By R. C. Stone, C. C. Dahn (auth.), Erik Høg, P. Kenneth Seidelmann (eds.)
Astrometry is at the threshold of serious alterations considering this decade, on my own, is witnessing an development of stellar positions akin to the complete development of the former centuries. The Hipparcos satellite tv for pc has concluded its observations, and the catalog is in education. initial effects guarantee that the Hipparcos catalog will offer positions, parallaxes and annual right motions for over 100,000 stars with accuracies of 1.5 milliarcseconds. additionally, the Tycho catalog will supply positions of approximately 30 milliarcseconds accuracy for over 1 million stars, and annual right motions with three milliarcsecond accuracy will thus be ob tained through first epoch positions from the Astrographic Catalog. Optical interferometers at the floor are starting operation, and those tools promises observational accuracies of roughly one milliarcsecond. additionally, the conventional reference body according to the joys damental Catalog of vivid stars is being changed by means of the extragalactic ref erence body, in accordance with radio resources with accuracies of 1 milliarcsecond. therefore, astrometry will switch from a primary reference body outlined by way of the dynamical reference body of the sun approach with accuracies of a hundred milliarcseconds to a space-fixed, extragalactic reference body with accuracies of 1 milliarcsecond. destiny astrometric observations could be within the 1 -100 milliarcsecond accuracy diversity. there are various recommendations for destiny astrometric tools in area. each one of these delivers sub-milliarcsecond astrometric accuracies.
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Additional info for Astronomical and Astrophysical Objectives of Sub-Milliarcsecond Optical Astrometry: Proceedings of the 166th Symposium of the International Astronomical Union, Held in the Hague, The Netherlands, August 15–19, 1994
When the catalogs have been adjusted to the zero points of DE200, they are combined to give stellar positions and proper motions. The zero points of these positions and motions should coincide with those of the DE200 over a wide range of epochs. The positions and motions will first be used to make a final adjustment to the equinox and equator of each of the Step 1 catalogs. This prepares each catalog for Step 2 by bringing it into coincidence with the mean zero points of the system. 2. STEP 2 The data of step 2 come from a combination of absolute and quasi-absolute catalogs.
SPIE, 628,422. M. (1994) Baseline Metrology System of the USNO Astrometric lntetferometer, in Amplitude and Intensity Spatial Interferometry II, ed. B. Breckinridge, Proc SPIE, 2200, 71. J. (1994) Four Years of Astrometric Measurements with the Mark III Optical lntetferometer, Astron. , 108, 326. Mozurkewich, D. (1994) A Hybrid Design for a Six Way Beam Combiner, in Amplitude and Intensity Spatial Interferometry II, ed. B. Breckinridge, Proc. SPlE, 2200, 76. H. (1988) The Marlc III Stellar lntetferometer, Astron.
The results of Tab. 1 are based on the observations made TABLE 1. Internal error of a single observation vs. (mas) 90 87 115 99 119 194 63 78 92 110 122 188 in winter, spring, and summer seasons and for a wide variety of declination zones from -10 0 to +420. For a region closer to the zenith the internal errors become smaller in all magnitudes. The field of view covers the width of 37 arcmin in declination. 3 square degrees. In this size of area about 7500 stars brighter than 16th mag are expected to be found, or roughly 60,000 stars during eight consecutive hours.