2001A&A...374..105S

The discrepancy between the Pleiades cluster distance based on Hipparcos parallaxes and main sequence fitting is investigated on the basis of Stroemgren photometry of F-type stars. Field stars with the same metallicity as the Pleiades have been selected from the m₁ index and a technique has been developed to locate the ZAMS of these field stars in color-magnitude diagrams based on the color/temperature indices b-y, v-y, and β. Fitting the Pleiades to these ZAMS relations results in a distance modulus of 5.61±0.03mag in contrast to the Hipparcos modulus of 5.36±0.06mag. Hence, we cannot confirm the recent claim by Grenon (1999, in Proc. of 11th Cambridge workshop on cool stars, in press) that the distance problem is solved by adopting a low metallicity of the Pleiades ([Fe/H]_Pleiades=-0.11) as determined from Geneva photometry. The metallicity sensitivity of the ZAMS determined by the field stars is investigated, and by combining this sensitivity in all three color/temperature indices b-y, v-y, and β we get a independent test of the Pleiades distance modulus which support our value of 5.61mag. Furthermore, the field star sample used for the comparison is tested against theoretical isochrones of different ages to show that evolutionary effects in the field star sample are not biasing our distance modulus estimate significantly. Possible explanations of the Pleiades distance problem are discussed and it is suggested that the discrepancy in the derived moduli may be linked to a non-spherical shape of the cluster.