We present the results from a large near-infrared spectroscopic survey with Subaru/FMOS (\textit{ FastSound}) consisting of $\sim$ 4,000 galaxies at $z\sim1.4$ with significant H$\alpha$ detection. We measure the gas-phase metallicity from the [N~{ \sc ii}]$\lambda$6583/H$\alpha$ emission line ratio of the composite spectra in various stellar mass and star-formation rate bins. The resulting mass-metallicity relation generally agrees with previous studies obtained in a similar redshift range to that of our sample. No clear dependence of the mass-metallicity relation with star-formation rate is found. Our result at $z\sim1.4$ is roughly in agreement with the fundamental metallicity relation at $z\sim0.1$ with fiber aperture corrected star-formation rate. We detect significant [S~{ \sc ii}]$\lambda\lambda$6716,6731 emission lines from the composite spectra. The electron density estimated from the [S~{ \sc ii}]$\lambda\lambda$6716,6731 line ratio ranges from 10 -- 500 cm$^{ -3}$, which generally agrees with that of local galaxies. On the other hand, the distribution of our sample on [N~{ \sc ii}]$\lambda$6583/H$\alpha$ vs. [S~{ \sc ii}]$\lambda\lambda$6716,6731/H$\alpha$ is different from that found locally. We estimate the nitrogen-to-oxygen abundance ratio (N/O) from the N2S2 index, and find that the N/O in galaxies at $z\sim1.4$ is significantly higher than the local values at a fixed metallicity and stellar mass. The metallicity at $z\sim1.4$ recalculated with this N/O enhancement taken into account decreases by 0.1 -- 0.2 dex. The resulting metallicity is lower than the local fundamental metallicity relation.
Categories: astro-ph.GA