Astrometry with the Keck Interferometer
A key thrust of NASA's Origins program is the search for and detection of planetary systems about other stars.
astrometry↗
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Problems of astrometry
Construction of reliable inertial coordinate system - star catalogs from Ukrainian observatories, ILS materials analysis and increasing accuracy of astrometric observations
STELLAR MOTION↗
Photographic astrometry and overlap reduction techniques
Rigorous adjustment algorithms are discussed which extract hidden information contained in overlapping photographs of star fields. In particular, the development of adequate physical and statistical models is emphasized.
Googe, W. D.↗
Inversion of very large matrices encountered in large scale problems of photogrammetry and photographic astrometry
The simultaneous adjustment of very large nets of overlapping plates covering the celestial sphere becomes computationally feasible by virtue of a twofold process that generates a system of normal equations having a bordered-banded coefficient matrix, and solves such a system in a highly efficient manner. Numerical results suggest that when a well constructed spherical net is subjected to a rigorous, simultaneous adjustment, the exercise of independently established control points is neither required for determinancy nor for production of accurate results.
Brown, D. C.↗
Time, geodesy, and astrometry: Results from radio interferometry
The results from a total of a dozen transcontinental and intercontinental VLBI experiments are discussed. Particular emphasis is placed on: (1) the inferred behavior of the frequency standards, usually hydrogen masers, on time scales from 10 to 100,000 seconds; (2) the estimated celestial positions of the observed radio sources; (3) the determinations of the vector baselines; and (4) the inferred values of polar motion and UT.1.
Clark, T. A.↗
Application of very long baseline interferometry to Astrometry and Geodesy: effects of frequency standard instability on accuracy
The accuracy of geodetic and astrometric information obtained from very long baseline interferometry (VLBI) observations is dependent upon the stability of the frequency standard, or clock, used at each site of VLBI array. The sensitivities of two hydrogen maser frequency standards of different design to pressure, temperature, and magnetic field variations were measured; and, for one of the standards, sensitivity was found to be severe enough to degrade the information content of VLBI measurements. However, the effect on the geometric and astrometric information of such clock instabilities, with time scales of hours or greater, can be sharply reduced through the use of differencing techniques.
Clark, T. A.↗
Radio Astrometry
The utilization of conventional and VLBI interferometer techniques for accurate determination of UTI, polar motion, and radio source position catalog data is discussed.
Johnston, K. J.↗
Luminosity and astrometry of comets: A review
Visual and photographic observations of the brightness of comets are reviewed including methods and sources of errors. Nuclear magnitude estimates are discussed and interpreted in relation to determination of appropriate exposure times for photographic observations. The importance of brightness ephemarides is emphasized.
Roemer, E.↗
Space telescope optical telescope assembly/scientific instruments. Phase B: Preliminary design and program definition study. Volume 2A(3): Astrometry
Wide field measurements, namely, measurements of relative angular separations between stars over a relatively wide field for parallax and proper motion determinations, were made with the third fine guidance sensor. Narrow field measurements, i.e., double star measurements, are accomplished primarily with the area photometer or faint object camera at f/96. The wavelength range required can be met by the fine guidance sensor which has a spectral coverage from 3000 to 7500 A. The field of view of the fine guidance sensor also exceeds that required for the wide field astrometric instrument. Requirements require a filter wheel for the wide field astrometer, and so one was incorporated into the design of the fine guidance sensor. The filter wheel probably would contain two neutral density filters to extend the dynamic range of the sensor and three spectral filters for narrowing effective double star magnitude difference.
Source record↗
The potential for astrometry in the infrared
Infrared interferometry promises to be a useful astrometric technique. Preliminary measurements of the star alpha Orionis made with a heterodyne interferometer exhibit phase coherence over a period of at least 1000 seconds. The measurements were equivalent to a positional determination of 60 milliarcsecond accuracy every 5 seconds of integration.
Storey, J. W. V.↗
Phase delay astrometry and its geodetic applications
The accuracy inherent in the fringe phase in the determination of source positions was calculated. It is shown that accuracy can be utilized by applying differencing techniques in order to circumvent such systematic effects as clock drift and delay due to the propagation media.
