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Aims: We investigate how much of the [CII] emission in the nucleus of thenearby spiral galaxy IC 342 is contributed by PDRs and by the ionized gas. Weexamine the spatial variations of starburst/PDR activity and study thecorrelation of the [CII] line with the [NII] 205{\textmu}m emission line comingexclusively from the HII regions. Methods: We present small maps of [CII] and[NII] lines recently observed with the GREAT receiver on board SOFIA. Inparticular we present a super-resolution method to derive how unresolved,kinematically correlated structures in the beam contribute to the observed lineshapes. Results: We find that the emission coming from the ionized gas shows akinematic component in addition to the general Doppler signature of themolecular gas. We interpret this as the signature of two bi-polar lobes ofionized gas expanding out of the galactic plane. We then show how this requiresan adaptation of our understanding of the geometrical structure of the nucleusof IC~342. Examining the starburst activity we find ratios$I([CII])/I(^{12}\mathrm{CO} (1-0))$ between 400 and 1800 in energy units.Applying predictions from numerical models of HII and PDR regions to derive thecontribution from the ionized phase to the total [CII] emission we find that35-90% of the observed [CII] intensity stems from the ionized gas if bothphases contribute. Averaged over the central few hundred parsec we find for the[CII] contribution a HII-to-PDR ratio of 70:30. Conclusions: The ionized gas inthe center of IC 342 contributes more strongly to the overall [CII] emissionthan is commonly observed on larger scales and than is predicted. Kinematicanalysis shows that the majority of the [CII] emission is related to the strongbut embedded star formation in the nuclear molecular ring and only marginallyemitted from the expanding bi-polar lobes of ionized gas.

[CII] 158$\mu$m and [NII] 205$\mu$m emission from IC 342 - Disentangling the emission from ionized and photo-dissociated regions