S315p.176 — Stellar mass - Metallicity Relation for AKARI-FMOS Infrared Luminous Galaxies at z~0.9

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Aug 4th at 6:00 PM until 6:00 PM

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Author(s): Nagisa Oi1, Hideo Matsuhara1, Tomo Goto3, Chris Pearson4, Véronique Buat2, Matthew A Malkan5

Institution(s): 1. JAXA/ISAS, 2. Laboratoire d'Astrophysique de Marseille, 3. National Tsing Hua University, 4. Rutherford Appleton Laboratory, 5. University of California, Los Angeles

Heavy elements are synthesized in stars and returned into the interstellar medium reflecting the result of the past star formation activity in a galaxy. Thus, the gas phase metallicity is a key parameter in understanding the processes of the formation and the evolution of a galaxy. Many investigations of stellar mass (M*) and gas phase metallicity (Z) relation (MZ relation), which is more massive galaxies tend to be more metal-rich, and a fundamental relation (FMR), whereby galaxies define a tight surface in the three-dimensional space of M*, Z, and Star Formation Rate (SFR) have done up to z~3.3. However, this relation only holds to ultraviolet, optical, or near-infrared selected star forming galaxies. Since most of star formation activities in galaxies at high-z universe are hidden by dust, to fully understand the MZ relation and its evolution, it is critical to study dusty galaxies.

Here, we investigate the MZ relation and FMR for infrared bright galaxies at z~0.9 discovered by AKARI NEP-Deep survey.
We estimated the M* and Z from SED fitting using the AKARI NEP-Deep data with its follow-up multi-wavelength photometric data (from X-ray to FIR) and from Halpha-[NII] emission line ratio taken by Subaru/FMOS, respectively. We found that (1) the infrared bright galaxies at z~0.9 is already chemically evolved to the level of star-forming galaxies in the local universe, and (2) the metallicity of our sample is systematically larger than that of the FMR. The results suggest a possibility that metal was actively created in dusty galaxies up to z~1, then outflow blows out dust and gas, suddenly stopping the chemical evolution and star formation activity, and the galaxies end up being what they are today.