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We present a stellar mass-metallicity relation at z~1.4 with anunprecedentedly large sample of ~340 star-forming galaxies obtained with FMOSon the Subaru Telescope. We observed K-band selected galaxies at 1.2 < z_{ph} <1.6 in the SXDS/UDS fields with M_{*} > 10^{9.5} M_{\sun}, and expectedF(H\alpha) > 5 \times 10^{-17} erg s^{-1} cm^{-2}. Among the observed ~1200targets, 343 objects show significant H\alpha emission lines. The gas-phasemetallicity is obtained from [NII]\lambda 6584/H\alpha line ratio, afterexcluding possible active galactic nuclei (AGNs). Due to the faintness of the[NII]\lambda 6584 lines, we apply the stacking analysis and derive themass-metallicity relation at z~1.4. Our results are compared to past results atdifferent redshifts in the literature. The mass-metallicity relation at z~1.4is located between those at z~0.8 and z~2.2; it is found that the metallicityincreases with decreasing redshift from z~3 to z~0 at fixed stellar mass.Thanks to the large size of the sample, we can study the dependence of themass-metallicity relation on various galaxy physical properties. The averagemetallicity from the stacked spectra is close to the local FMR in the highermetallicity part but >0.1 dex higher in metallicity than the FMR in the lowermetallicity part. We find that galaxies with larger E(B-V), B-R, and R-Hcolours tend to show higher metallicity by ~0.05 dex at fixed stellar mass. Wealso find relatively clearer size dependence that objects with smaller halflight radius tend to show higher metallicity by ~0.1 dex at fixed stellar mass,especially in the low mass part.

The mass-metallicity relation at z~1.4 revealed with Subaru/FMOS