Carbon recombination lines in the Orion Bar

We have carried out VLA D-array observations of the C91 α carbon recombination line as well as Effelsberg 100-m observations of the C65 α line in a 5 ′ square region centered between the Bar and the Trapezium stars in the Orion Nebula with spatial resolutions of 10 ′′ and 40 ′′ , respectively. The results show the ionized carbon in the PDR associated with the Orion Bar to be in a thin, clumpy layer sandwiched between the ionization front and the molecular gas. From the observed line widths we get an upper limit on the temperature in the C + layer of 1500 K and from the line intensity a hydrogen density between 5 × 10 4 and 2 . 5 × 10 5 cm − 3 for a homogeneous medium. The observed carbon level population is not consistent with predictions of hydrogenic recombination theory but could be explained by dielectronic recombination. The layer of ionized carbon seen in C91 α is found to be essentially coincident with emission in the v=1-0 S(1) line of vibrationally excited molecular hydrogen. This is surprising in the light of current PDR models and some possible explanations of the discrepancy are discussed.