  We present the discovery of extended X-ray emission from the planetary nebula
(PN) NGC 5189 around the [WO1]-type WD 1330-657 with XMM-Newton. The
X-ray-emitting gas fills the cavities detected in the Hubble Space Telescope [O
III] narrow-band image and presents a limb-brightened morphology towards the
outer edges of the east and west lobes. The bulk of the X-ray emission is
detected in the soft (0.3 - 0.7 keV) band with the XMM-Newton EPIC spectra
dominated by the C VI Ly$\alpha$ line at 0.37 keV (=33.7 \AA). Spectral
analysis resulted in carbon and neon abundances 38 and 6 times their solar
values, with a plasma temperature of $kT=0.14\pm0.01$ keV ($T=1.6\times10^{6}$
K) and X-ray luminosity of $L_\mathrm{X}=(2.8\pm0.8)\times10^{32}$ erg
s$^{-1}$. NGC 5189 is an evolved and extended PN ($\lesssim$0.70 pc in radius),
thus, we suggest that the origin of its X-ray emission is consistent with the
born-again scenario in which the central star becomes carbon-rich through an
eruptive very late thermal pulse, subsequently developing a fast, carbon-rich
wind powering the X-ray emission as suggested for A30 and A78.
