The stellar emission-line fluxes presented in Table 3, are measured from a spectrum integrated over an aperture ( ) covering the central star in the WiFeS field. The emission line identification, wavelength, dereddened flux corrected for reddening using (H), equivalent width (Å), and FWHM (Å) are given in columns 1-5, respectively. All fluxes are given relative to CIV 5805, on a scale where CIV5805=100. We note that the width of CIV 5805 is narrower than typical Wolf-Rayet central starts of PNe with the same stellar temperature (see e.g Crowther et al., 1998; Acker & Neiner, 2003), so it could be a wels as identified by DePew et al. (2011). Following the method used by Acker & Neiner (2003), a terminal wind velocity of 640kms is deduced from FWHMCIV5805Å. However, we get a terminal velocity of 1560kms from FWHMCIV5805Å reported by DePew et al. (2011). Although the CIII 5696 line is not detected, the CIII/IV 4650 is possibility identified. The HeII 4686 line is fairly strong, but it could have a nebular origin. We see the presence of strong NIII 4634,4641 lines and weak NV 4603,4932 lines. Assuming that the HeII 4686 line is a stellar emission line, M2-42 could have a stellar characteristics similar to WN8-type stars of van der Hucht (2001) based on NIII4641 HeII4686) and NIIINV. However, NII 3995 and NIV 3479-3484, 4058 lines are not in the wavelength coverage of our WiFeS observations, so we cannot certainly classify it as one of nitrogen sequences of Wolf-Rayet central stars of PNe.