English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present the stellar mass ($M_{*}$)--gas-phase metallicity relation (MZR)and its scatter at intermediate redshifts ($0.5\leq z\leq0.7$) for 1381 fieldgalaxies collected from deep spectroscopic surveys. The star formation rate(SFR) and color at a given $M_{*}$ of this magnitude-limited ($R\lesssim24$ AB)sample are representative of normal star-forming galaxies. For masses below$10^9 M_\odot$, our sample of 237 galaxies is $\sim$10 times larger than thosein previous studies beyond the local universe. This huge gain in sample sizeenables superior constraints on the MZR and its scatter in the low-mass regime.We find a power-law MZR at $10^{8} M_\odot < M_{*} < 10^{11} M_\odot$:${12+log(O/H) = (5.83\pm0.19) + (0.30\pm0.02)log(M_{*}/M_\odot)}$. Our MZRshows good agreement with others measured at similar redshifts in theliterature in the intermediate and massive regimes, but is shallower than theextrapolation of the MZRs of others to masses below $10^{9} M_\odot$. The SFRdependence of the MZR in our sample is weaker than that found for localgalaxies (known as the Fundamental Metallicity Relation). Compared to a varietyof theoretical models, the slope of our MZR for low-mass galaxies agrees wellwith predictions incorporating supernova energy-driven winds. Being robustagainst currently uncertain metallicity calibrations, the scatter of the MZRserves as a powerful diagnostic of the stochastic history of gas accretion, gasrecycling, and star formation of low-mass galaxies. Our major result is thatthe scatter of our MZR increases as $M_{*}$ decreases. Our result implies thateither the scatter of the baryonic accretion rate or the scatter of the$M_{*}$--$M_{halo}$ relation increases as $M_{*}$ decreases. Moreover, ourmeasures of scatter at $z=0.7$ appears consistent with that found for localgalaxies.

Stellar Mass--Gas-phase Metallicity Relation at $0.5\leq z\leq0.7$: A Power Law with Increasing Scatter toward the Low-mass Regime