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We present a detailed analysis of IC 4776, a planetary nebula displaying amorphology believed to be typical of central star binarity. The nebula is shownto comprise a compact hourglass-shaped central region and a pair of precessingjet-like structures. Time-resolved spectroscopy of its central star revealsperiodic radial velocity variability consistent with a binary system. While thedata are insufficient to accurately determine the parameters of the binary, themost likely solutions indicate that the secondary is probably a low-mass mainsequence star. An empirical analysis of the chemical abundances in IC 4776indicates that the common-envelope phase may have cut short the AGB evolutionof the progenitor. Abundances calculated from recombination lines are found tobe discrepant by a factor of approximately two relative to those calculatedusing collisionally excited lines, suggesting a possible correlation betweenlow abundance discrepancy factors and intermediate-period post-common-envelopecentral stars and/or Wolf-Rayet central stars. The detection of a radialvelocity variability associated with binarity in the central star of IC 4776may be indicative of a significant population of (intermediate-period)post-common-envelope binary central stars which would be undetected by classicphotometric monitoring techniques.

The planetary nebula IC 4776 and its post-common-envelope binary central star