NIR Spectroscopy of Star-Forming Galaxies at <i>z</i> ∼ 1.4 with Subaru/FMOS: The Mass–Metallicity Relation
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- Kiyoto Yabe
- 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-Cho, Sakyo-ku, Kyoto 606-8502 kiyoyabe@kusastro.kyoto-u.ac.jp, ohta@kusastro.kyoto-u.ac.jp
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- Kouji Ohta
- 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-Cho, Sakyo-ku, Kyoto 606-8502 kiyoyabe@kusastro.kyoto-u.ac.jp, ohta@kusastro.kyoto-u.ac.jp
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- Fumihide Iwamuro
- 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-Cho, Sakyo-ku, Kyoto 606-8502 kiyoyabe@kusastro.kyoto-u.ac.jp, ohta@kusastro.kyoto-u.ac.jp
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- Suraphong Yuma
- 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-Cho, Sakyo-ku, Kyoto 606-8502 kiyoyabe@kusastro.kyoto-u.ac.jp, ohta@kusastro.kyoto-u.ac.jp
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- Masayuki Akiyama
- 2Astronomical Institute, Tohoku University, Aoba-ku, Sendai 980-8578
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- Naoyuki Tamura
- 3Subaru Telescope, National Astronomical Observatory of Japan, 650 North A’ohoku Place, Hilo, HI 96720, USA
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- Masahiko Kimura
- 3Subaru Telescope, National Astronomical Observatory of Japan, 650 North A’ohoku Place, Hilo, HI 96720, USA
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- Naruhisa Takato
- 3Subaru Telescope, National Astronomical Observatory of Japan, 650 North A’ohoku Place, Hilo, HI 96720, USA
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- Yuuki Moritani
- 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-Cho, Sakyo-ku, Kyoto 606-8502 kiyoyabe@kusastro.kyoto-u.ac.jp, ohta@kusastro.kyoto-u.ac.jp
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- Masanao Sumiyoshi
- 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-Cho, Sakyo-ku, Kyoto 606-8502 kiyoyabe@kusastro.kyoto-u.ac.jp, ohta@kusastro.kyoto-u.ac.jp
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- Toshinori Maihara
- 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-Cho, Sakyo-ku, Kyoto 606-8502 kiyoyabe@kusastro.kyoto-u.ac.jp, ohta@kusastro.kyoto-u.ac.jp
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- John Silverman
- 4Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Kashiwanoha, Kashiwa, Chiba 277-8583
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- Gavin Dalton
- 5Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
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- Ian Lewis
- 5Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
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- David Bonfield
- 5Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
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- Hanshin Lee
- 5Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
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- Emma Curtis Lake
- 5Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
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- Edward Macaulay
- 5Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
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- Fraser Clarke
- 5Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
説明
<jats:title>Abstract</jats:title> <jats:p>We present near-infrared spectroscopic observations of star-forming galaxies at $z$$\sim $ 1.4 with FMOS on the Subaru Telescope. We observed $K$-band selected galaxies in the SXDS/UDS fields with $K$$\leq$ 23.9 mag, 1.2 $\leq$$z_{\rm ph}$$\leq$ 1.6, $M_{*}$$\geq$ 10$^{9.5}\ M_{\odot}$, and expected F(H$\alpha $) $\geq$ 10$^{-16}\ $erg s$^{-1}\ $cm$^{-2}$; 71 objects in the sample have significant detections of H$\alpha $. For these objects, excluding possible AGNs, identified from the BPT diagram, gas-phase metallicities were obtained from the [N II] / H$\alpha $ line ratio. The sample is split into three stellar-mass bins, and the spectra are stacked in each stellar-mass bin. The mass–metallicity relation obtained at $z$$\sim $ 1.4 is located between those at $z$$\sim $ 0.8 and $z$$\sim $ 2.2. We constrain the intrinsic scatter to be $\sim $ 0.1 dex, or larger in the mass–metallicity relation at $z$$\sim $ 1.4; the scatter may be larger at higher redshifts. We found trends that the deviation from the mass–metallicity relation depends on the SFR (Star-formation rate) and the half light radius: Galaxies with higher SFR and larger half light radii show lower metallicities at a given stellar mass. One possible scenario for the trends is the infall of pristine gas accreted from IGM, or through merger events. Our data points show larger scatter than the fundamental metallicity relation (FMR) at $z$$\sim $ 0.1, and the average metallicities slightly deviate from the FMR. The compilation of the mass–metallicity relations at $z$$\sim $ 3 to $z$$\sim $ 0.1 shows that they evolve smoothly from $z$$\sim $ 3 to $z$$\sim $ 0 without changing the shape so much, except for the massive part at $z$$\sim $ 0.</jats:p>
収録刊行物
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- Publications of the Astronomical Society of Japan
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Publications of the Astronomical Society of Japan 64 (3), 60-, 2012-06-25
Oxford University Press (OUP)
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詳細情報 詳細情報について
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- CRID
- 1362544420787067904
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- ISSN
- 2053051X
- 00046264
- http://id.crossref.org/issn/00046264
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- データソース種別
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- Crossref