Chandra Deep Field South: The 1Msec Catalog
Chandra Deep Field South: The 1Msec Catalog
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钱德拉深场南：1Msec 目录
DOI：
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发表时间：
2001
期刊：
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通讯作者：
C. Norman
中科院分区：
文献类型：
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作者：
R. Giacconi;A. Zirm;J. Wang;P. Rosati;M. Nonino;P. Tozzi;R. Gilli;V. Mainieri;G. Hasinger;L. Kewley;J. Bergeron;S. Borgani;R. Gilmozzi;N. Grogin;A. Koekemoer;E. Schreier;W. Zheng;C. Norman
在这篇文章中，我们介绍了钱德拉深场南方(CDFS)942K曝光的源星表，它是利用钱德拉X射线天文台上的ACIS-I获得的。星表的生成使用两种不同的方法同时进行；一种是我们自己设计的方法，使用的是SExtractor算法的修改版本；另一种是专门为Chandra观测开发的小波变换技术。通过广泛的模拟评估，已经设置了检测阈值，以便具有少于10个杂乱源。我们把目录细分为四个部分。主列表由两种检测方法共有的对象组成。两个次要列表包含由以下两种方法检测到的源：1)单独的SExtractor算法和2)单独的小波技术。第四个列表包括可能的扩散源或扩展源。软带(0.5-2keV)和硬带(2-10keV)的瞄准点处的磁通极限分别为5.5E-17erg/S/cm^2和4.5E-16erg/S/cm^2。总共有346个源，其中在0.5-2keV波段探测到307个，在2-10keV波段探测到251个。
我们还提供了编目来源的光学标识。我们的主要光学数据是R波段成像，深度为R~26.5(织女星)。我们发现R波段/钱德拉偏移量很小，~1角秒。坐标互相关法发现，R中覆盖的85%的Chandra信号源的对应值在3-sigma误差框内(约1.5角秒，具体取决于离轴角度和信噪比)。未确定的源比例约为10-15%，接近已确定样品的观测X射线通量与R波段比率分布的预期极限。
In this Paper we present the source catalog obtained from a 942 ks exposure of the Chandra Deep Field South (CDFS), using ACIS-I on the Chandra X-ray Observatory. Catalog generation proceeded simultaneously using two different methods; a method of our own design using a modified version of the SExtractor algorithm, and a wavelet transform technique developed specifically for Chandra observations. The detection threshold has been set in order to have less than 10 spurious sources, as assessed by extensive simulations. We subdivided the catalog into four sections. The primary list consists of objects common to the two detection methods. Two secondary lists contain sources which were detected by: 1) the SExtractor algorithm alone and 2) the wavelet technique alone. The fourth list consists of possible diffuse or extended sources. The flux limits at the aimpoint for the soft (0.5--2 keV) and hard (2--10 keV) bands are 5.5E-17 erg/s/cm^2 and 4.5E-16 erg/s/cm^2 respectively. The total number of sources is 346; out of them, 307 were detected in the 0.5--2 keV band, and 251 in the 2--10 keV band.
We also present optical identifications for the catalogued sources. Our primary optical data is R band imaging to a depth of R~26.5 (Vega). We found that the R-band/Chandra offsets are small, ~1 arcsec. Coordinate cross-correlation finds 85% of the Chandra sources covered in R to have counterparts within the 3-sigma error box (>~1.5 arcsec depending on off-axis angle and signal-to-noise). The unidentified fraction of sources, approximately ~10--15 %, is close to the limit expected from the observed X-ray flux to R-band ratio distribution for the identified sample.