来自卡特琳娜巡天图像的深共加天空
Deep Co-Added Sky from Catalina Sky Survey Images
摘要：
一些天气天空调查正在进行或正在计划中。通常，它们是用小望远镜和相对较短的曝光时间完成的。寻找瞬态或可变源需要与更深的基线图像进行比较，理想情况下，这些图像是通过同一望远镜和照相机获得的。考虑到这一点，我们已经从山上的0.68米施密特望远镜堆叠图像。毕格罗花了十多年的时间作为卡特琳娜巡天的一部分。为了生成Catalina实时瞬变测量的深层参考图像，在8000个字段中使用了近80万张图像，覆盖面积超过27000平方米。°的已经进入了比单个图像深3个数量级的深度堆栈。CRTS系统在成像中不使用滤波器，因此没有标准通带来测量光学量值。我们通过比较这些宽带未滤波的共同添加的图像与$g$ -波段中的图像来估计深度，并发现图像深度范围从22.0- 24.2横跨天空，200个图像堆栈达到22.8的等效AB星等灵敏度。我们比较了各种用于共同添加天文图像的最先进的软件包，并使用SWarp进行堆叠。我们在此描述所采用的程序的细节。这种方法可能是有用的，在其他全景成像应用，以及其他调查。这些叠加的图像可以通过大学间天文学和天体物理学中心（IUCAA）的服务器获得。
英文摘要：
A number of synoptic sky surveys are underway or being planned. Typically they are done with small telescopes and relatively short exposure times. A search for transient or variable sources involves comparison with deeper baseline images, ideally obtained through the same telescope and camera. With that in mind we have stacked images from the 0.68~m Schmidt telescope on Mt. Bigelow taken over ten years as part of the Catalina Sky Survey. In order to generate deep reference images for the Catalina Real-time Transient Survey, close to 0.8 million images over 8000 fields and covering over 27000~sq.~deg. have gone into the deep stack that goes up to 3 magnitudes deeper than individual images. CRTS system does not use a filter in imaging, hence there is no standard passband in which the optical magnitude is measured. We estimate depth by comparing these wide-band unfiltered co-added images with images in the $g$-band and find that the image depth ranges from 22.0--24.2 across the sky, with a 200-image stack attaining an equivalent AB magnitude sensitivity of 22.8. We compared various state-of-the-art software packages for co-adding astronomical images and have used SWarp for the stacking. We describe here the details of the process adopted. This methodology may be useful in other panoramic imaging applications, and to other surveys as well. The stacked images are available through a server at Inter-University Centre for Astronomy and Astrophysics (IUCAA).
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