太阳系外行星的凌星观测研究

为对太阳系外行星的物理参数进行更精确估算,利用山东大学威海天文台/威海市天文台的1 m反射望远镜,对7颗已知具有行星系统的恒星:TrES-1、TrES-3、XO-2、WASP-1、WASP-2、WASP-3、HAT-P-7,进行了凌星现象的观测研究.介绍观测和数据处理的基本情况,给出凌星光变曲线结果及由之推算出的一些行星参数.在总结结果并加以分析的同时,展望下一步将进行的更为深入细致的研究.     

Photoelectric photometry of asteroids 37, 80, 97, 216, 270, 313, and 471

Photoelectric observations of several minor planets were made from 1975 to 1977 at the Astronomical Observatory of Torino. Lightcurves and period information are given for 7 objects: 37 Fides, 80 Sappho, 97 Klotho, 216 Kleopatra, 270 Anahita, 313 Chaldaea, and 471 Papagena.     

Automated astrographic plates measuring process

The astrographic plates measuring process applied at the Astronomical Observatory of Valencia has been described.The measure of astrographic plates of our minor planets observation programme has been carried out by means of a binocular microscope with a photometer, held by a personal computer through an interface. The process of measure in each position of the plate holder is automated, once two stars are selected and the sequence of the objects to be measured is defined.The process will be improved in the next future, by the substitution of the searching device (a photometer) by a CCD camera plus a digitizer board.Paper presented at the 11th European Regional Astronomical Meetings of the IAU on New Windows to the Universe, held 3–8 July, 1989, Tenerife, Canary Islands, Spain.     

Photometric Follow-up Transit (Primary Eclipse) Observations of WASP-43 b and TrES-3b and A Study on Their Transit Timing Variations

Two photometric follow-up transit (primary eclipse) observations on WASP-43 b and four observations on TrES-3 b are performed using the Xuyi Near-Earth Object Survey Telescope. After differential photometry and light curve analysis, the physical parameters of the two systems are obtained and are in good match with the literature. Combining with transit data from a lot of literature, the residuals (O ? C) of transit observations of both systems are fitted with the linear and quadratic functions. With the linear fitting, the periods and transit timing variations (TTVs) of the planets are obtained, and no obvious periodic TTV signal is found in both systems after an analysis. The maximum mass of a perturbing planet located at the 1:2 mean motion resonance (MMR) for WASP-43 b and TrES-3 b is estimated to be 1.826 and 1.504 Earth mass, respectively. By quadratic fitting, it is confirmed that WASP-43 b may have a long-term TTV which means an orbital decay. The decay rate is shown to be P? = (?0.005248 ± 0.001714) s·yr^?1, and compared with the previous results. Based on this, the lower limit of the stellar tidal quality parameter of WASP-43 is calculated to be ${Q^{\prime }}_{*}\ge 1.5\times {10}^5$, and the remaining lifetimes of the planets are presented for the different ${Q^{\prime }}_{*}$ values of the two systems, correspondingly.     

Long-term transit timing monitoring and homogenous study of WASP-32

We report new photometric observations of the transiting exoplanetary system WASP-32 made by using CCD cameras at Yunnan Observatories and Ho Koon Nature Education cum Astronomical Centre, China from 2010 to 2012. Following our usual procedure, the observed data are corrected for systematic errors according to the coarse decorrelation and SYSREM algorithms so as to enhance the signal of the transit events. Combined with radial velocity data presented in the literature, our newly observed data and earlier photometric data in the literature are simultaneously analyzed to derive the physical parameters describing the system by employing the Markov chain Monte Carlo technique. The derived parameters are consistent with the result published in the original paper about WASP-32b, but the uncertainties of the new parameters are smaller than those in the original paper. Moreover, our modeling result supports a circular orbit for WASP-32b. Through the analysis of all available mid-transit times, we have refined the orbital period of WASP-32b; no evident transit timing variation is found in these transit events.     

