A New Simplified Selection Algorithm of the Guide Star Catalogue for a Star Sensor

2014 ◽  
Vol 67 (6) ◽  
pp. 984-994 ◽  
Author(s):  
Xinlu Li ◽  
Jinhua Yang ◽  
Liu Zhang ◽  
Shuang Li ◽  
Guang Jin
Keyword(s):  
Uniform Distribution ◽  
Solid Angle ◽  
Screening Method ◽  
Study Objective ◽  
Star Catalogue ◽  
Star Tracking ◽  
Angle Method ◽  
Celestial Sphere ◽  
Guide Star ◽  
Star Pattern Identification

A guide star catalogue characterised by fewer guide stars, uniform distribution and high completeness is conducive to the improvement of star pattern identification and star tracking efficiency, and it has become an important study objective. A screening method, which takes “quasi-uniform distribution” of space solid angles as the principle and the size of the space solid angle corresponding to 4°×4° on the equator as the reference and divided the whole celestial sphere into 2,664 sub-blocks in sequence, is proposed in this paper. Based on this method, a “quasi-uniform” guide star catalogue with 2,937 guide stars was obtained. According to our ergodic statistical analysis of the whole celestial sphere, in a 12°×12° field of view, after the space solid angle method was used to divide the celestial sphere, the probability of emergence of three guide stars was 99·9% or above, while the number of guide stars decreased by 12·6% compared to the inscribed cube method. It can be concluded that when the completeness is equal, the space solid angle method is superior to the inscribed cube method in both capacity and distribution uniformity.

Division of guide star catalogue based on space solid angle “quasi uniform distribution”

2014 ◽  
Vol 22 (8) ◽  
pp. 2242-2246
Author(s):  
李欣璐 LI Xin-lu ◽  
杨进华 YANG Jin-hua ◽  
张刘 ZHANG Liu ◽  
金光 JIN Guang
Keyword(s):  
Uniform Distribution ◽  
Solid Angle ◽  
Star Catalogue ◽  
Guide Star

Optimization of guide star catalog for daytime star sensors

2019 ◽  
Vol 34 (01n03) ◽  
pp. 2040065
Author(s):  
Feng Wu ◽  
Xifang Zhu ◽  
Qingquan Xu ◽  
Ruxi Xiang ◽  
Qiuyang Yu ◽  
...  
Keyword(s):  
Signal To Noise Ratio ◽  
Simple Calculation ◽  
High Signal ◽  
Star Sensor ◽  
Infrared Band ◽  
Star Catalog ◽  
Celestial Sphere ◽  
Guide Star ◽  
Star Pattern Identification ◽  
Navigation Information

Daytime star sensor provides accuracy navigation information to air vehicles near the ground in the daytime by observing stars. It has been an important development of modern star sensors. In order to achieve a high signal-to-noise ratio, daytime star sensors work in the infrared band to avoid interferences from sky background. Daytime star sensors output accurate attitudes by identifying the observed stars in the field of view (FOV) according to the loaded guide star catalog. Guide stars are usually required to be distributed uniformly on the celestial sphere to improve the performance of star pattern identification. The parameters including limiting magnitude and FOV are determined by processing the 2MASS star catalog as the original star data and performing star distribution statistics. After constellation features are discussed, the idea of distributing stars in the local FOV to constellations is put forward by using the star pair angular separations. An optimization algorithm to build the guide star catalog for daytime stars is proposed to achieve evenly distributed guide stars. The guide star catalog is established and analyzed, proving that the proposed algorithm has simple calculation and easy realization. The Boltzmann entropy of obtained guide star catalog drops two orders of magnitude. Guide stars are distributed more uniformly.

scholarly journals Astrometric Positions of Quasars by CCD Observations

1997 ◽  
Vol 165 ◽  
pp. 547-550
Author(s):  
M. Assafin ◽  
R. Vieira Martins ◽  
A.H. Andrei
Keyword(s):  
Reference System ◽  
Star Catalogue ◽  
Sky Survey ◽  
Ccd Observations ◽  
Guide Star ◽  
Celestial Reference System

AbstractWe present results of CCD observations for 85 quasars with −80° ≤ δ ≤ +20° declination, belonging to the International Celestial Reference System (ICRS). The positions are referred to the Carlsberg Series (CAMC) and PPM catalogues. We discuss a method which allows one to obtain precise positions based only on CCD observations, on the use of the Digitized Sky Survey of ST ScI and on the Guide Star Catalogue. The results are compared with the VLBI positions.

scholarly journals The Second Guide Star Catalogue

1998 ◽  
Vol 179 ◽  
pp. 431-432 ◽  
Author(s):  
B. McLean ◽  
G. Hawkins ◽  
A. Spagna ◽  
M. Lattanzi ◽  
B. Lasker ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
New Technology ◽  
Great Success ◽  
Next Generation ◽  
Large Aperture ◽  
Star Catalogue ◽  
Queue Scheduling ◽  
Natural Data ◽  
Data Source ◽  
Guide Star

Although the HST GSC–I (Paper-I: Lasker et al. 1990, Paper-II: Russell et al. 1990, Paper-III: Jenkner et al. 1990) has been used with great success operationally, it was always known that it was possible to improve the scientific and operational usefulness by an increase in scope to include multi-color and multi-epoch data. Once the GSC-II concept was established, it was evident that, even beyond the original motivations in HST operations, it would address a number of other astronomical needs such as increasing demands for fainter catalogues to support remote or queue scheduling capabilities and adaptive optics on the next generation of large-aperture, new-technology telescopes. In addition, the all sky nature of the GSC–II makes it a natural data source for research in galactic structure.

