&lt;title&gt;Full-sky Astrometric Mapping Explorer (FAME) CCD centroiding experiment&lt;/title&gt;

Triebes, K.; Gilliam, L.; Hilby, Timothy; Horner, Scott D.; Perkins, Patrick; Vassar, R.; Harris, Frederick H.; Monet, D. G.

doi:10.1117/12.394031

Cited by 8 publications

(10 citation statements)

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“…The SIM target selection is yet to happen, but will be focussed towards searches for low-mass planets around a few nearby stars, calibration of the distance scale, and detailed studies of known micro-lensing events. FAME (Full-Sky Astrometric Mapping Explorer; Triebes et al 2000), selected by NASA in the MIDEX competition in 1999, and DIVA (Double Interferometer for Visual Astrometry; Röser et al 1997), a small German astronomy satellite planned for launch in 2004, are essentially successors to Hipparcos, with an extension of limiting sensitivity, sample size and accuracy (statistical weight) by a factor of order 100 in each. DIVA and FAME will both provide an excellent reference frame, substantially improve calibration of the distance scale and the main phases of stellar evolutionary astrophysics, and map the Solar Neighbourhood to much improved precision.…”

Section: Gaia and Other Space Missionsmentioning

confidence: 99%

GAIA: Composition, formation and evolution of the Galaxy

Perryman

Boer

Gilmore

et al. 2001

A&A

1,035

1,023

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Abstract. The GAIA astrometric mission has recently been approved as one of the next two "cornerstones" of ESA's science programme, with a launch date target of not later than mid-2012. GAIA will provide positional and radial velocity measurements with the accuracies needed to produce a stereoscopic and kinematic census of about one billion stars throughout our Galaxy (and into the Local Group), amounting to about 1 percent of the Galactic stellar population. GAIA's main scientific goal is to clarify the origin and history of our Galaxy, from a quantitative census of the stellar populations. It will advance questions such as when the stars in our Galaxy formed, when and how it was assembled, and its distribution of dark matter. The survey aims for completeness to V = 20 mag, with accuracies of about 10 µas at 15 mag. Combined with astrophysical information for each star, provided by on-board multi-colour photometry and (limited) spectroscopy, these data will have the precision necessary to quantify the early formation, and subsequent dynamical, chemical and star formation evolution of our Galaxy. Additional products include detection and orbital classification of tens of thousands of extra-Solar planetary systems, and a comprehensive survey of some 10 5 −10 6 minor bodies in our Solar System, through galaxies in the nearby Universe, to some 500 000 distant quasars. It will provide a number of stringent new tests of general relativity and cosmology. The complete satellite system was evaluated as part of a detailed technology study, including a detailed payload design, corresponding accuracy assesments, and results from a prototype data reduction development.

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Section: Gaia and Other Space Missionsmentioning

confidence: 99%

GAIA: Composition, formation and evolution of the Galaxy

Perryman

Boer

Gilmore

et al. 2001

A&A

1,035

1,023

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“…In the star field data reduction, we use three algorithms to do the calculation of the centroid, namely, the photon weighted means(PWM), the linear corrected photon weighted means(LCPWM) [2,3] and the Gauss fitting. The standard deviations are derived.…”

Section: The Centroid Calculationmentioning

confidence: 99%

“…In this paper, we present the preliminary results of determining the separations between star images. Without calibration of pixel positions and intra-pixel response, we have demonstrated that the standard deviation of differential centroiding is below 7.4e-3 pixel by the algorithm of linear corrected photon weighted means(LCPWM) [2,3]. For comparison, the photon weighted means(PWM) and Gauss fitting are also used in the data reduction.…”

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confidence: 98%

Preliminary results of centroiding experiment for the STEP mission

Li¹,

Li²,

Cao³

et al. 2015

SPIE Proceedings

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Search for Terrestrial Exo-Planet (STEP) [1] was originally proposed in 2013 by the National Space Science Center, Chinese Academy of Sciences, which is currently being under background engineering study phase in China. The STEP mission is a space astrometry telescope working at visible light wavelengths. The STEP aims at the nearby terrestrial planets detection through micro-arcsecond-level astrometry. Determination of the separation between star images on a detector with high precision is very important for astrometric exoplanets detection through the observation of star wobbles due to planets. The requirement of centroiding accuracy for STEP is 1e-5 pixel. A centroiding experiment have been carried out on a metrology testbed in open laboratory. In this paper, we present the preliminary results of determining the separations between star images. Without calibration of pixel positions and intra-pixel response, we have demonstrated that the standard deviation of differential centroiding is below 7.4e-3 pixel by the algorithm of linear corrected photon weighted means(LCPWM) [2,3]. For comparison, the photon weighted means(PWM) and Gauss fitting are also used in the data reduction. These results pave the way for the geometrical calibration and the intra-pixel quantum efficiency(QE) calibration of detector array equipment for micro-pixel accuracy centroiding.

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“…This assumption was originally adopted by the FAME group for their laboratory experiment (Triebes et al 1999(Triebes et al , 2000. However, our treatment of the coefficient k is different from that of the FAME group.…”

Section: Ccd Centroiding Experimentsmentioning

confidence: 99%

The optical system for JASMINE and the CCD centroiding experiment

Yano¹,

Gouda²,

Kobayashi³

et al. 2004

Proc. IAU

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We have investigated the optical design for the Japan astrometry satellite mission (JASMINE). In order to accomplish measurements of astrometric parameters with high accuracy, optics with a long focal length and a wide focal plane for astrometry are required. In 1977 Korsch proposed a three mirror system with a long focal length and a wide focal plane. The Korsch system is one of the convincing models. However, the center of the field is totally vignetted because of the fold mirror. Therefore we consider an improved Korsch system in which the center of the field is not vignetted. Finally, we obtain the diffraction limited optical design with small distortion. Our project needs a common astrometric technique to obtain precise positions of star images on solid state detectors to accomplish its objectives. In order to determine the centers of stars, an image of the point source must be focused onto the CCD array with a spread of a few pixels. The distribution of photons (photoelectrons) over a set of pixels enables us to estimate positions of stars with sub-pixel accuracy. We modify the algorithm to estimate the real positions of stars from the photon weighted mean, which was originally developed by the FAME (Full-Sky Astrometric Mapping Explorer) group. Finally, we obtain the results from the experiment that the accuracy of estimation of distance between two stars has a variance of about 1/300 pixel; that is, the error for one measurement is about 1/300 pixel, which is almost an ideal result given by Poisson photon noise. We also investigate the accuracy of estimation of positions with a different size of PSF. In this case also, we find that the accuracy of estimation has a variance of about 1/300 pixel.

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<title>Full-sky Astrometric Mapping Explorer (FAME) CCD centroiding experiment</title>

Cited by 8 publications

References 0 publications

GAIA: Composition, formation and evolution of the Galaxy

GAIA: Composition, formation and evolution of the Galaxy

Preliminary results of centroiding experiment for the STEP mission

The optical system for JASMINE and the CCD centroiding experiment

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