AzTEC对COSMOS场的毫米测量- III。超过0.72平方米的源目录°的以及由大尺度结构
AzTEC millimeter survey of the COSMOS field - III. Source catalog over 0.72 sq. deg. and plausible boosting by large-scale structure
摘要：
我们提出了一个0.72平方米。°的利用安装在10米阿塔卡马亚毫米望远镜实验（ASTE）上的AzTEC相机在COSMOS场的中心区域进行了1.1mm的连续测量，测量深度为1 sigma ~ 1.26 mJy/束。我们已经发现了189个候选源，信噪比信噪比S/N >= 3.5，其中129个，信噪比>= 4，可以被认为是假的机会很小（<2%）。我们提出了与本次调查得出的数量计数，这表明了显着过剩的来源相比，从~0.5平方米的数量计数。°的在水肺半度河外巡天中在类似深度取样的区域（SHADES，Austermann等人，2010年）。然而，它们与那些被认为太小而不能表征整个空白区域人口的区域相一致。我们确定的差异是更显着的S > 5 mJy制度，并表明，这些过剩的数量计数有关的地区，在红移z < 1.1的星系更密集的集群。在红移区间0.6 < z < 0.75的光学红外星系的位置与1.1mm亮星群（S > 5 mJy）的位置相关性最强，这一结果并不完全取决于调查采样区域内是否存在丰富的星系团。对于在1.1毫米处观测到的数量计数过剩，最可能的解释是中等放大水平的星系-星系和星系群透镜效应，随着样本的流量密度越来越大，振幅也会增加。这种效应在其他高红移族群中也应该可以检测到。
英文摘要：
We present a 0.72 sq. deg. contiguous 1.1mm survey in the central area of the COSMOS field carried out to a 1sigma ~ 1.26 mJy/beam depth with the AzTEC camera mounted on the 10m Atacama Submillimeter Telescope Experiment (ASTE). We have uncovered 189 candidate sources at a signal-to-noise ratio S/N >= 3.5, out of which 129, with S/N >= 4, can be considered to have little chance of being spurious (< 2 per cent). We present the number counts derived with this survey, which show a significant excess of sources when compared to the number counts derived from the ~0.5 sq. deg. area sampled at similar depths in the Scuba HAlf Degree Extragalactic Survey (SHADES, Austermann et al. 2010). They are, however, consistent with those derived from fields that were considered too small to characterize the overall blank-field population. We identify differences to be more significant in the S > 5 mJy regime, and demonstrate that these excesses in number counts are related to the areas where galaxies at redshifts z < 1.1 are more densely clustered. The positions of optical-IR galaxies in the redshift interval 0.6 < z < 0.75 are the ones that show the strongest correlation with the positions of the 1.1mm bright population (S > 5 mJy), a result which does not depend exclusively on the presence of rich clusters within the survey sampled area. The most likely explanation for the observed excess in number counts at 1.1mm is galaxy-galaxy and galaxy-group lensing at moderate amplification levels, that increases in amplitude as one samples larger and larger flux densities. This effect should also be detectable in other high redshift populations.
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