论文标题
在z = 3.25处具有强[O III]线的星形星系的物理特性
The Physical Properties of Star-Forming Galaxies with Strong [O III] Lines at z=3.25
论文作者
论文摘要
我们对z = 3.254 $ \ pm $ 0.029的34个[O III]发射线星系（ELG）的物理性质分析进行了分析。这些ELS是从深窄的H2S（1）和383 Arcmin $^{2} $的宽Ks成像中选择的，该$^{2} $用CFHT/WIRCAM获得。我们从U到KS构建光谱能分布（SED），以得出ELG的物理特性。这些[O III] ELG被确定为具有强[O III]线的星形星系，l（[O III]）〜10 $^{42.6} $ -10 $ -10 $^{44.2} $^{44.2} $ erg s $^{ - 1} $ 〜10-210 m $ _ \ odot $ yr $^{ - 1} $的编队率。我们的结果表明，我们的样本星系中有24％是尘土飞扬的，AV> 1 mag和ew（oiii）$ _ {REST} $ 〜70-500 $Å$，通常在光学选择的[O III] ELG样品中错过。他们的休息型紫外线和来自HST/ACS的光学形态和HST/WFC3深成像表明，这些[O III] ELG主要是多组分系统（可能是合并）或紧凑。由于灰尘衰减，其中有20％的紫外线几乎是看不见的。有趣的是，我们发现我们的样品居住在过度密度中，由两个组成部分组成：一个东南（Se），其过度密度因子为$δ_{gal} $ 〜41 $ 〜41，比13 $^{3} $ cmpc $^{3} $ and Northwest（NW）和另一个西北（nw）和$δ_{$δ_{38} $ agal} $^38 abor live a ival} $ cmpc $^{3} $。预计这两个过度密度的子结构将在z = 0处大规模化，总质量为〜1.1 x 10 $^{15} $ m $ _ \ odot $和〜4.8 x 10 $^{14} $ m $ $ _ \ odot $，并且可能合并成一个类似昏迷的星系群。
We present an analysis of physical properties of 34 [O III] emission-line galaxies (ELGs) at z=3.254$\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 $Å$, 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 samples reside in an overdensity consisting of two components: one southeast (SE) with an overdensity factor of $δ_{gal}$ ~ 41 over a volume of 13$^{3}$ cMpc$^{3}$ and the other northwest (NW) with $δ_{gal}$ ~ 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.
