The IFU observations were performed using the Wide Field Spectrograph (WiFeS; Dopita et al., 2007; Dopita et al., 2010) mounted on the 2.3-m Australian National University (ANU) telescope on 2010 April 20. Table 1 presents an observation journal, including the exposure time used for each PN in our WiFeS observations (column 3), and information on the HST observations (columns 5-8).
|Exp. (s)||Obs. Date||Filter||Exp. (s)||Obs. Date||Programme ID|
|Hen3-1333||PNG332.909.9||1200||2010 Apr 20||F606W||56||2002 Sep 17||9463|
|Hen2-113||PNG321.003.9||60,1200||2010 Apr 20||F814W||56||2003 Mar 09||9463|
WiFeS is an image-slicing IFU developed and built for the ANU, feeding a double-beam spectrograph. It has a field-of-view (FOV) of 25 arcsec 38 arcsec and a spatial resolution of 1 arcsec. We used the spectral resolution of . The classical data accumulation mode was used, so a suitable sky window has been selected from the science data for the sky subtraction purpose. We also acquired series of bias, dome flat-field frames, twilight sky flats, arc lamp exposures, wire frames and standard stars for bias-subtraction, flat-fielding and calibrations (fully described by Danehkar, 2014).
The WiFeS data were reduced using the IRAF pipeline WIFES (version 2.14). We utilized the same data reduction procedure described in detail by Danehkar et al. (2013) and Danehkar et al. (2014), which includes flat-fielding, bias-subtraction, wavelength calibration, spatial calibration and flux calibration.