/ftp/cats/I/16



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I/16           Catalog of 3356 Faint Stars, 1950                (Larink+ 1955)
The following files can be converted to FITS (extension .fit .fgz or .fiZ)
	catalog.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=I/16
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drwxr-xr-x 317 cats archive 8192 Feb 28 11:16 [Up] drwxr-xr-x 2 cats archive 240 Aug 21 2023 [TAR file] -rw-r--r-- 1 cats archive 461 Dec 19 2022 .message -r--r--r-- 1 cats archive 4527 Dec 27 1999 ReadMe -rw-r--r-- 1 cats archive 574 Feb 14 2013 +footg5.gif -rw-r--r-- 1 cats archive 11974 Feb 14 2013 +footg8.gif -r--r--r-- 1 cats archive 111264 Dec 27 1999 catalog.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : I/16 Catalog of 3356 Faint Stars, 1950 (Larink+ 1955) ================================================================================ Katalog von 3356 Schwachen Sternen fuer das Aequinoktium 1950 Larink J., Bohrmann A., Kox H., Groeneveld J., Klauder H. <Verlag der Sternwarte, Hamburg-Bergedorf (1955)> ================================================================================ ADC_Keywords: Fundamental catalog; Positional data; Proper motions Description: This catalog of 3356 faint stars was derived from meridian circle observations at the Bergedorf and Heidelberg Observatories. The positions are given for the equinox 1950 on the FK3 system. The stars are mainly between 8.0 and 10.0 visual magnitude. A few are brighter than 8.0 mag. The lower limit in brightness resulted from the visibility of the stars. Introduction: All stars were observed at both the Heidelberg and Bergedorf Observatories. Normally, at each observatory, two observations were obtained with the clamp east and two with the clamp west. The mean errors are comparable for the two observatories with no significant systematic difference in the positions between them. The mean errors of the resulting positions should be approximated 0.011s/cos(dec) in right ascension and ).023" in declination. The proper motions were derived from a comparison with the catalog positions with the positions in the AGK2 and AGK2A with a 19 year baseline and from a comparison of new positions with those in Kuestner 1900 with about a fifty year baseline. The magnitudes were taken from the AGK2. Most spectral types were determined by A. N. Vyssotsky. A few are from the Bergedorfer Spektraldurchmusterung.