Neutron-capture element abundances in the planetary nebula NGC 5315 from deep high-resolution optical and near-IR spectrophotometry

TL;DR

This study performs a detailed spectroscopic analysis of planetary nebula NGC 5315, detecting neutron-capture elements and assessing s-process enrichment, revealing no significant enrichment typical for its type.

Contribution

First detailed high-resolution optical and near-IR spectroscopic analysis of NGC 5315 focusing on neutron-capture element abundances and s-process enrichment.

Findings

Detected n-capture elements Kr, Se, possibly Br and Xe.

Found no substantial s-process enrichment in NGC 5315.

Results align with previous studies on the same object.

Abstract

We have done a spectroscopical analysis of the type I planetary nebula (PN) NGC 5315, through high-resolution (R$\sim$40000) optical spectroscopy with UVES at the 8.2m Very Large Telescope, and medium-resolution (R$\sim$4800) near-IR spectroscopy with FIRE at the 6.5m Magellan Baade telescope, covering a wide spectral range from 0.31 $\mu$m to 2.50 $\mu$m. The main aim of this work is to investigate the slow neutron(n)-capture process (the s-process) in the Asymptotic Giant Branch (AGB) star progenitor of a type I PNe. We detected and identified about 700 features, including lines from the n-capture elements Kr, Se, and possibly Br and Xe. We compute physical conditions using line ratios of common ions. Ionic abundances are computed for the species with available atomic data. We calculate total abundances using recent ionization correction factors (ICFs) or by summing ionic abundances. Our results for common elements are in good agreement with previous works on the same object. We do not find a substantial s-process enrichment in NGC 5315, which is typical for type I PNe.