Wittels, J. J.↗
Submilliarcsecond astrometry via VLBI. I - Relative position of the radio sources 3C 345 and NRAO 512
The relative position and relative proper motion of the radio sources 3C 345 and NRAO 512 are estimated from four sets of VLBI observations spread out over the period from October 1971 to May 1974. The use of phase-connection techniques yields the separation, in 1950.0 coordinates, of the centers of brightness of the compact components of the two sources. An upper bound of 0.0005 arcsec/yr is placed on the relative proper motion (70% estimated confidence limits). Bounds that can be placed on the distances to the two sources are considered, prospects for improvement in the determination of relative position and proper motion of these sources are discussed, and other possible applications of the basic technique are described.
Shapiro, I. I.↗
On the overlapping plate method in astrometry
A method is proposed for the simplification of the algorithms of Eichhorn and Russell (1976) for obtaining the solutions of astrometric problems using the overlapping plate method. The method provides the parameter vector (consisting of 'star constants' and plate constants) as well as the covariance matrix of the parameters. A considerable reduction in the amount of matrix algebra required is obtained with the present method.
Jefferys, W. H.↗
Space telescope astrometry
A description of instruments used for astrometric observations are examined with special emphasis on the Fine Guidance Systems of the space telescope. The telescope consists of a 2.4 meter diameter primary and a secondary figured to the Ritchey-Chretien design that yields a f/24 focal plane. The function of the FGS is to keep the total guidance jitter within the ST requirement of + or - 0.0007 rms, and to maximize the probability of finding suitable guide stars with the available 210 arcmin. Attention is given to the focal plane arrangement and to the ray paths and output images from the Koester's prisms. Some projected scientific uses of the space telescope are given as well as beneficial areas of close cooperation between the space telescope and the ESA.
Van Altena, W.↗
Space Telescope astrometry from CCD images
The astrometric application of the Wide Field Camera and the Planetary Camera is reviewed. It is shown that the digital image centering algorithms can yield a positional accuracy of 0.1 milli-arcsecond. Deconvolution of CCD's sensitivity, non-flatness of the filters, and crinkling of the CCD surface may limit the positional accuracy of 1 milli-arcsecond.
Chiu, L.-T. G.↗
Very-long-baseline radio interferometry - The Mark III system for geodesy, astrometry, and aperture synthesis
Up to 112 megabit/sec from each radio telescope of an interferometric array can be recorded and processed by the Mark III VLBI system. Sample results are given for baseline lengths between three antennas in the U.S. and three in Europe, as well as for the arc lengths between the positions of six extragalactic radio sources. No significant change is detected in any of these quantities. Signals of a given polarization or of pairs of orthogonal polarizations may be recorded in up to 28 contiguous bands, each nearly 2 MHz wide, for mapping the brightness distribution of compact radio sources. The demonstrated ability to record large bandwidths, and to link many large radio telescopes, allows compact sources with flux densities below 1 millijansky to be detected and studied.
Rogers, A. E. E.↗
Theoretical studies of the effects of grain noise on photographic stellar astrometry and photometry
A method of incorporating the effects of photographic emulsion grain noise into digital image centering algorithms is presented which improves the accuracy of the derived stellar positions and magnitudes. Theoretical formulae are then derived for the limiting error of the center, and the photometric parameters. For IIIa-J, this error is 0.2-0.3 mu for bright unsaturated images, which agrees quite well with measurements made with the Yale PDS microdensitometer. It is expected that, with further improvements in the positional accuracy of the PDS, it should be possible to reach the emulsion grain noise limit, providing that emulsion shifts or other large scale errors do not dominate. It is also shown that, with appropriate trimming, marginal distribution image centering algorithms can yield an accuracy only slightly poorer than that obtained with two-dimensional distributions.
Lee, J.-F.↗
Cometary Astrometry
Modern techniques for making cometary astrometric observations, reducing these observations, using accurate reference star catalogs, and computing precise orbits and ephemerides are discussed in detail and recommendations and suggestions are given in each area.
Yeomans, D. K.↗