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

Abstract

We present an analysis of physical properties of 34 [O III] emission-line galaxies (ELGs) at z=3.254$\pm$0.029 in the Extended Chandra Deep Field South (ECDFS). These ELGs are selected from deep narrow H2S(1) and broad Ks imaging of 383 arcmin${}^2$ obtained with CFHT/WIRCam. We construct spectral energy distributions (SEDs) from U to Ks to derive the physical properties of ELGs. These [O III] ELGs are identified as starburst galaxies with strong [O III] lines of L([O III]) ~ 10${}^{42.6}$ - 10${}^{44.2}$ erg s${}^{-1}$, and have stellar masses of M* ~ 10${}^{9.0}$-10${}^{10.6}$ M${}_{\odot }$ and star formation rates of ~ 10-210 M${}_{\odot }$ yr${}^{-1}$. Our results show that 24% of our sample galaxies are dusty with Av > 1 mag and EW(OIII)${}_{rest}$ ~ 70-500 $\mathring{A}$, 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 samples reside in an overdensity consisting of two components: one southeast (SE) with an overdensity factor of ${\delta }_{gal}$ ~ 41 over a volume of 13${}^3$ cMpc${}^3$ and the other northwest (NW) with ${\delta }_{gal}$ ~ 38 over a volume of 10${}^3$ cMpc${}^3$. The two overdense substructures are expected to be virialized at z=0 with a total mass of ~ 1.1 x 10${}^{15}$ M${}_{\odot }$ and ~ 4.8 x 10${}^{14}$ M${}_{\odot }$, and probably merge into a Coma-like galaxy cluster.

arXiv comment22 pages, 11 figures, 3 tables. Accepted for publication in ApJ

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