Aq Psc – Analysis of New Light Curves

New BV light curves of the A-type W UMa star AQ Psc (P = 0.476d) have been observed and are described. A few times of minimum light are obtained and the ephemeris is improved. The light curves are analyzed for the binary parameters with a light curve synthesis method. Combining the results with Lu and Rucinski’s spectroscopic mass ratio we determined the masses and radii of the components: M ₁ = 1.69M _⊙, M ₂ = 0.38M _⊙, R ₁ = 1.77R _⊙, and R ₂ = 0.89R _⊙.     

Giga-Pixels and Sky Surveys

We describe a project to build a new type of astronomical CCD that should significantly decrease the cost per pixel of detectors. This device should also provide very fast readout, autoguiding capability, image motion compensation, and good red sensitivity. This revised version was published online in July 2006 with corrections to the Cover Date.     

SciMeasure Wavefront Sensor Cameras and their Application in the Palomar Adaptive Optics System

SciMeasure, in collaboration with Emory University and the Jet Propulsion Laboratory, has developed a very versatile CCD controller for use in adaptive optics, optical interferometry, and other applications requiring high-speed readout rates and/or low read noise. The overall architecture of this controller system will be discussed and its performance using both EEV CCD39 and MIT/LL CCID-19 detectors will be presented. This controller is used in the adaptive optics system, developed by JPL, for the 200′′ Hale telescope at Palomar Mountain. Early diffraction-limited science results, recently achieved by the AO system, are presented. We gratefully acknowledge the financial support of NASA through SBIR contracts NAS8–97195 and NAS8–98081. This revised version was published online in July 2006 with corrections to the Cover Date.     

Cosmic rays and other nonsense in astronomical CCD imagers

Cosmic-ray muons make recognizable straight tracks in the new-generation CCD's with thick sensitive regions. Wandering tracks (‘worms’), which we identify with multiply-scattered low-energy electrons, are readily recognized as different from the muon tracks. These appear to be mostly recoils from Compton-scattered gamma rays, although worms are also produced directly by beta emitters in dewar windows and field lenses. The gamma rays are mostly byproducts of ⁴⁰K decay and the U and Th decay chains. Trace amounts of these elements are nearly always present in concrete and other materials. The direct betas can be eliminated and the Compton recoils can be reduced significantly by the judicious choice of materials and shielding. The cosmic-ray muon rate is irreducible. Our conclusions are supported by tests at the Lawrence Berkeley National Laboratory low-level counting facilities in Berkeley and 180 m underground at Oroville, California. This revised version was published online in July 2006 with corrections to the Cover Date.     

土星卫星CCD定位观测的初步分析

发表了１９９４年８月土星主要卫星ＣＣＤ观测的相对位置资料及其与理论值的比较分析。观测使用了开放实验室分山基地的１５６ｃｍ天体测量望远镜上的ＣＣＤ探测器．对观测资料的分析表明；Ｒｈｅａ和Ｄｉｏｎｅ相对于Ｔｉｔａｎ的位置精度为０．１２”。这相当于距离土星７００ｋｍ．土星卫星ＣＣＤ观测与最佳的照相观测比较，其位置精度相当。     

基于USB30.0的EMCCD相机高速数据传输系统韵研究

自动成像协会（AutomatedImagingAssociation,AIA）在2013年初发布了用于高速图像数据传输的USB3Vision标准。首先简要介绍了基于该标准的EMCCD相机高速数据传输系统的设计方案,重点介绍了传输系统的构建和图像采集软件的设计。其中,传输系统的构建主要是在QUARTUSII的开发环境下,移植EMCCD相机数字控制器,使用VHDL语言编程设计一个控制器,产生USB3．0芯片USB3014的读写时序以及相关的逻辑信号,并且完成模拟图像产生和针对USB3Vision标准的数据传输格式转换的功能;图像采集软件的编写是在VS2010开发环境下利用CYPRESS公司提供的应用程序接151（API）,采用c＋＋语言实现。最后进行了模拟图像的采集实验,并且进行了误码率估算。     

RTS2中新CCD类型扩展方法

CCD是天文望远镜中最常见的观测终端设备,也是望远镜自主控制系统中的重要组成部分。随着天文望远镜自主观测需求的不断出现以及技术的快速发展,开源的RTS2软件系统成为目前该领域研究中受到较多关注的系统之一。但RTS2支持的CCD设备较为有限,同时控制接口约定也相对固定。在针对部分特殊的CCD设备(如LAMOST中采用的32台CCD设备、选址用的部分CCD设备)时,仅实现原有类的方法是不够的。在深入分析RTS2源码的基础上,重点从参数、命令、协议扩展方面研究基于原有的Camera类,通过继承的方法构造新的CCD类型,实现对LAMOST项目的 CCD控制,取得了较好的效果,对在RTS2中集成望远镜系统其他类型设备也有较好的参考价值。     

天王星卫星两种定标方法测定结果的比较

利用新发表的高精度、高密度天体测量星表UCAC2,对天王星的五颗主要卫星的CCD观测图像重新进行量测,采用不同方法作定标归算,并使用两种理论模型(GUST86和GUST06模型)计算卫星的理论位置。对不同方法所得到的卫星位置的O-C结果的分析和比较表明,本文获得的卫星位置精度,除天卫五(Miranda)有显著提高,其他4颗卫星的位置精度基本相同。本文中天卫一和天卫三的结果与"亮卫星定标法"的结果在精度上相当,天卫二的位置精度与其他天王星卫星的位置精度具有较好的一致性,这从另一方面证明了我们的"亮卫星定标法"的可靠性。此外我们还获得了天卫四的位置与精度。     

绕月探测工程CCD立体相机的实验室辐射定标

探月光学有效载荷系统含CCD立体相机与干涉成像光谱仪两台光学遥感器,CCD立体相机完成的科学目标主要是与激光高度计配合获取月球表面三维立体图像。文章主要叙述了三线阵立体相机的工作原理,定标内容、目的以及CCD裸片像元检测和整机的相对定标和绝对定标过程。     

云南天文台1米反光镜CCD系统的性能补充

云南天文台新安装的Tek 1024×1024 CCD照相机性能良好,本文讨论了该CCD使用手册上没有列出的某些性能,包括:bias的pattern;oversacn区;坏象元问题;以及快门效应。