Table 2 represents a full list of observed lines and their measured fluxes from different apertures (arcsecarcsec) taken from field 2: (A) the ring and (B) the inside of the shell. Fig. 1 (bottom panel) shows the location and area of each aperture in the nebula. The top and bottom panels of Fig. 2 show the extracted blue and red spectra after integration over the aperture located on the ring with the strongest lines truncated so the weaker features can be seen. The emission line identification, laboratory wavelength, multiplet number, the transition with the lower- and upper-spectral terms, are given in columns 1-4 of Table 2, respectively. The observed fluxes of the interior and ring, and the fluxes after correction for interstellar extinction are given in columns 5-8. Columns 9 and 10 present the integrated and dereddened fluxes after integration over two apertures (A and B). All fluxes are given relative to H, on a scale where .
|3726 O II||3726.03||F1|
|3729 O II||3728.82||F1||*||*||*||*||*||*|
|3869 Ne III||3868.75||F1||128.93::||199.42::||144.31::||195.22::||145.82::||204.57::|
|3967 Ne III||3967.46||F1||-||-||15.37::||20.26::||-||-|
|4363 O III||4363.21||F2||37.02::||46.58::||5.60||6.57||5.15||6.15|
|4686 He II||4685.68||3-4||80.97||87.87||29.98||31.72||41.07||43.76|
|4959 O III||4958.91||F1||390.90||373.57||173.63||168.27||224.48||216.72|
|5007 O III||5006.84||F1||1347.80||1259.76||587.22||560.37||763.00||724.02|
|5412 He II||5411.52||4-7||19.33||15.01||5.12||4.30||6.90||5.68|
|5755 N II||5754.60||F3||7.08:||4.90:||13.69||10.61||10.17||7.64|
|5876 He I||5875.66||V11||-||-||11.51||8.69||8.96||6.54|
|6548 N II||6548.10||F1||115.24||63.13||629.36||414.79||513.64||321.94|
|6584 N II||6583.50||F1||458.99||249.05||1980.47||1296.67||1642.12||1021.68|
|6678 He I||6678.16||V46||-||-||3.30||2.12||2.68||1.63|
|6716 S II||6716.44||F2||60.63||31.77||131.84||84.25||116.21||70.36|
|6731 S II||6730.82||F2||30.08||15.70||90.39||57.61||76.98||46.47|
|7005 [Ar V]||7005.40||F1||5.46:||2.66:||-||-||-||-|
|7136 Ar III||7135.80||F1||31.81||15.03||26.22||15.59||27.75||15.51|
|7320 O II||7319.40||F2||18.84||8.54||9.00||5.20||10.96||5.93|
|7330 O II||7329.90||F2||12.24||5.53||4.50||2.60||6.25||3.37|
|7751 Ar III||7751.43||F1||46.88||19.38||10.97||5.95||19.05||9.60|
|9069 S III||9068.60||F1||12.32||4.07||13.27||6.16||13.34||5.65|
For each spatially resolved emission line profile, we extracted flux intensity, central wavelength (or centroid velocity), and FWHM (or velocity dispersion). Each emission line profile for each spaxel is fitted to a single Gaussian curve using the MPFIT routine (Markwardt, 2009), an IDL version of the MINPACK-1 FORTRAN code (Moré, 1977), which applies the Levenberg-Marquardt technique to the non-linear least-squares problem. Flux intensity maps of key emission lines of field 2 are shown in Fig.3 for O III 5007, H 6563, N II 6584 and S II 6716; the same ring morphology is visible in the N II map as seen in Fig.1. White contour lines in the figures depict the distribution of the narrow-band emission of H and N II taken with the ESO 3.6 m telescope, which can be used to distinguish the borders between the ring structure and the inside region. We excluded the stellar continuum offset from the final flux maps using MPFIT, so spaxels show only the flux intensities of the nebulae.
The H and H Balmer emission-line fluxes were used to derive the logarithmic extinction at H, , for the theoretical line ratio of the case B recombination ( K and cm; Hummer & Storey, 1987). Each flux at the central wavelength was corrected for reddening using the logarithmic extinction according to
Accordingly, we obtained an extinction of [ ] for the total fluxes (column 9 in Table 2). Our derived nebular extinction is in good agreement with the value found by Exter et al. (2010), for the central star, though they obtained for the nebula. It may point to the fact that all reddening is not due to the interstellar medium (ISM), and there is some dust contribution in the nebula. Adopting a total observed flux value of log(H)= ergcms for the ring and interior structure (Frew et al., 2013a; Frew et al., 2013b; Frew, 2008) and using , lead to the dereddened H flux of log(H)= ergcms.
According to the strength of He II 4686 relative to H, the PN SuWt 2 is classified as the intermediate excitation class with (Dopita & Meatheringham, 1990) or (Reid & Parker, 2010). The EC is an indicator of the central star effective temperature (Reid & Parker, 2010; Dopita & Meatheringham, 1991). Using the -EC relation of Magellanic Cloud PNe found by Dopita & Meatheringham (1991), we estimate kK for . However, we get kK for according to the transformation given by Reid & Parker (2010) for Large Magellanic Cloud PNe.