共查询到20条相似文献，搜索用时 62 毫秒
1.
天文观测站夜天空星像星等信息和天区分布信息可用于指导多设备巡天观测.建立全天相机监测系统(Monitoring all-sky system)对本地天区夜天空实时监测,获取的监测图像需要有效的方法进行处理以提取全天图像星像信息.由于全天图像视场大和高阶扭曲的影响,采用天顶等距投影与多项式函数组合的方法计算图像的底片常数.天文定位的均方根残差约为0.15个像素.通过对图像中亮星部分测光得到的星等差,改正大气消光误差.最后使用HEALPix (Hierarchical Equal Area isoLatitude Pixelation)方法实现天区划分和每个天区可观测极限星等值的存储. 相似文献
2.
3.
《天文研究与技术》2021,(1)
在建的云南大学多通道测光巡天望远镜(Multi-channel Photometric Survey Telescope, Mephisto)预计在2022年开展W巡天(Mephisto-W Survey),将对北半球可观测天区(赤纬δ-15~°,面积约26 000平方度)开展多通道多历元测光巡天,为细致描绘银河系结构、深刻理解星系形成和演化理论、精确限制宇宙学模型、深入探究暗物质暗能量本质提供重大契机。基于丽江观测站天文台址监测系统2019全年观测数据,利用机器学习方法模拟丽江站一年的台址条件模型,简单估算了在不同曝光时间下,多通道多历元测光巡天一整年对巡天天区的可观测次数与期望极限星等。考虑到多通道多历元测光巡天的科学目标,建议对每个天区单次观测采用曝光2次,每次时长为20 s的曝光模式,在这种曝光模式下,可以实现全年对巡天天区在每组滤波片组合(ugi和vrz)下分别进行约3.8次观测,单次观测r波段极限星等可达22.37等,叠加星等可达23.11等。 相似文献
4.
5.
6.
用于低纬子午环的CCD象元尺寸的大小将影响可观测的视场和星像的定位精度。本文根据低纬子午环配备CCD的观测原理,综合考虑视场和星像的定位精度两方面的因素,认为选择1024×1024(24μ)的CCD芯片是一种切实可行的方案。 相似文献
7.
盱眙近地天体望远镜CCD视场为1.94°×1.94°,作为大视场望远镜由于存在场曲现象,因此根据单颗星像调焦会导致PSF(Point Spread Function)分布不均匀.研究所拍摄图像的PSF分布特征,并通过拟合半高全宽和离焦量的函数关系模拟出弯曲焦面,从而确定出最佳成像平面.制定出根据PSF的半高全宽直方图来判断最佳成像平面的调焦方法. 相似文献
8.
本文给出在北京天文台兴隆观测站获得的盾牌座δ型变星金牛座θ~2的新光电测光资料,它们是新近开展的一次多台站国际联合观测的一部分。以前得到的四频率解(文[1])与新资料符合得极好。单次测量的残差约±0.003星等。 相似文献
9.
1996年4月10日，使用北京天文台兴隆观测站60cm望远镜及其主焦上的TI215CCD照相机[1]，在NGC4027天区发现了一颗超新星．这是今年开始的超新星巡天计划的第一个结果．这颗超新星已被McDonald天文台的王力帆证实，并被分类为Ⅱ型超新星．国际天文学会中央电报局已将它列为SN1996W[2]． 相似文献
10.
11.
Roy E. Hoffman 《Monthly notices of the Royal Astronomical Society》2003,340(3):1039-1051
12.
13.
C. Fabricius L. Helmer O. H. Einicke L. V. Morrison P. Gibbs L. Quijano J. L. Muiños 《Astrophysics and Space Science》1991,177(1-2):35-40
At the Carlsberg Automatic Meridian Circle on La Palma an observing programme of 72500 stars is in progress. The observing conditions are discussed and a status report is presented as well as some plans for future programmes. A special effort is made for stars between vis. mag. 11
m
.
0 and 12
m
.
0 in a general net as well as in radio source fields. Some of these sources will be observed with the Danish 1.5m telescope on La Silla. Also discussed are fundamental programmes and large astrophysical programmes. 相似文献
14.
G. I. Pinigin 《Astrophysics and Space Science》1991,177(1-2):225-227
Observing programs are discussed for the Pulkovo automatic horizontal meridian circle. The instrument is highly efficient and yields precise and accurate positions. We prepare an observing program of faint FK5 stars with the aim of improving on the system of this catalogue and also prepare a program of observations of IRS reference catalogue stars. 相似文献
15.
Brian Warner 《Astrophysics and Space Science》1995,228(1-2):283-297
Suggestions and examples are given for photometric and spectrographic programs with 0.5 - 1.0m telescopes, both at poor and at good sites. The importance is stressed of coordination between observers at sites spread over a region or around the world. As an example of the latter, the Whole Earth Telescope group and their successful observing programs are described. 相似文献
16.
17.
F. Primas 《Astrophysics and Space Science》1999,265(1-4):67-70
A new sample of 7 stars ranging in metallicity from [Fe/H] = −2.0 to [Fe/H] = −0.75 has been analyzed in the boron spectral
region. The targets were selected according to the availability (in the literature) of their lithium and beryllium abundances,
because the simultaneous knowledge of LiBeB in the same targets is a powerful diagnostic for testing depletion and internal
mixing predicted by different stellar structure models. Two stars (HD 94028 and HD 194598), characterized by similar Li contents,
are found to have also similar B abundances, despite a 0.3 dex difference in their Be abundances claimed by Thorburn and Hobbs
(1996). Four stars out of 7 are characterized by strongly depleted Li and Be abundances: 2 of them (HD 2665 and HD 3795) are
also significantly B-depleted, while two others (HD 106516 and HD 221377) have near normal B abundances despite being depleted
by a factor ≥ 10 in both Li and Be abundances. These stars place strong constraints on the nature and depth of the mixing
processes responsible for their light element abundances. The 7th star (HD 160617) shows the remarkable aspect of deficient
B, probably deficient Be, and completely normal Li. No stellar destruction mechanism can explain this. Rather, chemical inhomogeneities
in the halo could be the cause.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
18.
19.
The Space InfraRed Telescope Facility (SIRTF) is the fourth and finalelement in NASA's family of orbiting Great Observatories. SIRTFconsists of a 0.85-meter diameter telescope and three cryogenically-cooledscience instruments capable of observing from the near- to the far-infrared,between 3 and 180 m. Incorporating the latest in large-format infrareddetector arrays, SIRTF offers orders-of-magnitude improvements in capabilityover existing facilities. Launch is scheduled for December 2001, with ananticipated lifetime of up to 5 years. SIRTF will observe targets rangingfrom small, icy bodies in the outer Solar System to the most luminousknown objects in the distant reaches of the Universe. SIRTF representsan important scientific and technical bridge to NASA's new Origins program,and is managed for NASA by the Jet Propulsion Laboratory, CaliforniaInstitute of Technology. 相似文献