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Wide-Field Stellar Statistics from Tautenburg Schmidt Plates

Published online by Cambridge University Press:  26 July 2016

E. Schilbach ,
R.-D. Scholz  and
S. Hirte
E. Schilbach
Affiliation:
WIP-Projekt Astrometrie bei der Universität Potsdam, Sternwarte Babelsberg, An der Sternwarte 16, D-14482 Potsdam, Germany
R.-D. Scholz
Affiliation:
WIP-Projekt Astrometrie bei der Universität Potsdam, Sternwarte Babelsberg, An der Sternwarte 16, D-14482 Potsdam, Germany
S. Hirte
Affiliation:
WIP-Projekt Astrometrie bei der Universität Potsdam, Sternwarte Babelsberg, An der Sternwarte 16, D-14482 Potsdam, Germany

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For a detailed investigation of the kinematics of our Galaxy we need accurate proper motions and photometric data of stars over a wide range of magnitudes. The proper motions have to be obtained with respect to an extragalactic, i.e. nonrotating reference system. The best way to determine absolute proper motions of a great number of stars for further statistical analysis is to use the enormous amount of information stored on photographic plates taken with large Schmidt telescopes within the last decades. Since automated measuring machines have become available it is no longer a problem to extract this information from a Schmidt plate. Large Schmidt plates cover a sky area of more than 30 square degrees with usually thousands of stars and hundreds of galaxies per square degree outside the galactic plane. With the Tautenburg Schmidt telescope (134/200/400) more than 8000 plates have been taken in selected Northern sky areas since it was mounted in 1960. A 24 cm × 24 cm Tautenburg plate covers a field of about 10 square degrees, and a 20 minute exposure of a B plate has a limiting magnitude of 19 to 21. In comparison to other large Schmidt telescopes the plate bending is reduced to a minimum due to the four metre focal length and the use of relatively small plates. Therefore irregular positional shifts of the emulsion caused by the rebending after the exposure are of less influence. The large focal length leads to a plate scale of 51 arcsec/mm providing a relatively high positional accuracy.

Type
Part Nine: Galactic Structure
Information
Symposium - International Astronomical Union , Volume 161: Astronomy from Wide-Field Imaging , 1994 , pp. 441 - 443
Copyright
Copyright © Kluwer 1994 

References

Bunclark, P.S. and Irwin, M.J., 1983. In Proc. Statistical Methods in Astronomy Symp., Strasbourg (ESA SP-201), p. 195.Google Scholar
Dick, W.R., Ruben, G., Schilbach, E. and Scholz, R.-D., 1987. Astron. Nachr., 308, 211.CrossRefGoogle Scholar
Hirte, S., Dick, W.-R., Schilbach, E. and Scholz, R.-D., 1990. In ‘Errors, Uncertainties and Bias in Astronomy’, eds. Jaschek, C. and Murtagh, F., Cambridge University Press, p. 343.Google Scholar
Kharchenko, N.V., Schilbach, E. and Scholz, R.-D., 1993. See poster paper at this Symposium.Google Scholar
Schilbach, E., 1988. In ‘Mapping the Sky. Past Heritage and Future Direction’, eds. Debarbart, et al., Reidel Publ. Comp., Dordrecht, p. 451.Google Scholar
Schilbach, E. and Scholz, R.-D., 1992. Astron. Nachr., 313, 243.CrossRefGoogle Scholar
Schilbach, E., Guibert, J., Geffert, M. and Hirte, S., 1993. In ‘Developments in Astrometry and their Impact on Astrophysics and Geodynamics’, eds. Mueller, et al., Reidel Publ. Comp., Dordrecht, p. 255.Google Scholar
Scholz, R.-D. and Hirte, S., 1991. Astron. Nachr., 312, 45.Google Scholar
Scholz, R.-D., Odenkirchen, M. and Irwin, M.J., 1993. Mon. Not. R. astron. Soc., in press.Google Scholar