All Tables

Table 1: Flux intensities of the main emission lines detected, measured on the extracted spectra (no slit losses correction applied yet). The first column indicates the label of the spectrum as specified in Fig. 1. In the next eight columns we report the observed fluxes of [OII] (3727 Å), H $\beta$ (4861 Å), [OIII] (4959 + 5007 Å), [OI] (6300 Å), H $\alpha$ +[NII] (6563, 6548 and 6584 Å) and [SII] (6717 Å), respectively. Fluxes are in 10^-16 [erg cm^-2 s^-1]. The last column shows the E(B-V) derived from the Balmer decrement, as described in the text. The last two rows report the fluxes for the two nuclei: the southern consists of spectra #4, 5 and 6, the northern of #13 and 14. The nuclear fluxes are larger than the sum of fluxes in individual spectra, because they were measured on total nuclei extractions and not computed as sums.
Table 2: Observed fluxes and magnitudes of the Superantennae. Optical and IRAS data, from Mirabel et al. (1991), are in the first thirteen rows, the next six rows report the ISOCAM LW bands fluxes by Charmandaris et al. (2002) and finally Klaas et al. (2001) measurements are in the last eleven rows; the 1300 $\mu$ m datum was obtained with SEST, while the others with ISOPHOT. Infrared observations marked with ^* have been splitted between the two nuclei, by means of a procedure described in the text. Integrated IR fluxes were obtained from IRAS data through Sanders & Mirabel (1996) calibration and are expressed in W m^-2.
Table 3: Spatial dependence of the star formation rate ( $M_\odot$ /yr) and extinction (A_V) in Superantennae, as derived from the best fit models. Each row refers to a different SSP; ages and durations, in years, are reported in columns two and three respectively. The following pairs of columns refers to the numbered galaxy regions and provide the SFR and extinction values for each SSP. Values are not shown when the star formation rate is negligible. The bottom three rows in each panel give the total stellar mass sampled by the spectrum and the A_V extinction as computed combining the three youngest populations (young) and all the 10 SSPs (total). See text for more details.
Table 4: Values of the ongoing star formation rate SFR (in $M_\odot$ /yr) derived from: the main emission lines, after correction for extinction and for the AGN contribution, and adopting the the Kennicutt's calibration; from the far-IR luminosity (Kennicutt's calibration); and from our global best-fit model. The latter has been computed combining the two youngest single stellar populations. All SFRs dignostics adopt a Salpeter IMF between 0.1 and 100 $M_\odot$ .