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We present a detailed study of the stellar and orbital parameters of thepost-common envelope binary central star of the planetary nebula Ou~5.Low-resolution spectra obtained during the primary eclipse -- to our knowledgethe first isolated spectra of the companion to a post-common-envelope planetarynebula central star -- were compared to catalogue spectra, indicating that thecompanion star is a late K- or early M-type dwarf. Simultaneous modelling ofmulti-band photometry and time-resolved radial velocity measurements was thenused to independently determine the parameters of both stars as well as theorbital period and inclination. The modelling indicates that the companion staris low mass ($\sim$0.25~M$_\odot$) and has a radius significantly larger thanwould be expected for its mass. Furthermore, the effective temperature andsurface gravity of nebular progenitor, as derived by the modelling, do not lieon single-star post-AGB evolutionary tracks, instead being more consistent witha post-RGB evolution. However, an accurate determination of the componentmasses is challenging. This is principally due to the uncertainty on the locusof the spectral lines generated by the irradiation of the companion'satmosphere by the hot primary (used to derive companion star's radialvelocities), as well as the lack of radial velocities of the primary.

The post-common-envelope binary central star of the planetary nebula Ou 5: a doubly-eclipsing post-red-giant-branch system