ISM EXCITATION AND METALLICITY OF STAR-FORMING GALAXIES AT Z similar or equal to 3.3 FROM NEAR-IR SPECTROSCOPY

作者：Onodera M; Carollo C M; Lilly S; Renzini A; Arimoto N; Capak P; Daddi E; Scoville N; Tacchella S; Tatehora S; Zamorani G

来源：Astrophysical Journal, 2016, 822(1): 42.

DOI：10.3847/0004-637X/822/1/42

• galaxies: evolution
• galaxies: formation
• galaxies: high-redshift
• galaxies: stellar content
• Supporting material: figure set
• machine-readable tables

We study the relationship between stellar mass, star formation rate (SFR), ionization state, and gas-phase metallicity for a sample of 41 normal star-forming galaxies at 3 less than or similar to z less than or similar to 3.7. The gas-phase oxygen abundance, ionization parameter, and electron density of ionized gas are derived from rest-frame optical strong emission lines measured on near-infrared spectra obtained with Keck/Multi-Object Spectrograph for Infra-Red Exploration. We remove the effect of these strong emission lines in the broadband fluxes to compute stellar masses via spectral energy distribution fitting, while the SFR is derived from the dust-corrected ultraviolet luminosity. The ionization parameter is weakly correlated with the specific SFR, but otherwise the ionization parameter and electron density do not correlate with other global galaxy properties such as stellar mass, SFR, and metallicity. The massmetallicity relation (MZR) at z similar or equal to 3.3 shows lower metallicity by similar or equal to 0.7 dex than that at z = 0 at the same stellar mass. Our sample shows an offset by similar or equal to 0.3 dex from the locally defined mass-metallicity-SFR relation, indicating that simply extrapolating such a. relation to higher redshift may predict an incorrect evolution of MZR. Furthermore, within the uncertainties we find no SFR-metallicity correlation, suggesting a less important role of SFR in controlling the metallicity at high redshift. We finally investigate the redshift evolution of the MZR by using the model by Lilly et al., finding that the observed evolution from z = 0 to z similar or equal to 3.3 can be accounted for by the model assuming a weak redshift evolution of the star formation efficiency.

• 出版日期2016-5-1
• 单位中国科学院国家天文台; SAP; 中国地震局