兴隆60cm望远镜主焦CCD系统测光性能的研究

对兴隆６０ｃｍ望远镜主焦ＣＣＤ系统的测光性能进行了测试和研究,测定了ＣＣＤ快门时间函数,讨论了快门延迟效应对短时间曝光观测的可能影响,通过观测大批Ｌａｎｄｏｌｔ标准星,较准确地定出了ＢＶＲＩ宽带测光的星等系统转换关系,结果表明本系统与标准ＢＶＲＩ系统很接近,对ＣＣＤ系统的天文测光精度作了仔细的检验和分析,工对ＰＳＦ拟合测光和孔径测光两种方法进行了比较。     

兴隆60cm反射镜主焦CCD测光系统的基本性能测试

给出兴隆60cm反射镜主焦CCD系统测光性能的测试结果，内容包括bias和暗流的稳定性测试、平场分析、增益和读出噪声测定等。以期为CCD测光工作提供参考和指导。     

兴隆80cm TNT望远镜测光性能的研究

对兴隆80cm TNT望远镜CCD系统进行了测试和研究.观测了大批Landolt标准星定出了UBVRI宽带滤光片的星等系统转换关系,重点讨论了白光与R滤光片之间的关系,结果表明该系统与标准Johnson系统很接近,白光与R滤光片之间也比较接近.同时测定了兴隆站的夜天光.     

云南天文台1m望远镜卡焦(缩焦)CCD测光系统的初步研究

用云台１ｍ望远镜镜卡焦（缩焦）ＣＣＤ测光系统对测光标准星进行了ＢＶＲＩ四色测光,计算得到了该系统的转换方程及其转换结果,并对计算结果进行了分析讨论．     

云南天文台1m望远镜卡焦（缩焦）CCD测光系统的初步研究

用云台１ｍ望远镜卡焦（缩信）ＣＣＤ测光系统对测光标准准星进行了ＢＶＲＩ四色测光,计算得到了该系统的转换方程及其转换结果,并对计算结果进行了分析讨论。     

1.56m望远镜CCD照相机系统的消光系数和转换系数测定

测定了1.56m望远镜CCD照相机系统的消光系数和转换系数，消光系数k′和k″列在表1和表2，从观测星等到标准星等的转换系数列在表3，结果表明1.56m望远镜CCD测光系数做绝对测光是有困难的，最好是做相对测光。     

施密特望远镜CCD BVRI测光系统的初步研究

本文利用Thomson CCD,在北京天文台兴隆站施密特望远镜上进行BVRI四色测光,得到了该测光系统的颜色转换方程,并对所得结果进行了分析探讨。同时论证了BAO-CCD系统在施密特望远镜上用于测光的可行性。     

南京大学65cm反射式望远镜CCD相机的性能研究

2021年6月,使用南京大学本科实验教学的65 cm反射式望远镜系统,对其后端的电荷耦合器件(Charge-Coupled Device, CCD)的性能采用圆顶平场法进行了实际测定,得到了CCD相机的快门函数;同时用平场序列曝光,检测了CCD相机的线性。CCD相机的读出值从0到61 900模数转换单位(Analog-Digital Unit, ADU)非线性小于1%,同时CCD相机的増益为1.02e^-/adu,读出噪音为13e^-。但对于恒星这样的点光源的观测,当像元的数值高于38 000 adu时产生溢出。因此,在使用本CCD相机做点光源观测研究时,需要选择恰当的曝光时间,避免星像溢出。实际天文观测中,利用此研究得到的快门函数可以对观测图像进行校准,有效提高测光精度。     

云南天文台1.2米望远镜测光性能研究

利用云南天文台1.2m望远镜多色测光系统,选取一批Landoh标准星,利用较差测量的方法对该系统进行了大气消光系数和仪器转换系数的测定,分析了这套新的测光系统的性能.计算结果表明本系统与Johnson标准测光系统非常接近.同时也对该系统的测光精度进行了测定,在标准测光夜下测量亮于13.5等的星时,其V波段测光精度可达到0.041星等.     

