-3 (Osterbrock & Ferland 2006). Column (5): Spitzer/MIPS 24 μm luminosities from Pereira-Santaella et al. (2011) and archival data, in units of [×1010 L⊙]. Columns (6) and (7): Observed (6) and extinction-corrected (7) ΣSFR in [M⊙ yr-1 kpc-2]. Column (8): AV in magnitudes. All the uncertainties are calculated by a bootstrap method of N = 300 simulations, added in quadrature to the 15% systematic error from the absolute flux calibration.
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