ISO LWS observations of planetary nebula fine-structure lines

We have obtained 43-198 mum far-infrared (IR) spectra for a sample of 51 Ga lactic planetary nebulae (PN) and protoplanetary nebulae (PPN), using the L ong Wavelength Spectrometer (LWS) on board the Infrared Space Observatory ( ISO), Spectra were also obtained of the former PN candidate Lo 14. The spec tra yield fluxes for the fine-structure lines [N II] 122 mum, [N II] 57 mum and [O III] 52 and 88 mum emitted in the ionized regions and the [O I] 63- and 146-mum and [C II] 158-mum lines from the photodissociation regions (P DRs), which have been used to determine electron densities and ionic abunda nces for the ionized regions and densities, temperatures and gas masses for the PDRs. The strong [N III] and [O III] emission lines detected in the LW S spectrum taken centred on Lo 14 could be associated with the nearby stron g radio and infrared source G 331.5-0.1. We find that the electron densities yielded by the [O III] 88 mum/52 mum do ublet ratio are systematically lower than those derived from the optical [A rIV] lambda 4740/lambda 4711 and [Cl III] lambda 5537/lambda 5517 doublet r atios, which have much higher critical densities than the 52- and 88-mum li nes, suggesting the presence of density inhomogeneities in the nebulae. Ion ic abundances, N+/H+, N2+/H+ and O2+/H+, as well as the N2+/O2+ abundance r atio, which provides a good approximation to the N/O elemental abundance ra tio, are derived. Although ionic abundances relative to Hf deduced from the far-IR fine-structure lines are sensitive to the adopted electron density and the presence of density inhomogeneities, the strong dependence on the n ebular physical conditions is largely cancelled out when N2+/O2+ is calcula ted from the 57 mum/(52 mum + 88 mum) flux ratio, owing to the similarity o f the critical densities of the lines involved. The temperatures and densities of the PDRs around 24 PN have been determine d from the observed [O I] and [C II] line intensity ratios. Except for a fe w objects, the deduced temperatures fall between 200 and 500 K, peaking aro und 250 K. The densities of the PDRs vary from 10(4)-10(5) cm(-3), reaching 3 x 10(5) cm(-3) in some young compact PN. With a derived temperature of 1 600K and a density of 10(5) cm(-3), the PDR of NGC 7027 is one of the warme st and at the same time one of the densest amongst the nebulae studied. For most of the PN studied, the [C II]-emitting regions contain only modest am ounts of material, with gas masses less than or equal to0.1 M-circle dot. E xceptional large PDR masses are found for a few nebulae, including NGC 7027 , the bipolar nebulae M2-9 and NGC 6302, the young dense planetary nebulae BD+30 degrees 3639, IC 418 and NGC 5315, and the old, probably recombining, nebulae IC 4406 and NGC 6072.