# The SAMI Galaxy Survey: Exploring the gas-phase Mass-Metallicity Relation

## TL;DR

This study uses spatially resolved spectroscopy from the SAMI Galaxy survey to analyze the gas-phase mass-metallicity relation in about 1000 galaxies, confirming previous findings that this relation shows little dependence on star formation rate.

## Contribution

It provides a detailed spatially resolved analysis of the mass-metallicity relation across a large galaxy sample, clarifying the relation's dependence on star formation rate.

## Key findings

- The shape of the MZR is consistent across different calibrators.
- No significant secondary relation between MZR and SFR or sSFR was found.
- Dependence on SFR is weak, confined to low mass or high SFR regimes.

## Abstract

We present a detailed exploration of the stellar mass vs. gas-phase metallicity relation (MZR) using integral field spectroscopy data obtained from ~1000 galaxies observed by the SAMI Galaxy survey. These spatially resolved spectroscopic data allow us to determine the metallicity within the same physical scale (Reff) for different calibrators. The shape of the MZ relations is very similar between the different calibrators, while there are large offsets in the absolute values of the abundances. We confirm our previous results derived using the spatially resolved data provided by the CALIFA and MaNGA surveys: (1) we do not find any significant secondary relation of the MZR with either the star formation rate (SFR) nor the specific SFR (SFR/Mass) for any of the calibrators used in this study, based on the analysis of the {individual} residuals, (2) if there is a dependence with the SFR, it is weaker than the reported one ($r_c\sim -$0.3), it is confined to the low mass regime (M*<10$^9$Msun) or high SFR regimes, and it does not produce any significant improvement in the {description of the average population of galaxies. The aparent disagreement with published results based on single fiber spectroscopic data could be due to (i) the interpretation of the secondary relation itself, (ii) the lower number of objects sampled at the low mass regime by the current study, or (iii) the presence of extreme star-forming galaxies that drive the secondary relation in previous results