The Abundances of Light Neutron-Capture Elements in Planetary Nebulae

Abstract

We present preliminary results from a large-scale survey of the neutron( n )-capture elements Se and Kr in Galactic planetary nebulae (PNe). These elements may be produced in PN progenitors by s -process nucleosynthesis, and brought to the stellar envelope by third dredge-up (TDU). We have searched for [Kr iii] 2.199 and [Se iv] 2.287 $\mu$ m in 120 PNe, and detected one or both lines in 79 objects, for a detection rate of 66%. In order to determine abundances of Se and Kr, we have added these elements to the atomic database of the photoionization code CLOUDY, and constructed a large grid of models to derive corrections for unobserved ionization stages. Se and Kr are enriched in $\sim$ 73% of the PNe in which they have been detected, and exhibit a wide range of abundances, from roughly solar to enriched by a factor of 10 or more. These enrichments are interpreted as evidence for the operation of the s -process and TDU in the progenitor stars. In line with theoretical expectations, Kr is more strongly enhanced than Se, and the abundances of both elements are correlated with the carbon abundance. Kr and Se are strongly enhanced in Type I PNe, which may be evidence for the operation of the $^{22}$ Ne neutron source in intermediate-mass AGB stars. These results constitute the first broad characterization of s -process enrichments in PNe as a population, and reveal the impact of low- and intermediate-mass stars on the chemical evolution of trans-iron elements in the Galaxy.