论文标题
搜索很长的I：飞行员Alma 2mm的亮尘星系的随访，作为红移滤波器
Searching Far and Long I: Pilot ALMA 2mm Follow-up of Bright Dusty Galaxies as a Redshift Filter
论文作者
论文摘要
在早期时期的尘土形成星系（DSFG）的完整人口普查是为了限制对宇宙恒星形成速率密度（CSFRD）的模糊贡献（CSFRD），但是$ Z \ sim 4 $以外的DSFG既罕见又很难从与磁质数据相关的光度数据中，因此很难识别出具有用于降低的光度数据，这是由于具有subbillimeter Phototem photemeter photopertry in cumbsillimeter Phototemers in subbillimeter Phototermy phototermy而言。在这里，我们提出了一项试点研究，以获取随访的Atacama大毫米阵列（ALMA）$ 2 \，$ mm观测39 $ 850 \，\rmμm$ $ $ $ MM $ MM-rmμm-bright Dusty Galaxies在SSA22领域中。经验建模建议$ 2 \，以$ 850 \，\rmμm -1 \ $ 850 \，$毫米为单位的样本的$毫米成像，$ mm可以快速，轻松地将“ Haystack in Haystack in Haystack” dsfgs隔离为$ z> 4 $或超越。将档案符号成像与我们测量的ALMA $ 2 \，$ mm的光度法（$1σ\ sim 0.08 \，$ mjy $ \，$ beam $^{ - 1} $ rms）相结合，我们用它们来表征Galaxies的IR seds，并使用它们来约束Redshifts。通过可用的红移约束，通过六个亚毫米频带的组合拟合，我们将每个均可识别6/39高 - $ z $候选者，$> 50 \％$ $坐在$ z> 4 $中，并找到Redshift和$ 2 \ $ 2 \，$ MM FLUX密度之间的正相关。具体而言，我们的模型建议将$ 2 \ $ mm添加到中等约束的IR SED中，将从$ΔZ/（1+Z）= 0.3 $到$ΔZ/（1+Z）= 0.2 $提高毫米衍生的红移的准确性。我们的IR SED特征为样品中相对较高的发射光谱指数（$ \langleβ\ rangle = 2.4 \ pm0.3 $）提供了证据。我们衡量特别明亮（$ s_ {850 \rmμm}> 5.55 \，$ mjy）dsfgs从$ 2 <z <5 $ $ 2 <z <5 $贡献$ \ sim10 $％，从以前的工作中确认了使用类似样品的发现。
A complete census of dusty star-forming galaxies (DSFGs) at early epochs is necessary to constrain the obscured contribution to the cosmic star formation rate density (CSFRD), however DSFGs beyond $z \sim 4$ are both rare and hard to identify from photometric data alone due to degeneracies in submillimeter photometry with redshift. Here, we present a pilot study obtaining follow-up Atacama Large Millimeter Array (ALMA) $2\,$mm observations of a complete sample of 39 $850\,\rmμm$-bright dusty galaxies in the SSA22 field. Empirical modeling suggests $2\,$mm imaging of existing samples of DSFGs selected at $850\,\rmμm - 1\,$mm can quickly and easily isolate the "needle in a haystack" DSFGs that sit at $z>4$ or beyond. Combining archival submillimeter imaging with our measured ALMA $2\,$mm photometry ($1σ\sim 0.08\,$mJy$\,$beam$^{-1}$ rms), we characterize the galaxies' IR SEDs and use them to constrain redshifts. With available redshift constraints fit via the combination of six submillimeter bands, we identify 6/39 high-$z$ candidates each with $>50\%$ likelihood to sit at $z > 4$, and find a positive correlation between redshift and $2\,$mm flux density. Specifically, our models suggest the addition of $2\,$mm to a moderately constrained IR SED will improve the accuracy of a millimeter-derived redshift from $Δz/(1+z) = 0.3$ to $Δz/(1+z) = 0.2$. Our IR SED characterizations provide evidence for relatively high emissivity spectral indices ($\langle β\rangle = 2.4\pm0.3$) in the sample. We measure that especially bright ($S_{850\rmμm}>5.55\,$mJy) DSFGs contribute $\sim10$% to the cosmic-averaged CSFRD from $2<z<5$, confirming findings from previous work with similar samples.