scholarly journals Corrected GSC: Reference catalogue for CCD observations. Now

1996 ◽  
Vol 172 ◽  
pp. 483-486
Author(s):  
A. Lopez Garcia ◽  
L.I. Yagudin
Keyword(s):  
Hubble Space Telescope ◽  
Systematic Errors ◽  
Reduction Model ◽  
Adjustment Procedure ◽  
Star Catalogue ◽  
Accuracy Level ◽  
Ccd Observations ◽  
Telescope Optics ◽  
Guide Star ◽  
Dependent Error

Astrometrical properties of the Hubble Space Telescope Guide Star Catalogue (GSC) were recently investigated by the same authors through its comparison with the PPM catalogue. In this paper, a new systematic plate-based magnitude dependent error produced by telescope optics and by the incompleteness of plate reduction model has been found after applying a simplified block adjustment procedure. New subroutine for correction of all systematic errors is developed and GSC can be used now as a dense reference catalogue on about 0.4″ accuracy level.

scholarly journals A Test of the Astrometric Quality of the Southern Guide Star Catalog 1.2

1995 ◽  
Vol 166 ◽  
pp. 375-375
Author(s):  
B. Bucciarelli ◽  
C. R. Sturch ◽  
B. M. Lasker ◽  
M. G. Lattanzi ◽  
T. M. Girard ◽  
...  
Keyword(s):  
Limited Area ◽  
Large Database ◽  
Star Catalog ◽  
Star Catalogue ◽  
Star Density ◽  
Filtering Technique ◽  
Suitable Reference ◽  
Guide Star ◽  
External Check

We used preliminary positions of the Yale Southern Proper Motion (SPM) catalogue (Platais, Girard et al., Astronomy from Large Database II, eds. Heck & Murtag, 1992) in a region of 5 fields around the South Galactic Pole to assess the astrometric accuracy of the mask solution (Taff, Lattanzi and Bucciarelli, ApJ 361, 667, 1990), which will be used (in combination with the subplate method) for the construction of the Guide Star Catalogue (GSC) version 1.2. Another semi-external check is done by direct comparison of GSC positions of stars lying onto overlapping plate areas. Results in tables 1 and 2 show that the average rms of the GSC–SPM differences is quite satisfactory (∼ 0.33 arcsecper coordinate), while an error degradation (up to ∼ 1 arcsecpositional) can occurr within a limited area at the plate corners, its signature varying from plate to plate. This can be cured on a plate-by-plate basis by the use of a filtering technique, e.g., as provided by the Collocation method (Bucciarelli, Lattanzi and Taff, ApJ Suppl. 84, 91, 1993), wherever a suitable reference star density is available.

scholarly journals A fast method to retrieve data from a large star catalogue file

1982 ◽  
Vol 64 ◽  
pp. 99-101
Author(s):  
A. Schuetz
Keyword(s):  
Fast Method ◽  
Star Catalogue ◽  
Celestial Sphere

AbstractA method optimized for the access from a large catalogue of stars lying in a given cap of the celestial sphere is described. The performances of the method applied to the SAO catalogue are presented.

Astral Sciences in Ancient China

2018 ◽  
pp. 128-144
Author(s):  
Xu Fengxian
Keyword(s):  
Empty Space ◽  
Han Dynasty ◽  
The Sun ◽  
Space Theory ◽  
Ancient China ◽  
Star Catalogue ◽  
The Earth ◽  
The People ◽  
Solar Eclipses ◽  
Celestial Sphere

The chapter studies ancient Chinese astronomy, which focused on computing and predicting the movements of the heavens (天 tian), the sun, moon, stars, and asterisms, which was the duty of the rulers, in order that the people be well-regulated. Heavenly bodies were allocated to terrestrial zones, especially 28 constellations roughly along the equator or the ecliptic, the seven stars of the Big Dipper (regarded as the carriage of heaven), and the five planets. Unusual celestial phenomena were recorded, such as solar eclipses, comets, and meteorites. The 盖天 gai tian theory (celestial dome theory), the 浑天 hun tian Theory (celestial sphere theory) and the 宣夜 xuan ye theory (infinite empty space theory) were the three primary theories of the structure of the heaven and the earth, in the Han dynasty (202 bce—220 ce). The earliest extant Chinese star catalogue of the whole sky was composed in the 1st century bce, and the definitive constellation system of 283 constellations, 1464 or 1465 stars was composed in the 3rd century ce.

Pentagram star pattern identification algorithm applied in three-head star sensors

2017 ◽  
Vol 31 (19-21) ◽  
pp. 1740046
Author(s):  
Feng Wu ◽  
Xifang Zhu ◽  
Xiaoyan Jiang
Keyword(s):  
Monte Carlo ◽  
Success Rate ◽  
Pattern Identification ◽  
Identification Algorithm ◽  
Star Sensor ◽  
Star Pattern ◽  
Monte Carlo Experiments ◽  
Celestial Sphere ◽  
Star Pattern Identification

A pentagram star pattern identification algorithm for three-head star sensors was proposed. Its realization scheme was presented completely. Simulated star maps were produced by letting the three-head star sensor travel around the celestial sphere randomly and image the observed stars. Monte Carlo experiments were carried out. The performances of the pentagram algorithm were evaluated. It proves that its identification success rate reaches up to 98%.

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