Tomoko L. Suzuki, Tadayuki Kodama, Ken Ichi Tadaki, Masao Hayashi, Yusei Koyama, Ichi Tanaka, Yosuke Minowa, Rhythm Shimakawa, Moegi Yamamoto

Research output: Contribution to journalArticlepeer-review

14 Citations (Scopus)


We present the physical properties of [O III] emission line galaxies at z > as the tracers of active galaxies at 1 Gyr before the peak epoch at z ∼ 2. We have performed deep narrowband imaging surveys in the Subaru/XMM-Newton Deep Survey Field with the Multi-object InfraRed Camera and Spectrograph on the Subaru Telescope and have constructed coherent samples of 34 [O III] emitters at z = 3.2 and 3.6, as well as 107 Hα emitters at z = 2.2 and 2.5. We investigate their basic physical quantities, such as stellar masses, star formation rates (SFRs), and sizes, using the publicly available multiwavelength data and high-resolution images from the Hubble Space Telescope. The stellar masses and SFRs show a clear correlation known as the "main sequence" of star-forming galaxies. It is found that the location of the main sequence of the [O III] emitters at z = 3.2 and 3.6 is almost identical to that of the Hα emitters at z = 2.2 and 2.5. Also, we investigate their mass-size relation and find that the relation does not change between the two epochs. When we assume that the star-forming galaxies at z = 3.2 grow simply along the same main sequence down to z = 2.2, galaxies with M∗ = 109-1011 M increase their stellar masses significantly by a factor of 10-2. They climb up the main sequence, and their SFRs also increase a lot as their stellar masses grow. This indicates that star formation activities of galaxies are accelerated from z > toward the peak epoch of galaxy formation at z ∼ 2.

Original languageEnglish
Article number208
JournalAstrophysical Journal
Issue number2
Publication statusPublished - 2015 Jun 20
Externally publishedYes


  • galaxies: evolution
  • galaxies: formation
  • galaxies: high-redshift

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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