共查询到20条相似文献，搜索用时 78 毫秒
1.
北京天文台的锑化铟光度计,于1982年秋在兴隆观测站的60公分反射望远镜上投入了观测。这种光度计可以用来观测天体的宽带JHKLM光度,本文将介绍它的设计原理、构造、以及性能和特点。文末还将介绍兴隆站的近红外大气消光情况以及YYGem。的部分观测结果。 相似文献
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本文给出在美国佛罗里达(Florida) 大学的Rosemary Hill天文台研制的一个观测资料实时处理的近红外光度计的主要结构和性能。着重讨论了该仪器的数据采集系统,并对将来仪器的改进提出了一些设想。 相似文献
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一个利用光子计数方式的、可以同时对变星、比较星和天空背景进行测光的光度计已装于北京天文台兴隆工作站的60cm反光望远镜.它有一台专用计算机实时处理三个通道的数据,结果可以由打印机输出,对快变现象还可以在CRT或长图记录仪上显示.光度计经过几年试用,已取得一些观测结果,表明性能基本满足天文观测的要求. 相似文献
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基于Camera Link总线的CCD高速图像采集技术 总被引：1，自引：0，他引：1
现代天文学研究越来越依赖于高质量的天文观测结果。针对天文实测的需要,对基于Camera Link总线的CCD高速图像采集技术进行了系统调研,分析对比了Camera Link总线技术及其优缺点,对基于Camera link接口的高速CCD采集技术进行了深入的研究,着重讨论了单缓存与双缓存高速采集技术和实现机制。经实际测试,所实现的技术稳定、可靠,CPU负载低,采集速度达到了厂家给出的CCD相机的最高采集速度,可以满足天文大数据量采集与准实时观测的需要。 相似文献
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本文叙述了用于北京天文台60厘米反光望远镜上的掩星用光度计。光度计由可调电平补偿的直流放大器组成。数据采集系统采用以8085 为cpu 的 SDK-85 单板微型计算机和相应的接口电路组成。为了得到精确的观测时刻,还发展了用微型计算机作短波时号对钟的装置。系统的时间分辨率可达1毫秒,时刻记录精度为±2毫秒。最后,还给出了掩星观测的实例。 相似文献
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现代大型天文望远镜的控制一般由多台独立(或组成集群)的计算机完成。这些计算机的性能、效率与可靠性直接影响整个望远镜的稳定运行。因此,需要研制一套实时对各控制计算机(节点)硬件资源信息进行采集、存储、监控的软件系统,并提供一定的预警功能。这样的系统可以有效排除隐患进而提高望远镜整体观测运行的效率。在深入分析LAMOST观测运行需求的基础上,采用异步协程技术,设计和开发了一套基于Python语言的硬件资源监控系统,系统可以高效稳定地采集获取计算机的各种状态,也可以获得相应部件的实时信息,并提供多种人机交互方式,为后续开发提供了扩展接口。该系统部署于LAMOST环境中,实际运行表明整个系统取得了较好的效果。 相似文献
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B. N. Ashoka Kumar V. C. Babu S. Seetha V. Girish S. K. Gupta Ram Sagar S. Joshi P. Narang 《Journal of Astrophysics and Astronomy》2001,22(1):131-144
The design and performance of a portable three channel photometer installed at the Uttar Pradesh State Observatory (UPSO),
Naini Tal is described. The photometer is modular and the whole unit can be disassembled as individual channels such that
the system can also be used as a single channel or two channel photometer. The system also has provision to monitor a guide
star. The instrument was put into operation since November 1999 on the 1m Sampurnanand telescope at UPSO, Naini Tal. Since
then, it is used extensively for the ‘Survey of rapidly oscillating Ap (roAp) stars in the northern sky’ from UPSO. Observational
results using this new photometer in its initial phase of operation are discussed. The advantage of having continuous sky
measurement is demonstrated. 相似文献
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对北京天文台新近改造成的三通道高速光度计的结构和性能进行介绍,并给出了在兴隆站85公分望远镜的一些实测结果. 相似文献
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Yang Tinggao 《时间频率学报》1995,(1)
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 相似文献
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J. W. Campbell 《Astrophysics and Space Science》1971,11(3):417-422
A stellar photometer utilizing a Cassegrain telescope optical system was flown in a Skylark rocket. The photometer scanned the night sky using the precessional and roll motions of the rocket and obtained observations of some ninety-two stars at a wavelength of 1450 Å. 相似文献
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If the hypothesis is correct that most solar-like stars have planetary systems and have planets in inner orbits, then approximately 1% of these stars should have planets with orbital planes close enough to our line of sight to show transits. To get a statistically significant estimate of the fraction of stars that have planets in inner orbits, it is necessary to monitor thousands of stars continuously for a period of several years. To accomplish this requires the use of a multi-channel photometer system. We present here several multi-channel methods that have been used for ground-based observations and a concept for applying multi-channel photometry to the detection of numerous Earth-sized planets.Paper presented at the Conference onPlanetary Systems: Formation, Evolution, and Detection held 7–10 December, 1992 at CalTech, Pasadena, California, U.S.A. 相似文献
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在1984年2—3月,用美国McDonald天文台91cm反射镜的UBV测光系统和云南天文台35厘米反射镜V色测光系统,对Archer 1959年在后发座用照相方法发现的24颗变(双)星中的17颗进行了观测研究,全部没有大于0~m.07的光变,其中12颗的连续观测时间长于半个周期以上,因而至少它们不是原定周期和变幅的那种变星。其他5颗或Archer未给周期,或观测复盖不够半个周期,未能肯定。最后给出这些星和比较星的星等和色指数。 相似文献
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We report observations of 24 stars in the fields of the three Seyfert galaxies MCG +08-23-067, Mrk 817, and Mrk 290. The observations
were made with a CCD array photometer in the BVRcIc bands. The V magnitudes of the observed stars ranged from 13.5 and 17.2.
