# Far-infrared metallicity diagnostics: Application to local ultraluminous infrared galaxies

## TL;DR

This paper develops and tests far-infrared line ratio diagnostics for measuring galaxy metallicities, especially useful for high-redshift objects obscured by dust, and applies them to local ULIRGs.

## Contribution

It introduces new far-IR metallicity diagnostics based on CLOUDY modeling and validates them on local ULIRGs, expanding tools for dust-obscured galaxy studies.

## Key findings

- Far-IR line ratios reliably measure metallicity in dusty galaxies.
- The [OIII]52μm/[NIII]57μm ratio is robust against AGN presence.
- Local ULIRGs have sub-solar to solar metallicities, below the mass-metallicity relation.

## Abstract

The abundance of metals in galaxies is a key parameter which permits to distinguish between different galaxy formation and evolution models. Most of the metallicity determinations are based on optical line ratios. However, the optical spectral range is subject to dust extinction and, for high-z objects (z > 3), some of the lines used in optical metallicity diagnostics are shifted to wavelengths not accessible to ground based observatories. For this reason, we explore metallicity diagnostics using far-infrared (IR) line ratios which can provide a suitable alternative in such situations. To investigate these far-IR line ratios, we modeled the emission of a starburst with the photoionization code CLOUDY. The most sensitive far-IR ratios to measure metallicities are the [OIII]52$\mu$m and 88$\mu$m to [NIII]57$\mu$m ratios. We show that this ratio produces robust metallicities in the presence of an AGN and is insensitive to changes in the age of the ionizing stellar. Another metallicity sensitive ratio is the [OIII]88$\mu$m/[NII]122$\mu$m ratio, although it depends on the ionization parameter. We propose various mid- and far-IR line ratios to break this dependency. Finally, we apply these far-IR diagnostics to a sample of 19 local ultraluminous IR galaxies (ULIRGs) observed with Herschel and Spitzer. We find that the gas-phase metallicity in these local ULIRGs is in the range 0.7 < Z_gas/Z_sun < 1.5, which corresponds to 8.5 < 12 + log (O/H) < 8.9. The inferred metallicities agree well with previous estimates for local ULIRGs and this confirms that they lie below the local mass-metallicity relation.