All Tables

Table 1: Log of the observations. R gives the average spectral resolution as measured from the data. The resolution varies by 10% from one spectrum to the next. The seeing is the one recorded by the observatory DIMM monitor, and not the effective spatial resolution obtained from the data cube.
Table 2: Fluxes for the strong emission lines in units of 10^-16 erg s^-1 cm^-2 corrected for Galactic extinction. The magnitudes are given in AB units. The first three rows correspond to different aperture sizes. For the WR and SN region the radial apertures are 2 $^{\prime \prime }$ defined to include all the flux from the regions seen in the H $\alpha$ image. Below the first three rows the fluxes are extracted from the images in a square aperture of $3\times 3$ spaxels equivalent to 4 arcsec² around the coordinates in Col. 1. The magnitudes are calculated from the spectra extracted within this aperture. Note that the properties vary with the chosen aperture; especially the equivalent widths show differences as described in Sect. 3.4. The oxygen abundance and N/O abundance ratio in the two last columns are discussed in Sect. 3.8. The uncertainties for line fluxes and magnitudes are $\approx$ 10%, <4% for the H $\alpha$ and H $\beta$ EW, 0.12 mag for the reddening, and 0.14 dex for the oxygen abundance calibration. The uncertainty of the N/O ratio is 0.2 dex. The last row gives the mean of the individual regions, and the uncertainty is the standard deviation.
Table 3: Table for derived quantities for the different regions. The last row gives the mean and standard deviation for all the regions. Column 2 is the SFR derived from the observed H $\alpha$ flux, and Col. 3 corrects the SFR for the extinction given in Table 2. Column 4 gives the best fit age. The mass (Col. 5) is determined from population modelling. The mass to light ratio (Col. 6) uses the luminosity L_B derived from the B magnitude relative to the AB magnitude for the sun $M_{B,{\odot }}=5.33$ . Column 7 lists the specific SFR per Gyr normalised to the mass after correction for the host extinction, and Col. 8 lists the luminosity specific SFR, both derived after correcting for intrinsic extinction.