# Identification of Near-Infrared [Se III] and [Kr VI] Emission Lines in Planetary Nebulae

## TL;DR

This study detects specific near-infrared emission lines of selenium and krypton in planetary nebulae, enabling improved methods for determining their elemental abundances and testing ionization correction models.

## Contribution

It reports the first detection of [Se III] 1.0994 micron and provides new collision strength calculations and ionization correction factors for Se and Kr in planetary nebulae.

## Key findings

- Detection of [Se III] and [Kr VI] lines in planetary nebulae.
- New collision strengths for Se^{2+} and Kr^{5+}.
- Refined ionization correction factors for Se and Kr abundances.

## Abstract

We identify [Se III] 1.0994 micron in the planetary nebula (PN) NGC 5315 and [Kr VI] 1.2330 micron in three PNe, from spectra obtained with the FIRE spectrometer on the 6.5-m Baade Telescope. Se and Kr are the two most widely-detected neutron-capture elements in astrophysical nebulae, and can be enriched by s-process nucleosynthesis in PN progenitor stars. The detection of [Se III] 1.0994 micron is particularly valuable when paired with observations of [Se IV] 2.2858 micron, as it can be used to improve the accuracy of nebular Se abundance determinations, and allows Se ionization correction factor (ICF) schemes to be empirically tested for the first time. We present new effective collision strength calculations for Se^{2+} and Kr^{5+}, which we use to compute ionic abundances. In NGC 5315, we find that the Se abundance computed from Se^{3+}/H^+ is lower than that determined with ICFs that incorporate Se^{2+}/H^+. We compute new Kr ICFs that take Kr^{5+}/H^+ into account, by fitting correlations found in grids of Cloudy models between Kr ionic fractions and those of more abundant elements, and use these to derive Kr abundances in four PNe. Observations of [Se III] and [Kr VI] in a larger sample of PNe, with a range of excitation levels, are needed to rigorously test the ICF prescriptions for Se and our new Kr ICFs.