窄线赛弗特1星系Arakelian564的测光

使用上海天文台 1.5 6m望远镜 ,对窄线赛弗特 1星系Ark 5 6 4进行了时间跨度为 3星期的观测 ,给出了VRI波段的光学观测结果。使用交叉相关方法研究了三个波段之间的时间延迟 ,但是未发现有时间延迟     

New photometric analysis of hot Jupiter: WASP-135b

We report photometric follow-up observations of WASP-135b obtained using the 1.23-m telescope at Calar Alto Observatory and 1.00-m telescope at TÜBİTAK National Observatory during the 2017 and 2018 observational seasons. Eight new transit light curves of WASP-135b were analyzed with jktebop code. The ratio of the planet radius to radius of host star, fractional radius of host star, and orbital inclination of WASP-135b were found to be 0.138 ± 0.002, 0.181 ± 0.008 and 82.44 ± 0.64 degrees, respectively. Planetary radius of WASP-135b was derived from transit parameters to be 1.075 ± 0.150 R_J. The transit ephemeris of WASP-135b was also updated using the maximum likelihood method (MLM). 165 well-known hot Jupiters (HJs) were selected from the Exoplanet Data Explorer database and the classification of these HJs together with WASP-135b, based on their equilibrium temperatures and Safronov numbers, is discussed.     

UBV光电测光系统的转换方程和精度比较

根据对鬼星团中Ｊｏｈｎｓｏｎ测光标准星的观测，我们研究了北京天文台６０ｃｍ望远镜直流光电光度计ＵＢＶ测光系统的转换方程．应用该方程推算了对三颗变星观测得到的ＵＢＶ星等，讨论了所得光变曲线的精度，并与较差方法所得结果进行了比较     

Astroinformation resource of the Ukrainian virtual observatory: Joint observational data archive, scientific tasks, and software

This paper reviews the most important components of the national project of the Ukrainian Virtual Observatory (UkrVO). Among them, there is the establishment of a Joint Digital Archive (JDA) of observational data, which has been obtained at Ukrainian observatories since the 1890s, including an astronegative JDA (more than 200 thousand plates). Since this task requires VO-oriented software, such issues as content verification software, integrity and administration of the JDA, compliance of image formats with the IVOA standards, and photometric and astrometric calibration of images are considered as the most important directions of software development, which carried out by members of the UkrVO. The scientific projects using local data archives of the UkrVO are discussed, namely: an analysis of a long observational series of active galactic nuclei, the study of solar flares and solar active regions based on spectral observational archives, research and discovery of variable stars, and the study of stellar fields in the vicinity of gamma-ray bursts. Particular attention is devoted to the CoLiTec Program that permits us to increase a number of observed solar system bodies and allows us to discover new bodies; for example, the C/2010 (Elenin) and P/2011 N01 comets were discovered using this program at the ISON-NM Observatory. The paper notes the creation of the UkrVO JDA prototype that provides access to the databases of the Main Astronomical Observatory, National Academy of Sciences of Ukraine (MAO NAS of Ukraine); Nikolaev Astronomical Observatory (NAO); and Lvov Astronomical Observatory.     

上海天文台MK5A终端系统的安装与测试

简要阐述了上海天文台VLBI终端系统的发展历史与性能；介绍了在没有MK4解码器、互联网又不能满足需要的特殊情况下，利用数据质量分析仪(DQA)完成MK5A终端系统安装与测试的过程和方法。目前，MK5A终端系统已经成功地应用于上海天文台所有的VLBI实验。     

Photoelectric lightcurves of asteroid 433 Eros

Photoelectric observations of the asteroid 433 Eros were carried out with the 50-cm reflector of the Astronomical Observatory of the University of Cluj-Napoca on January 21 and February 4 and 5, 1975.     

吉林天文观测基地光学观测环境及相关研究进展

地基光学天文望远镜是人类探索与研究宇宙的重要手段, 对已有地基光学台址的光学观测环境进行监测分析, 可以为后期设备针对性改造以及观测者调整观测策略提供参考依据, 对提升地基光学设备的观测效能具有重要的意义. 吉林天文观测基地(简称``基地'')隶属于中国科学院国家天文台长春人造卫星观测站, 位于吉林省吉林市大绥河镇小绥河村南沟约5 km处(东经126.3^\circ, 北纬43.8^\circ, 海拔高度313m). 基地大气视宁度均值范围约为1.3$''$--1.4$''$、天顶附近V波段的天光背景亮度为20.64magcdotarcsec^-2、年晴夜数最高可达270余天, 具有良好的天文观测条件. 吉林天文观测基地于2016年投入运行, 现有1.2m光电望远镜、迷你光电阵列望远镜、大视场光电望远镜阵列、新型多功能阵列结构光电探测平台等多台(套)光电望远镜设备. 利用上述设备, 主要围绕空间目标探测与识别、精密轨道确定、光电探测新方法以及变源天体的多色测光等开展相关研究工作, 与多家国内高校及科研院所保持着良好的合作关系.     

