• DOI:10.3847/1538-4357/ac7392
• Corpus ID: 249097417

The Physical Properties of Star-forming Galaxies with Strong [O iii] Lines at z = 3.25

@article{Wen2022ThePP,
  title={The Physical Properties of Star-forming Galaxies with Strong [O iii] Lines at z = 3.25},
  author={Run Wen and Fangxia An and Xianzhong Zheng and Dongdong Shi and Jianbo Qin and Valentino Gonzalez and Fuyan Bian and Haiguang Xu and Zhizheng Pan and Qinghua Tan and Wenhao Liu and Min Fang and Jian Ren and Yu Heng Zhang and Man Qiao and Shuang Liu},
  journal={The Astrophysical Journal},
  year={2022},
  volume={933}
}

• Run Wen, F. An, +13 authors Shuang Liu
• Published 26 May 2022
• Physics
• The Astrophysical Journal

We present an analysis of physical properties of 34 [O iii] emission-line galaxies (ELGs) at z = 3.254 ± 0.029 in the Extended Chandra Deep Field South (ECDFS). These ELGs are selected from deep narrow H2S(1) and broad K s imaging of 383 arcmin2 obtained with CFHT/WIRCam. We construct spectral energy distributions (SEDs) from U to K s to derive the physical properties of ELGs. These [O iii] ELGs are identified as starburst galaxies with strong [O iii] lines of L OIII ∼ 1042.6–1044.2 erg s−1 and have stellar masses of M * ∼ 109.0–1010.6 M ⊙ and star formation rates of ∼10–210 M ⊙ yr−1. Our results show that 24% of our sample galaxies are dusty with A V > 1 mag and EW([O iii])rest ∼ 70–500 Å, which are often missed in optically selected [O iii] ELG samples. Their rest-frame UV and optical morphologies from HST/ACS and HST/WFC3 deep imaging reveal that these [O iii] ELGs are mostly multiple-component systems (likely mergers) or compact. And 20% of them are nearly invisible in the rest-frame UV owing to heavy dust attenuation. Interestingly, we find that our sample ELGs reside in an overdensity consisting of two components: one southeast (SE) with an overdensity factor of δ gal ∼ 41 over a volume of 133 cMpc3, and the other northwest (NW) with δ gal ∼ 38 over a volume of 103 cMpc3. The two overdense substructures are expected to be virialized at z = 0 with a total mass of ∼ 1.1 × 1015 M ⊙ and ∼ 4.8 × 1014 M ⊙ and probably merge into a Coma-like galaxy cluster.