  It is difficult to accurately measure the effective gravity (log g) in
late-type stars using broadband (eg. UBV or SDSS) or intermediate-band (uvby)
photometric systems, especially when the stars can cover a range of
metallicities and reddenings. However, simple spectroscopic observational and
data reduction techniques can yield accurate values for log g through
comparison of the Balmer jumps of low-resolution spectra with recent grids of
synthetic flux spectra.
