2006MNRAS.368.1959L

We present high-quality optical spectroscopic observations of the planetary nebula (PN) Hf2-2. The spectrum exhibits many prominent optical recombination lines (ORLs) from heavy-element ions. Analysis of the Hi and Hei recombination spectrum yields an electron temperature of ∼900 K, a factor of 10 lower than given by the collisionally excited [Oiii] forbidden lines. The ionic abundances of heavy elements relative to hydrogen derived from ORLs are about a factor of 70 higher than those deduced from collisionally excited lines (CELs) from the same ions, the largest abundance discrepancy factor (adf) ever measured for a PN. By comparing the observed Oiiλ4089/λ4649 ORL ratio to theoretical value as a function of electron temperature, we show that the Oii ORLs arise from ionized regions with an electron temperature of only ∼630 K. The current observations thus provide the strongest evidence that the nebula contains another previously unknown component of cold, high-metallicity gas, which is too cool to excite any significant optical or ultraviolet CELs and is thus invisible via such lines. The existence of such a plasma component in PNe provides a natural solution to the long-standing dichotomy between nebular plasma diagnostics and abundance determinations using CELs on the one hand and ORLs on the other.