Physical Conditions and Chemical Abundances of the Variable Planetary Nebula IC 4997

TL;DR

This study investigates the physical conditions and chemical abundances of the variable planetary nebula IC 4997, revealing high abundance discrepancy factors and contrasting metallicity indicators from different spectral lines.

Contribution

It provides detailed measurements of electron densities, temperatures, and chemical abundances using CELs and ORLs, highlighting the large abundance discrepancy factors in IC 4997.

Findings

Electron densities > 3 x 10^4 cm^-3

Electron temperatures > 14,000 K from CELs

Large abundance discrepancy factors (ADFs) > 7

Abstract

The planetary nebula (PN) IC 4997 is one of a few rapidly evolving objects with variable brightness and nebular emission around a hydrogen-deficient star. In this study, we have determined the physical conditions and chemical abundances of this object using the collisionally excited lines (CELs) and optical recombination lines (ORLs) measured from the medium-resolution spectra taken in July 2014 with the FIbre-fed \'Echelle Spectrograph on the Nordic Optical Telescope at La Palma Observatory. We derived electron densities of $\gtrsim 3 \times 10^4$ cm$^{-3}$ and electron temperatures of $\gtrsim 14,000$ K from CELs, whereas cooler temperatures of $\sim 11,000$ and $\sim 7,000$ K were obtained from helium and heavy element ORLs, respectively. The elemental abundances deduced from CELs point to a metal-poor progenitor with [O/H]$\lesssim-0.75$, whereas the ORL abundances are slightly above the solar metallicity, [O/H]$\approx 0.15$. Our abundance analysis indicates that the abundance discrepancy factors (ADFs$\equiv$ORLs/CELs) of this PN are relatively large: ADF(O$^{2+})\gtrsim 8$ and ADF(N$^{2+})\gtrsim 7$. Further research is needed to find out how the ADFs and variable emissions are formed in this object and whether they are associated with a binary companion or a very late thermal pulse.