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The formation of Wolf-Rayet central stars of planetary nebulae ([WR] CSPNe)whose spectroscopic appearance mimics massive WR stars remains poorlyunderstood. Least understood is the nature and frequency of binary companionsto [WR] CSPNe that may explain their H-deficiency. We have conducted asystematic radial velocity (RV) study of 6 [WR] CSPNe to search forpost-common-envelope (post-CE) [WR] binaries. We used a cross-correlationmethod to construct the RV time-series as successfully done for massive closebinary WR stars. No significant RV variability was detected for the late-[WC]type nuclei of Hen 2-113, Hen 3-1333, PMR 2 and Hen 2-99. Significant,large-amplitude variability was found in the [WC4] nucleus of NGC 5315. In the[WO1] nucleus of NGC 5189 we discovered significant periodic variability thatreveals a close binary with $P_\mathrm{orb}=4.04\pm0.1$ d. We measured asemi-amplitude of $62.3\pm1.3$ km s$^{-1}$ that gives a companion mass of$m_2\ge0.5$ $M_\odot$ or $m_2=0.84$ $M_\odot$ (assuming $i=45^\circ$). The mostplausible companion type is a massive WD as found in Fleming 1. The spectacularnebular morphology of NGC 5189 fits the pattern of recently discovered post-CEPNe extremely well with its dominant low-ionisation structures (e.g. as in NGC6326) and collimated outflows (e.g. as in Fleming 1). The anomalously long 4.04d orbital period is either a once-off (e.g. NGC 2346) or it may indicate thereis a sizeable population of [WR] binaries with massive WD companions inrelatively wide orbits, perhaps influenced by interactions with the strong [WR]wind.

monthly notices of the royal astronomical society

A radial velocity survey for post-common-envelope Wolf-Rayet central  stars of planetary nebulae: First results and discovery of the close binary  nucleus of NGC 5189