2004AJ....128.2265D

Based on synthetic flux spectra calculated from theoretical atmospheric models, a calibration of temperature and metallicity for the dwarfs observed in the Beijing-Arizona-Taiwan-Connecticut multicolor photometric system is presented in this paper. According to this calibration, stellar effective temperatures can be obtained from some temperature-sensitive color indexes. The sample stars have colors and magnitudes in the ranges 0.1<d-i<0.9 and 14.0<i<20.5. The photometric metallicities for these sample stars can be derived by fitting SEDs. We determine the average stellar metallicity as a function of distance from the Galactic plane. The metallicity gradient is found to be d[Fe/H]/dz=-0.37±0.1 dex/kpc for z<4 kpc and d[Fe/H]/dz=-0.06±0.09 dex/kpc between 5 and 15 kpc. These results can be explained in terms of different contributions in density distribution for Galactic model ``thin disk'', ``thick disk'', and ``halo'' components. However, for the gradient in z>5 kpc, it could not be interpreted according to the different contributions from the three components because of the large uncertainty. So it is possible that there is little or no gradient for z>5 kpc. The overall distribution shows a metallicity gradient d[Fe/H]/dz=-0.17±0.04 dex/kpc for z<15 kpc.