Designing Star Trackers to Meet Micro-Satellite Requirements

Huffman, Kara M.; Sedwick, Raymond J.; Stafford, James; Peverill, James; Seng, William Francis

doi:10.2514/6.2006-5654

Cited by 20 publications

(9 citation statements)

References 2 publications

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“…Considering x-and y-axes of boresight coordinate equal to zero in the charge-coupled device (CCD) frame, boresight coordinate in body frame is as follows: (13) Also, assuming that star identification has been done in the pattern recognition phase and its identification is known, unit vector of all stars in star catalog is clear as follows: (14) FOV dimension is 8 0 × 8 0 , so the angle of stars and boresight in the CCD coordinate could not be greater than 4°. Thus, the angle of the boresight vector in the inertial frame and all of the star vectors in the catalog are calculated at any time, and stars in each frame are recognized as follows: (15) Then, for star mapping on the CCD frame, star coordinates (in millimeters) are calculated as follows: (16) Also, star place in the CCD according to and is as follows and shown in Figure 3: (17) Because the N vector method is selected for attitude determination in this article, its relation will be introduced later.…”

Section: Attitude Determination By Star Trackermentioning

confidence: 99%

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Optimal attitude and position determination by integration of INS, star tracker, and horizon sensor

Rad

Nobari

Nikkhah

2014

IEEE Aerosp. Electron. Syst. Mag.

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Section: Attitude Determination By Star Trackermentioning

confidence: 99%

“…After another century had passed, scientists again noticed celestial navigation, and the first star sensor was invented and manufactured by NASA to be used in the Mars missions [14], [15]. As star catalogs and star sensors evolved, a wide utilization of this sensor on satellite and spacecraft began.…”

Section: Introductionmentioning

confidence: 99%

Optimal attitude and position determination by integration of INS, star tracker, and horizon sensor

Rad

Nobari

Nikkhah

2014

IEEE Aerosp. Electron. Syst. Mag.

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“…After removing the star streaks, the precise centre of the satellite is calculated by using centroiding algorithms with subpixel accuracy. The centre of an object is extracted by algorithms such as a Weighted Sum (WS) technique and a Maximum Likelihood Estimator (MLE) technique (Samaan, 2011;Huffman, 2006). Once the image coordinate is extracted, the precise celestial coordinate of the satellite is calculated by transformation parameters between two celestial and image coordinates systems.…”

Section: S θ = Radon (Abs (Fft (I)))mentioning

confidence: 99%

The Design and Implementation of an Optical Astronomical Satellite Tracking System

Samadzadegan

Alidoost

2013

Int. Arch. Photogramm. Remote Sens. Spatial Inf. Sci.

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ABSTRACT:This paper presents a satellite tracking method based on optical celestial images. The proposed method is composed of two acquiring modes that are called Sidereal Stare Mode (SSM) and Track Rate Mode (TRM). To track the unknown satellites, first of all the entire of the sky is observed and the primary knowledge of the satellite location is predicted in SSM. Then, the measured pointing data is calculated and used by the telescope to acquire the satellite tracking images at the appropriate time. The framework of SSM contains main steps such as the image correction due to the noise and the image background by applying the iterative filtering methods, the star detection and removal using a double gate filter and PSF concepts, the star identification for image calibration based on a star catalogue, the streak detection of the satellite using the matched filter and finally, the extraction of the celestial coordinate of the satellite as a predicted position. In TRM, the group of star streaks should be identified in the free background image. Then, Fast Fourier Transformation (FFT) is applied and the characteristic of star streaks are extracted. Finally, the centroid of the satellite is estimated precisely by applying a binary mask and the right ascension and declination of it is calculated using astrometric transformation parameters. In this study, the searching and tracking algorithms is applied on the simulation images to detect and identify the satellite position in the sky. Therefore, a telescope along with a CCD camera is simulated to generate sequences images using the well-known star catalogues, the optical and orbital parameters. The precise celestial coordinate of a real satellite and two fictitious satellites are obtained from simulated images. The study results show that the accuracy of the satellite estimated position after star calibration is better than 5 arc seconds and the satellites tracking accuracy is around 1-3 arc seconds.

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“…Next, a program must be written to calculate the position of star on the detector pixels. For this purpose, the interpolation algorithms are generally used [9,11,22]. For precise attitude determination, the location of star in celestial sphere (Fig.…”

Section: Optical System and Image Processingmentioning

confidence: 99%

“…Star sensor is an important and high precision attitude control system [4][5][6][7][8][9]. It is an electro-optical system taking a picture from a set of stars (as point sources at infinity [6,7]) in celestial sphere and comparing it with the same star pattern from reference star catalogue to calculate the angular deviation of the satellite to a specific reference [9][10][11]. Finally, this information is sent to inertial guidance and control system to attitude correction of satellite [12,13].…”

Section: Introductionmentioning

confidence: 99%