For stars of approximate magnitude 15, the typical photometric errors are 0.010, 0.011, 0.008 and 0.011 magnitude in the BVRI
bands, respectively. The BVRI magnitudes of all these stars were not known previously. In the field of the galaxy Mrk 290
a star has been found that probably has a periodic brightness variation with P=1.518 days and the mean value V=14.80 and which
may belong to the class of “spotted” stars. 14′x14′ charts are supplied for identifying the stars. These results can be used
for differential photometry of active galactic nuclei in the BVRI bands.
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Translated from Astrofizika, Vol. 51, No. 1, pp. 41–50 (February 2008). 相似文献
18.
The search of roAp stars at Mt. Dushak-Erekdag Observatory was started in 1992 using the 0.8 m Odessa telescope equipped with
a two-star high-speed photometer. We have observed more than a dozen stars so far and discovered HD 99563 as roAp star while
BD+8087 is suspected to have rapid oscillations. Negative results of our observations for the search of rapid oscillations
in four stars in NGC 752 are also discussed. 相似文献
19.
We solve the problem on a kinematic analysis of the three-dimensional velocity field of stars from zonal catalogues, i.e.,
catalogues in which the stars are presented at all right ascensions in some declination zones. We have constructed a system
of vector spherical harmonics with the properties of completeness and orthogonality for a chosen declination zone. We suggest
a method that allows the Ogorodnikov-Milne model parameters in the Galactic coordinate system to be estimated by analyzing
the proper motions and radial velocities of stars in the equatorial coordinate system. The vector spherical harmonics are
shown to have the following advantages over the standard approach based on a direct leastsquares estimation of the parameters
for a specific model. First, in contrast to the standard approach, the new method can reveal all systematic components of
the velocity field irrespective of a particular model. Second, it allows one to get rid of the correlation between the sought-for
parameters, which presents a serious problem for the conventional method in the case of zonal catalogues. Third, the method
of vector spherical harmonics allows the kinematic parameters to be estimated at least by two techniques. Comparison of these
two solutions makes it possible to test the standard kinematic model for compatibility with the observational data. The developed
method has been tested on the basis of numerical experiments and applied for a kinematic analysis of the proper motions of
Tycho-2 stars in the southern hemisphere for which the parallaxes can be estimated using data from the Tycho-2 Spectral Type
Catalogue. 相似文献
20.
Markus Nielbock Thomas Müller Ulrich Klaas Bruno Altieri Zoltán Balog Nicolas Billot Hendrik Linz Koryo Okumura Miguel Sánchez-Portal Marc Sauvage 《Experimental Astronomy》2013,36(3):631-660
We present a flux calibration scheme for the PACS chopped point-source photometry observing mode based on the photometry of five stellar standard sources. This mode was used for science observations only early in the mission. Later, it was only used for pointing and flux calibration measurements. Its calibration turns this type of observation into fully validated data products in the Herschel Science Archive. Systematic differences in calibration with regard to the principal photometer observation mode, the scan map, are derived and amount to 5 ? 6 %. An empirical method to calibrate out an apparent response drift during the first 300 Operational Days is presented. The relative photometric calibration accuracy (repeatability) is as good as 1 % in the blue and green band and up to 5 % in the red band. Like for the scan map mode, inconsistencies among the stellar calibration models become visible and amount to 2 % for the five standard stars used. The absolute calibration accuracy is therefore mainly limited by the model uncertainty, which is 5 % for all three bands. 相似文献