# Present-day mass-metallicity relation for galaxies using a new electron-temperature method

## TL;DR

This paper introduces a new electron-temperature method for accurately measuring gas-phase metallicity in local galaxies, improving the mass-metallicity relation by correcting biases in previous Te-based calibrations.

## Contribution

The paper develops a novel Te(OIII)-Te(OII) calibration that accounts for low-ionisation systems, enabling more precise metallicity estimates across diverse galaxy types.

## Key findings

- New Te calibration reduces metallicity underestimation in low-ionisation systems.
- Empirical correction improves accuracy of metallicity measurements for various galaxy sizes.
- Resulting mass-metallicity relation aligns well with independent measurement methods.

## Abstract

We investigate electron temperature (Te) and gas-phase oxygen abundance (Z_Te) measurements for galaxies in the local Universe (z < 0.25). Our sample comprises spectra from a total of 264 emission-line systems, ranging from individual HII regions to whole galaxies, including 23 composite HII regions from "star-forming main sequence" galaxies in the MaNGA survey. We utilise 130 of these systems with directly measurable Te(OII) to calibrate a new metallicity-dependent Te(OIII) - Te(OII) relation that provides a better representation of our varied dataset than existing relations from the literature. We also provide an alternative Te(OIII) - Te(NII) calibration. This new Te method is then used to obtain accurate Z_Te estimates and form the mass - metallicity relation (MZR) for a sample of 118 local galaxies. We find that all the Te(OIII) - Te(OII) relations considered here systematically under-estimate Z_Te for low-ionisation systems by up to 0.6 dex. We determine that this is due to such systems having an intrinsically higher O+ abundance than O++ abundance, rendering Z_Te estimates based only on [OIII] lines inaccurate. We therefore provide an empirical correction based on strong emission lines to account for this bias when using our new Te(OIII) - Te(OII) and Te(OIII) - Te(NII) relations. This allows for accurate metallicities (1sigma = 0.08 dex) to be derived for any low-redshift system with an [OIII]4363 detection, regardless of its physical size or ionisation state. The MZR formed from our dataset is in very good agreement with those formed from direct measurements of metal recombination lines and blue supergiant absorption lines, in contrast to most other Te-based and strong-line-based MZRs. Our new Te method therefore provides an accurate and precise way of obtaining Z_Te for a large and diverse range of star-forming systems in the local Universe.