Observed values of the Stroemgren uvby colors were collected from the literature. A computer program calculated the reddening for each star. This value was used to compute the unreddened value of (b-v), c1, and m1. These were then used to compute [c(1)], [m(1)], and [u-b] for the star. Except for the H beta index, the observed quantities are not included. Introduction: The stars were divided into groups by spectral types by means of the bracket quantities. Stars which deviated too greatly from the standard relations could not be dereddened. These include peculiar stars and high luminosity stars and are listed in reject.dat. Various discussions by Crawford were followed to deredden the other stars. The zero point of the [Fe/H] relation was changed from 0.4 to 0.2 on the basis of the study by Gustafsson and Nissen (1972A&A....19..261G) and some corrections were made to the effective temperature scale in order to fit the new model by Kurucz (1979ApJS...40....1K). Otherwise, the derivations followed the methods of Philip, Miller, and Relyea (1976, Dudley Obs. Rep. No. 12, 1).

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