关于地平式反射望远镜的CCD平场(英文)

现有标准设计的反光望远镜在拍摄CCD平场时,绝大多数都受残留散射光的影响.但是赤道式与地平式反光镜所受影响是不同的.在赤道式上做时间序列较差测光时,只要待测星永远位于CCD的固定像元上,不太准确的CCD平场也能得到高精度的测光结果.当需要0.1%～0.3%精度的平场时,则可以采用夜天平场.地平式的特点是,它的CCD相机必须置于旋转器上,在跟踪天体时不停地旋转,以抵消地球自转的影响.上述用于赤道式的方法失效,因此,在CCD平场时,消除散射光的影响比赤道式更为重要.一个典型的地平式反光镜的例子是NAOC兴隆天文台的EOS 1米镜.虽然该台已附加了防散射光的装置,但是对所有B、V、R、I滤光片,在不同旋转器位置拍摄的CCD平场,仍然有2%～3%的差别(主要是梯度).该文给出了改进的建议,必须满足下面两个条件:Cij=C(r);旋转器的中心与反光镜的光学中心重合.此问题的解决对所有地平式反光望远镜都有普遍意义.     

云台1m镜PI1024TKBCCDUBVRI测光系统

给出了云南天文台１ｍ望远镜ＰＩ１０２４ＴＫＢＣＣＤＵＢＶＲＩ测光系统的光谱响应曲线、中心波长和半宽,并同国际标准系统作了比较     

IRAF软件在Blazars天体中的CCD测光自动数据处理研究

针对IRAF软件在绝对测光法观测Blazars天体CCD测光中的应用,开发了一套自动数据处理的程序.该程序可以减少人为误操作的干扰,使观测结果更为稳定,提高了数据处理的效率.同时,在长期研究和使用IRAF软件的基础上,给出了我们应用IRAF软件在CCD测光中的一些研究结果,并对在Redhat Linux中的自动测光过程进行了总结.     

85cm天文望远镜圆顶和天窗自动化系统研制

描述了兴隆观测基地85cm天文望远镜圆顶及天窗自动控制系统的研制情况,给出了基于PLC控制器及Modbus通信协议的控制原理,以及系统中执行器、传感器等各部分的实现方法.本系统是兴隆观测基地实施圆顶通用化控制技术的一个案例.     

CCD Photometry of Very Young Open Clusters

We are developing a long term programme to determine abundances of peculiar stars, as a function of age, in open clusters with ages ≤ 5 × 10⁷ yr. A fundamental part will be to deduce the ages and physical properties of these clusters with higher accuracy than in previous studies. As part of this effort we present here CCD uvbyβ photometry of two open clusters, NGC 884 and NGC 869. This revised version was published online in July 2006 with corrections to the Cover Date.     

Problems of CCD Photometry of Fast-Moving Asteroids

The problems associated with the photometry of fast-moving asteroids are discussed. The effect of noise in CCD observations on the photometric accuracy is analyzed. A photometric accuracy limitation is shown to exist for observations of asteroids, which is determined by the angular rate of the object and the ratio of the flux from the object and noise due to sky background and dark current. The effective exposure for observing a moving object is determined. The method of overlapping areas is analyzed, which is used for obtaining the lightcurves of fast-moving asteroids. This method includes the determination of the mutual magnitude differences for the entire ensemble of comparison stars, the reduction of the magnitudes of all these stars to the magnitude of one of them adopted as the primary comparison star, the determination of the magnitude of the average star on each frame of the entire series of CCD observations, and the computation of the lightcurve as the difference between the magnitude of the asteroid and that of the average star.     

An Imaging Photon Counting Intensified CCD for High Speed Photometry

The scientific performance evaluation of a photon countingimaging system is presented. The detector is constituted by an ICCD camera with RbTe photocathode(optimized for UV radiation), and dedicated electronics for the acquisition and analysis ofthe events. For each photon event on the CCD, a real-time centroid calculation is performed, inorder to reach spatial resolution down to 25 m FWHM. The system has been tested usingthe 182 cm telescope of the Asiago Observatory.A standard stars field through U Johnson filter,and the Crab pulsar (PSR 0531+21) were observed. From the photometric data, relative magnitudes of the standard stars have been derived, showing a goodlinearity of the detector in the range of flux under consideration, as expected fromprevious laboratory measurements.The pulsar's data have been processed by FFT and epoch foldingtechniques to testthe detector's timing performances in the highest resolutionmode (4.512 ms).These observations show that a space resolved time analysis ofperiodic sources can be performed with 10^-7 s accuracy.     

CCD Photometry of Asteroid （147） Protogeneia

We measured the light-curve of the asteroid (147) Protogeneia in November 2004, with a CCD detector attached to the 1-meter telescope at the Yunnan Observatory, China. The synodic period and maximum amplitude of (147) at this apparition are 7.852 hours and 0.25 mag, respectively. The value of a/b for (147), from a preliminary estimation, is not less than 1.26:1.