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[Abridged] Several large scale photometric and spectroscopic surveys arebeing undertaken to provide a more detailed picture of the Milky Way. Given thenecessity of generalisation in the determination of, e.g., stellar parameterswhen tens and hundred of thousands of stars are considered it remains importantto provide independent, detailed studies to verify the methods used in thesurveys. We evaluate available calibrations for deriving [M/H] from Stromgrenphotometry and develop the standard sequences for dwarf stars to reflect theirmetallicity dependence and test how well metallicities derived from ugrizphotometry reproduce metallicities derived from the well-tested system ofStromgren photometry. We use a catalogue of dwarf stars with both Stromgrenuvby photometry and spectroscopically determined iron abundances (in total 451dwarf stars with 0.3<(b-y)_0<1.0). We also evaluate available calibrations thatdetermine log g. A larger catalogue, in which metallicity is determineddirectly from uvby photometry, is used to trace metallicity-dependent standardsequences for dwarf stars. We derive new standard sequences in the c_1,0 versus(b-y)_0 plane and in the c_1,0 versus (v-y)_0 plane for dwarf stars with 0.40 <(b-y)_0 < 0.95 and 1.10 < (v-y)_0 < 2.38. We recommend the calibrations byRamirez & Me'endez (2005) for deriving metallicities from Stromgren photometryand find that intermediate band photometry, such as Stromgren photometry, moreaccurately than broad band photometry reproduces spectroscopically determined[Fe/H]. Stromgren photometry is also better at differentiating between dwarfand giant stars. We conclude that additional investigations of the differencesbetween metallicities derived from ugriz photometry and intermediate-bandphotometry, such as Stromgren photometry, are required.

astronomy and astrophysics

The ability of intermediate-band Stromgren photometry to correctly  identify dwarf, subgiant, and giant stars and provide stellar metallicities  and surface gravities