大型天文台起源于深度测量--GOODS-South场的VLT/ISAAC近红外成像
The Great Observatories Origins Deep Survey - VLT/ISAAC Near-Infrared Imaging of the GOODS-South Field
摘要：
我们目前的VLT/ISAAC近红外成像调查在GOODS-South领域的最终公开数据发布。这次测量在J、H和Ks波段分别覆盖了172.5、159.6和173.1弧分^[2]的区域。对于点源，在75%的调查区域内达到J=25.0、H=24.5和Ks=24.4（5 σ，AB）的总极限震级。因此，这些观察结果比之前覆盖同一地区的EIS深度公众调查更深入。图像质量的特征在于点扩散函数的范围在0.34弧秒和0.65弧秒之间。在整个视野内，图像以~0.06 arcsec RMS的精度配准。整体光度精度，包括所有系统的影响，加起来0.05马格南。数据是公开的，从欧洲南方天文台科学档案设施。我们定义了KS选择源的目录，其中包含7079个物体的JHK测光。我们简要地讨论了所得的颜色分布的背景下，可用的红移数据。此外，我们估计的完整性分数和相对污染，由于虚假检测源目录从调查数据中提取。相对于以前的深近红外测量，由于这次测量的深度和面积的独特结合，微弱星系的表面密度以前所未有的准确度得到了确定。我们导出了在J=25.25，H=25.0，Ks=25.25（在AB系统中）的流量超过8个星等的星系数计数。在这三个波段中测得的对数斜率在0.24和0.27之间，非常相似。我们没有发现暗端对数星系数的斜率有显著变化的证据。
英文摘要：
We present the final public data release of the VLT/ISAAC near-infrared imaging survey in the GOODS-South field. The survey covers an area of 172.5, 159.6 and 173.1 arcmin^2 in the J, H, and Ks bands, respectively. For point sources total limiting magnitudes of J=25.0, H=24.5, and Ks=24.4 (5 sigma, AB) are reached within 75% of the survey area. Thus these observations are significantly deeper than the previous EIS Deep Public Survey which covers the same region. The image quality is characterized by a point spread function ranging between 0.34 arcsec and 0.65 arcsec FWHM. The images are registered with an accuracy of ~0.06 arcsec RMS over the whole field. The overall photometric accuracy, including all systematic effects, adds up to 0.05 mag. The data are publicly available from the ESO science archive facility. We define a catalog of Ks-selected sources which contains JHKs photometry for 7079 objects. We briefly discuss the resulting color distributions in the context of available redshift data. Furthermore, we estimate the completeness fraction and relative contamination due to spurious detections for source catalogs extracted from the survey data. With respect to previous deep near-infrared surveys, the surface density of faint galaxies has been established with unprecedented accuracy by virtue of the unique combination of depth and area of this survey. We derived galaxy number counts over eight magnitudes in flux up to J=25.25, H=25.0, Ks=25.25 (in the AB system). Very similar faint-end logarithmic slopes between 0.24 and 0.27 per mag were measured in the three bands. We found no evidence for a significant change in the slope of the logarithmic galaxy number counts at the faint end.
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