论文标题
商品 - alma：光学深色的阿尔玛星系在z = 3.5的地层簇上露出灯光
GOODS-ALMA: Optically dark ALMA galaxies shed light on a cluster in formation at z = 3.5
论文作者
论文摘要
在本文中，我们研究了在69 Arcmin^2 Alma 1.1mm连续调查中检测到的六个光学深色星系的性能。尽管它们都没有被列入最深的H频段烛台目录，但在商品南部的目录至H = 28.16ab，但我们能够将其中的两个从其明亮的邻居中解脱出来，并为他们测量$ h $ band Flux。我们注意到，AGS4和AGS15的H = 25.23，27.11AB。它们与明亮的光源的极端接近（0.50“，0.27”）及其极度晕厥使它们无法将其包含在H波段目录中。我们介绍了六个源中五个源的光谱扫描随访，其中五个源具有ALMA带4。在2mm连续体中都检测到，信噪比高于8。在AGS4（ν_{obs} = 151.44GHz中检测到一条发射线，s/n = 8.58）和ags17（ν_{obs} = 154.78GHz，s/n = 10.23），在这两种情况下，我们在z^{ags ags ags 4}} = 3.5} = 3.3} = 3.5} = 3.5} = 3.5中解释了这两种情况。 z^{ags4} _ {spec} = 3.467。这些红移既符合从紫外线到近红外光谱能量分布（SED）的光度红移的概率分布，又与这些红移处星系中典型的尘埃温度的远红外SED相匹配。我们提供的证据表明，光学深色星系的近70％（4/6星系）属于Z〜3.5处的星系过高密度。过度密度最大的是AGS24（M _ {\ Star} = 10^{11.32^{+0.02} _ { - 0.19}} M _ {\ odot}），是$ z $ z $ z $ \ \ fiff incam $ z $ \ \ \ field find，是$ z $ \ \ \ \ field，> \ field，> field，> \ \ \ \ \ fiend-它落在星系表面密度的峰值的中心，这表明周围的过度密度是病毒化过程中的原始群集，而AGS24是未来最亮的星系（BCG）的候选祖先。
In this paper we study the properties of the six optically dark galaxies detected in the 69 arcmin^2 GOODS-ALMA 1.1mm continuum survey. While none of them are listed in the deepest H-band based CANDELS catalog in the GOODS-South field down to H=28.16AB, we were able to de-blend two of them from their bright neighbor and measure an $H$-band flux for them. We note that AGS4 and AGS15 have H=25.23, 27.11AB respectively. Their extreme proximity (0.50", 0.27") to a bright optical source and their extreme faintness prevented them from being included in the H-band catalog. We present the spectroscopic scan follow-up of five of the six sources with ALMA band 4. All are detected in the 2mm continuum with signal-to-noise ratios higher than eight. One emission line is detected in AGS4 (ν_{obs} =151.44GHz with a S/N=8.58) and AGS17 (ν_{obs} =154.78GHz with a S/N=10.23), which we interpret in both cases as being due to the CO(6-5) line at z^{AGS4}_{spec}=3.556 and z^{AGS4}_{spec}=3.467, respectively. These redshifts match both the probability distribution of the photometric redshifts derived from the UV to near-infrared spectral energy distributions (SEDs) and the far-infrared SEDs for typical dust temperatures of galaxies at these redshifts. We present evidence that nearly 70% (4/6 of galaxies) of the optically dark galaxies belong to the same overdensity of galaxies at z~3.5. overdensity The most massive one, AGS24 (M_{\star} = 10^{11.32^{+0.02}_{-0.19}} M_{\odot}), is the most massive galaxy without an active galactic nucleus (AGN) at $z$\,>\,3 in the GOODS-ALMA field. It falls in the very center of the peak of the galaxy surface density, which suggests that the surrounding overdensity is a proto-cluster in the process of virialization and that AGS24 is the candidate progenitor of the future brightest cluster galaxy (BCG).
