tokens: PN G233.010.1: ring-like PN. More images can be found in Saurer Weinberger (1987) . PN G236.010.6: object poorly studied, morphology type one-side (see Ali et al. 2000 ) with radial filaments. More images can be found in Hartl Weinberger (1987) . PN G236.701.6: our image shows two areas of lower brightness that are not visible in the H image of the MASH catalogue. PN G239.612.0: round with internal structure and intense patches. More images can be found in Fredrick West (1984) . PN G239.613.9: Balick (1989) classified this PN as elliptical (early-middle subtype). Additional images can be found in Schwarz et al. (1992) . PN G243.837.1: Boffin et al. (2012a) performed a morphological analysis of this PN. PN G247.504.7: there is an HII region towards the SW, and it is unclear whether it is part of the PN or is the optical counterpart of the molecular cloud BRAN 63. PN G249.305.4: ring-like PN with a very faint CSPN. It shows several irregularities in the brightness of the ring. PN G249.807.1: this seems to be two overlapping PN. It is difficult to explain the homogeneous and extensive overdensity of material towards the NW. PN G250.401.3: classical bipolar PN with an arc towards the NW. It is also visible in the [N ii ] images of Kerber et al. (2000) . PN G257.500.6: poorly studied planetary nebula with intriguing morphology. The PN displays a ring-like structure of low surface brightness towards the NE and a emission region towards the SSE that is difficult to explain. It probably is a bipolar PN. This object requires a more detailed study. PN G258.015.7: Gonçalves et al. (2002) show an [N ii ] image, but it is not as deep as ours. In both cases the huge jet-like features are clearly visible. Additional images can be found in Corradi et al. (1996 , 1999) . PN G259.100.9: it is difficult to perform a morphological classification of this Type I PN. A complete analysis of this object was made by Jones et al. (2014) . Our [N ii ] image does not show any differences with the [N ii ]+H published in that article. A H image is presented by Górny et al. (1999) . PN G260.703.3: the H image of MASH catalogue displays a more extended HII region than our image. According to its morphology, it would not be a PN. It could be a filament of the supernova remnant (SNR) Puppis A ( Goudis Meaburn 1978 ). PN G261.603.0: Corradi Schwarz (1995) classify this Type I PN as a possible/probable bipolar. Our [N ii ] image shows a well-defined bipolar morphology with a pronounced waist, thus we confirm this classification. It is not evident from our image if the two saturated regions define the torus of the waist. If this were the case, the waist would not be perpendicular to the bipolar lobes. To answer this question, it is necessary to perform a detailed spectroscopic study. PN G261.908.5: this Type I PN has been classified by Peimbert Torres-Peimbert (1983) as a filamentary bipolar. More images can be found in Vázquez (2012) , Bohigas (2003) and Dufour (1984) . PN
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