V/70A               Nearby Stars, Preliminary 3rd Version  (Gliese+ 1991)
The following files can be converted to FITS (extension .fit .fgz or .fiZ)
Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=V/70A

drwxr-xr-x 141 cats archive 4096 Mar 17 2020 [Up] drwxr-xr-x 2 cats archive 288 May 26 16:25 [TAR file] -rw-r--r-- 1 cats archive 455 Sep 24 2012 .message -r--r--r-- 1 cats archive 10587 Jan 13 2008 ReadMe -rw-r--r-- 1 cats archive 1142 Sep 24 2012 +footg5.gif -rw-r--r-- 1 cats archive 13693 Sep 24 2012 +footg8.gif -r--r--r-- 1 cats archive 217756 Dec 6 1997 catalog.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html] -rw-r--r-- 1 cats archive 845 Feb 18 1999 notes.tex
Beginning of ReadMe : V/70A Nearby Stars, Preliminary 3rd Version (Gliese+ 1991) ================================================================================ Preliminary Version of the Third Catalogue of Nearby Stars GLIESE W., JAHREISS H. <Astron. Rechen-Institut, Heidelberg (1991)> ================================================================================ ADC_Keywords: Stars, nearby Description: The present version of the CNS3 contains all known stars within 25 parsecs of the Sun. It depends mainly on a preliminary version (Spring 1989) of the new General Catalogue of Trigonometric Parallaxes (YPC) prepared by Dr. William F. van Altena (Yale University). The catalogue contains every star with trigonometric parallax greater than or equal to 0.0390 arcsec, even though it may be evident from photometry or for other reasons that the star has a larger distance. For red dwarf stars, new color-magnitude calibrations for broad-band colors were carried out and applied. For white dwarfs, the recipes of McCook and Sion were applied (=1985ApJS...65..603M). Stroemgren photometry was used (not yet systematically) for early-type stars and for late dwarfs, the latter supplied by E. H. Olsen from Copenhagen Observatory (private communication). Contrary to the CNS2 (Gliese 1969) trigonometric parallaxes and photometric or spectroscopic parallaxes were not combined. The resulting parallax in the present version is always the trigonometric parallax -- if the relative error of the trigonometric parallax is smaller than 14 percent. The resulting parallax is the photometric or spectroscopic parallax only if no trigonometric parallax is available or if the standard error of the trigonometric parallax is considerably larger. Nomenclature Note: All new nearby stars have not been numbered, and only "NN" appears in the column "Name". There are therefore problems to designate these new stars, as e.g. in Reference =1994ApJS...93..287W . It is recommended for such stars to use one of the alternate designations from columns "Giclas", "LHS", "OtherName" or "Remarks". NOTE ADDED IN DECEMBER 1997: However, the usage found in the literature led to add a number for these "NN" stars, starting from 3001 (for star #2), 3002 (for star #4), etc, and ending with NN 4388.

© Université de Strasbourg/CNRS

    • Contact