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
defined to include all the flux from
the regions seen in the H image. Below the first three rows
the fluxes are extracted from the images in a square
aperture of 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 10%,
<4% for the H
and H 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.
defined to include all the flux from
the regions seen in the H
image. Below the first three rows
the fluxes are extracted from the images in a square
aperture of 
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. 
10%,
<4% for the H
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.