Chandra survey in the AKARI North Ecliptic Pole Deep Field - I. X-ray data, point-like source catalogue, sensitivity maps, and number counts
Chandra survey in the AKARI North Ecliptic Pole Deep Field - I. X-ray data, point-like source catalogue, sensitivity maps, and number counts
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AKARI 北黄道深场的钱德拉巡天 - I. X 射线数据、点状源目录、灵敏度图和计数
DOI：
10.1093/mnras/stu2010
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发表时间：
2015
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影响因子：
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通讯作者：
T.
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作者：
Krumpe;M.; Miyaji;T.; Brunner;H.; Hanami;H.; Ishigaki;T.; Takagi;T.; Markowitz;A. G.; Goto;T.; Malkan;M. A.; Matsuhara;H.; Pearson;C.; Ueda;Y.; Wada;T.
本文介绍了AKARIN北极深场300 ksq观测的资料产品。该领域有一套独特的九波段红外测光，覆盖AKARI红外相机的2-24 μm，包括Spitzer未覆盖的中红外（MIR）波段。该调查是迄今为止最深的调查之一，深度为1500微米，是迄今为止和平号空间站中具有类似深度的调查中最广泛的。这使得这一领域的唯一的行动星系核的镜像选择atz 101。我们设计了一个源检测程序，它执行联合最大似然PSF（点扩散函数）适合我们所有的15 mosaickedChandrapointings覆盖面积为0.34 deg 2。该过程已被高度优化，并通过模拟测试。我们提供了一个点源目录测光和贝叶斯为基础的90%的置信上限在0.5-7，0.5-2，2-7，2-4，和4-7千电子伏波段。该目录载有457个X射线源，假源比例估计为1.7%。还提供了所有波段的灵敏度和90%置信度通量上限图。我们寻找光学MIR同行在中央0.25 deg 2，深斯巴鲁Suprime-Cam多波段图像存在。在那里检测到的377个X射线源中，80%有光学对应物，60%也有AKARIMIR对应物。我们交叉匹配我们的X射线源与来自Hanami等人的MIR选择的活动星系核。大约30%的活动星系核具有MIR SEDs，完全可以由活动星系核活动来解释，这些活动星系核是强康普顿厚度的活动星系核候选者。
We present data products from the 300 ksChandrasurvey in theAKARINorth Ecliptic Pole Deep Field. This field has a unique set of nine-band infrared photometry covering 2–24 μm from theAKARIInfrared Camera, including mid-infrared (MIR) bands not covered bySpitzer. The survey is one of the deepest ever achieved at ∼15 μm, and is by far the widest among those with similar depths in the MIR. This makes this field unique for the MIR-selection of AGN atz∼ 1. We design a source detection procedure, which performs joint maximum likelihood PSF (point spread function) fits on all of our 15 mosaickedChandrapointings covering an area of 0.34 deg2. The procedure has been highly optimized and tested by simulations. We provide a point source catalogue with photometry and Bayesian-based 90 per cent confidence upper limits in the 0.5–7, 0.5–2, 2–7, 2–4, and 4–7 keV bands. The catalogue contains 457 X-ray sources and the spurious fraction is estimated to be ∼1.7 per cent. Sensitivity and 90 per cent confidence upper flux limits maps in all bands are provided as well. We search for optical–MIR counterparts in the central 0.25 deg2, where deep Subaru Suprime-Cam multiband images exist. Among the 377 X-ray sources detected there, ∼80 per cent have optical counterparts and ∼60 per cent also haveAKARIMIR counterparts. We cross-match our X-ray sources with MIR-selected AGN from Hanami et al. Around 30 per cent of all AGN that have MIR SEDs purely explainable by AGN activity are strong Compton-thick AGN candidates.