3 Observational results

Fig.2 presents spatially resolved maps of flux intensity and radial velocity derived from the H$ \alpha $ $ \lambda $6563 emission line for Hen3-1333 and Hen2-113. To extract them, we utilized a Gaussian curve fitting code, which allowed us to fit a single Gaussian profile to the H$ \alpha $ emission line for all spaxels across the IFU field. As seen in Fig.2, the radial velocity maps indicate the presence of outer faint lobes with a diameter of about 10 arcsec extending to the compact structure of $ \sim 3.5$ arcsec diameter (see Fig.1). Contour lines in the figure depict the 2D distribution of the H$ \alpha $ emission obtained from the SuperCOSMOS H$ \alpha $ Sky Survey (Parker et al., 2005), which may aid us in distinguishing the nebular borders. However, the broader point spread function (PSF) of the stellar H$ \alpha $ emission creates diffraction spikes around these PNe, so the contours do not actually show the nebular borders. The IFU flux map presents the resolved nebular H$ \alpha $ emission.

Table 2: LSR systemic velocities and HWHM expansion velocities.
Name $ v_{\rm sys}$(H$ \alpha $) $ V_{\rm HWHM}$(kms$ ^{-1}$)

(kms$ ^{-1}$) H$ \alpha $ [N II] [S II] Mean
Hen3-1333 $ -62.2$ $ 31.6$ $ 37.2$ $ 30.6$ $ 33.1\pm3.3$

$ -56.7$ $ 22.5$ $ 22.3$ $ 20.1$ $ 21.6\pm1.2$

Figure: HST images at two different contrast levels (left-hand and second panels), SHAPE mesh model (third panel), and rendered image (righ-handt panel) of (a) Hen3-1333 and (b) Hen2-113. The mesh models are shown at the best-fitting inclination. The synthetic rendered images have been obtained using a Gaussian blur.
(a) Hen3-1333
(b) Hen2-113

Table 2 lists our velocity results for different emission lines of the integrated spectrum of each PN. Column 2 presents the local standard of rest (LSR) systemic velocity ( $ v_{\rm sys}$) derived from the H$ \alpha $ emission line. Our expansion velocities ( $ v_{\rm exp}$) derived from the half width at half-maximum (HWHM) for H$ \alpha $ $ \lambda $6563, [N II] $ \lambda\lambda$6548,6584 and [S II] $ \lambda\lambda$6716,6731, and average HWHM values are presented in columns 3-6, respectively. Our observations for the H$ \alpha $ emission line give $ V_{\rm HWHM}=31.6$ and $ 22.5$kms$ ^{-1}$ for Hen3-1333 and Hen3-113, in good agreement with $ v_{\rm exp}=30$ and $ 19$kms$ ^{-1}$ derived by De Marco et al. (1997), respectively. For Hen3-113, Gesicki et al. (2006) also derived an expansion velocity of 18kms$ ^{-1}$ and a turbulence velocity of 15kms$ ^{-1}$.

From the HST image of Hen3-1333 displayed in the top panel of Fig.1, several elements can be identified: two pairs of bipolar lobes in the north and south, and some filamentary structures. The HST image of Hen2-113 (shown in the bottom panel of Fig.1), shows two pairs of bipolar lobes in the east and west, and a dark lane between the western border of two opposing lobes. But, the HST images are also obscured by the PSF diffraction spikes, which need to be considered carefully when studying the morphology.

Ashkbiz Danehkar