The applicability of the Strömgren system for abundance determination of late-type stars has been shown by several authors (e.g. Eggen 1978b, Bond 1980, Ardeberg and Lindgren 1981). The aim of our contribution is not to present a completely new calibration. Rather we want to discuss the (b-y)-m1 diagram with an increased sample of spectroscopically analysed stars, hoping to eliminate some unsatisfying properties of previous approaches and to make improvements in terms of generality and reliability.