2000A&A...363..947J

The G dwarf metallicity distribution of a mass limited sample of stars within 40 pc and south of δ=-26° and for which Stroemgren uvby and H_β photometry is available is studied. Special care is taken to ensure that the sample consists of stars with a main sequence lifetime longer than the age of the Galactic disk. Furthermore, binary stars, subgiants, active stars, etc. are removed to ensure that the sample is as clean as possible. The sample was limited to the mass interval 0.7-1.0M_☉ using masses determined by interpolation between theoretical evolutionary tracks. A mass interval was used as opposed to a color interval, as it is more directly comparable with theoretical models. The final sample contains 253 stars. Even though the sample shows a remarkably small low metallicity tail a new scale height weighting method was developed, and used. The resulting G dwarf distribution cannot be reconciled with the simple model for chemical evolution, in fact this dataset shows that the G dwarf problem is even larger than earlier results indicate.