Moderate resolution, integral field observations were obtained on 2010 April 22 under program number 1100147 (PI: Q.A. Parker) with the Wide Field Spectrograph (WiFeS; Dopita et al., 2007; Dopita et al., 2010) mounted on the Australian National University (ANU) 2.3 m telescope at Siding Spring Observatory. CCD chips with pixels are used as detectors. The spectrograph samples 0 along each of twenty five slitlets, which provides a field-of-view of and a spatial resolution element of . Each slitlet is designed to project to 2 pixels on the CCD chips, yielding a reconstructed point-spread function with a full width at half maximum (FWHM) of .
Figure 1 shows the WiFeS areal footprint used for our study. The main shell, the northeast (NE) jet and the southwest (SW) jet are also labeled on the figure. We used the spectral resolution of , covering 4415-5589Å in the blue channel and 5222-7070Å in the red channel. The red spectrum has a linear wavelength dispersion per pixel of Å, which yields a resolution of kms in velocity channels. The exposure time of 20min used for our observation yields a signal-to-noise ratio of S/N for the [NII] emission line. Data reduction was performed with the wifes IRAF package (described by Danehkar et al., 2014; Danehkar et al., 2013).
|(Å)||ID||Mult||Main Shell||NE Jet||SW Jet|
Table 1 presents a full list of observed line fluxes measured from three different apertures shown in Fig.2: the main shell ( ), the NE jet ( ) and the SW jet ( ). The laboratory wavelength, emission line identification and multiplet number are given in columns 1-3, respectively. Columns 4-9 present the observed line fluxes and the dereddened fluxes after correction for interstellar extinction for the three different regions, respectively. All fluxes are given relative to H, on a scale where . To extract the observed line fluxes, we applied a single Gaussian profile to each line. The logarithmic extinction was calculated from the Balmer flux ratio H/H. However, we adopted the extinction (H) derived by Wang & Liu (2007) for the main shell since the H emission line was saturated over the main shell area.