A Critical Look at the Mass-Metallicity-SFR Relation in the Local Universe. I. An Improved Analysis Framework and Confounding Systematics

TL;DR

This paper develops a new analysis framework to clarify the debated dependence of galaxy metallicity on star formation rate, revealing a weak or absent relation for massive galaxies and a more complex behavior for others.

Contribution

It introduces a non-parametric, astrophysically motivated method to analyze the local M-Z-SFR relation and assesses the impact of sample selection and measurement indicators.

Findings

Metallicity is anti-correlated with specific SFR across indicators.

No spurious relation due to measurement biases or aperture effects.

Dependence is stronger in high SSFR galaxies above the star-forming sequence.

Abstract

It has been proposed that the mass-metallicity relation of galaxies exhibits a secondary dependence on star formation rate (SFR), and that the resulting M-Z-SFR relation may be redshift-invariant, i.e., "fundamental." However, conflicting results on the character of the SFR dependence, and whether it exists, have been reported. To gain insight into the origins of the conflicting results, we (a) devise a non-parametric, astrophysically motivated analysis framework based on the offset from the star-forming ("main") sequence at a given stellar mass (relative specific SFR), (b) apply this methodology and perform a comprehensive re-analysis of the local M-Z-SFR relation, based on SDSS, GALEX, and WISE data, and (c) study the impact of sample selection, and of using different metallicity and SFR indicators. We show that metallicity is anti-correlated with specific SFR regardless of the indicators used. We do not find that the relation is spurious due to correlations arising from biased metallicity measurements, or fiber aperture effects. We emphasize that the dependence is weak/absent for massive galaxies ($\log M_*>10.5$), and that the overall scatter in the M-Z-SFR relation does not greatly decrease from the M-Z relation. We find that the dependence is stronger for the highest SSFR galaxies above the star-forming sequence. This two-mode behavior can be described with a broken linear fit in 12+log(O/H) vs. log (SFR$/M_*$), at a given $M_*$. Previous parameterizations used for comparative analysis with higher redshift samples that do not account for the more detailed behavior of the local M-Z-SFR relation may incorrectly lead to the conclusion that those samples follow a different relationship.