通过AzTEC/ASTE - I对GOODS-S场进行1.1 mm波长深度成像。源目录和数量计数
Deep 1.1 mm-wavelength imaging of the GOODS-S field by AzTEC/ASTE - I. Source catalogue and number counts
摘要：
[摘要]我们从ASTE望远镜上的AzTEC拍摄的GOODS-S场的1.1 mm混淆限制图中获得了第一个结果。我们拍摄了一个270平方英尺的。arcmin场的1σ深度为0.48 - 0.73 mJy/束，使这成为有史以来在mm波长下实现的最深空白场调查之一。虽然我们的GOODS-S地图是非常混乱的，我们证明，我们的源识别和数量计数分析是强大的，本文中讨论的技术是相关的其他深深困惑的调查。在这个均匀覆盖的区域内，我们发现了41个S/N >= 3.5的尘埃星暴星系，其中只有两个是错误的检测。我们从这个字段使用“P（d）”分析和半贝叶斯技术，并发现这两种方法给出了一致的结果得出1.1毫米数计数。我们的数据很好地符合Schechter函数模型（S '，N（3 mJy），α）=（1.30+ 0.19mJy，160+27（mJy/deg^2）^（-1），-2.0）。考虑到这次调查的深度，我们在S（1.1mm）= 0.5 mJy时对1.1 mm的数计数进行了第一次严格限制，并且我们发现证据表明，来自各种SCUBA调查的S（850μm）< 2.0 mJy的数计数的模糊端偏向于透镜星系团。与使用LABOCA相机对该区域进行的870 μm调查相比，我们发现与以前在1.1 mm处进行的调查相比，没有明显的源密度不足。此外，我们发现了大量LABOCA目录中未识别的SMG。我们发现，与波长< 500 μm的观测相反，MIPS 24 μm源不能分辨1.1 mm处宇宙红外背景中的总能量密度，这表明在这些较短波长处无法解释的z > 3尘埃遮蔽星系群可能贡献了1.1 mm处红外背景的很大一部分（约2/3）。
英文摘要：
[Abridged] We present the first results from a 1.1 mm confusion-limited map of the GOODS-S field taken with AzTEC on the ASTE telescope. We imaged a 270 sq. arcmin field to a 1σdepth of 0.48 - 0.73 mJy/beam, making this one of the deepest blank-field surveys at mm-wavelengths ever achieved. Although our GOODS-S map is extremely confused, we demonstrate that our source identification and number counts analyses are robust, and the techniques discussed in this paper are relevant for other deeply confused surveys. We find a total of 41 dusty starburst galaxies with S/N >= 3.5 within this uniformly covered region, where only two are expected to be false detections. We derive the 1.1mm number counts from this field using both a "P(d)" analysis and a semi-Bayesian technique, and find that both methods give consistent results. Our data are well-fit by a Schechter function model with (S', N(3mJy), α) = (1.30+0.19 mJy, 160+27 (mJy/deg^2)^(-1), -2.0). Given the depth of this survey, we put the first tight constraints on the 1.1 mm number counts at S(1.1mm) = 0.5 mJy, and we find evidence that the faint-end of the number counts at S(850μm) < 2.0 mJy from various SCUBA surveys towards lensing clusters are biased high. In contrast to the 870 μm survey of this field with the LABOCA camera, we find no apparent under-density of sources compared to previous surveys at 1.1 mm. Additionally, we find a significant number of SMGs not identified in the LABOCA catalogue. We find that in contrast to observations at wavelengths < 500 μm, MIPS 24 μm sources do not resolve the total energy density in the cosmic infrared background at 1.1 mm, demonstrating that a population of z > 3 dust-obscured galaxies that are unaccounted for at these shorter wavelengths potentially contribute to a large fraction (~2/3) of the infrared background at 1.1 mm.
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