Optical Monitoring of 3C 66A in 1994–2008

3C 66A is one of the most interesting blazar. Our monitoring was carried out with a 1.56-m telescope of the Shanghai Astronomical Observatory (SHAO) from 13 December 1994 to 9 November 2008. Some peaks and gradual brightening of the source up to three times were observed.     

Investigations of space debris at Terskol observatory

Within the framework of the “Astronomy in the Elbrus Region” international program, investigations of space debris objects using optical measurements are carried out at the observation complex of the Zeiss-2000 telescope (developed by the International Center for Astronomical and Medico-Ecological Research, National Academy of Sciences, Ukraine) at Terskol Observatory. The objectives of this study are to detect, catalog, and determine the physical characteristics of small-sized space debris fragments, maintain orbit catalogs, and investigate the influence of nongravitational perturbations on the orbital motion and the evolution of orbits of these fragments.     

Results of astrometric observations of stars with large proper motions using telescopes of the Research Institute of Nikolaev Astronomical Observatory

Astrometric CCD observations of stars with large proper motions were carried out during 2008–2014 using telescopes of the Nikolaev Astronomical Observatory. A catalog of positions and proper motion of 1596 fast stars with proper motions exceeding 150 mas/yr has been compiled based on observation results. The catalog covers the declination zone from 0° to 65°. The standard error of derived proper motion is 1…10 mas/yr for both coordinates depending on the observational history of the star. Data from eight different star catalogs and surveys have been used to derive proper motion. The comparison results of proper motion with data from modern catalogs and results of the statistical test for the detection of possible invisible components are given.     

22.6--3.8 GHz 太阳射电动态频谱仪

给出北京天文台 ２．６—３．８ ＧＨ_(ｚ)太阳射电动态频谱仪的性能、结构及初步观测结果．     

2000年度上海天文台卫星激光测距观测报告

介绍了 2 0 0 0年度上海天文台卫星激光测距观测和系统的改进情况     

Distributions of the Venus 1.27-μm O2 airglow and rotational temperature

Imaging spectroscopic observations of the Venus 1.27-μm O₂ airglow were carried out with ground-based telescopes from 2002 to 2007. Spectral image cubes were taken with the Okayama Astrophysical Observatory/infrared imaging spectrometer (superOASIS), the Gunma Astronomical Observatory/near-infrared camera and NASA's Infrared Telescope Facility/cryogenic echelle spectrograph (CSHELL). The rotational temperature shows weak positive correlation with the airglow intensity. However, there are some regions that have almost same intensities but different temperatures. The intensities tend to decrease from the anti-solar point to the terminator besides local features. These results indicate that there are local strong downward flows superimposed on the subsolar-to-antisolar circulation.     

Current state and development of the minor planets research in Nikolaev Astronomical Observatory

Regular positional observations of minor planets in Nikolaev Astronomical Observatory have been begun with installation of photographic Zone Astrograph in 1961. The observations of 19 selected minor planets up to 12 magnitude were obtained for 36 years. Accuracy of the photographic positions of minor planets is rather high, 0.15^′′-0.19^′′. These positions were used for improvement of the system of fundamental catalogue and determination of its orientation to the dynamical reference frame. CCD observations of asteroids have been begun at the Zone Astrograph in 2000. There was obtained about the same accuracy, as in photographic observations. During 2004-2006 NAO participated in international collaboration with TUBITAK National Observatory (Turkey) and Kazan State University (Russia) in positional and photometric observations of small Solar system bodies. About four thousands of CCD images for 58 asteroids of 11-18 mag were obtained with internal and external errors of 30-80 mas of a single determination. Some of these observations, as well as the observations of the Minor Planet Center, are being used for the current asteroid mass determinations in Nikolaev observatory. Available results allow us to consider the Russian-Turkish telescope RTT150 as a good candidate for ground-based astrometry support of the future space mission GAIA, moreover in the period before GAIA.