  Stellar spectra derived from current multiple-object fiber-fed spectroscopic
radial-velocity surveys, of the type feasible with, among other examples,
AUTOFIB, 2dF, HYDRA, NESSIE, and the Sloan survey, differ significantly from
those traditionally used for determination of stellar abundances. The spectra
tend to be of moderate resolution (around $1\,${\AA}) and signal-to-noise ratio
(around 10-20 per resolution element), and cannot usually have reliable
continuum shapes determined over wavelength ranges in excess of a few tens of
Angstroms. Nonetheless, we have developed techniques to extract true iron
abundances and surface gravities from such spectra of G-type stars in the
4000--$5000\,${\AA} wavelength region. The theoretical basis and calibration
using synthetic spectra are described in detail in another paper. The practical
application of these techniques to observational data is given in the present
paper. We show that this method can provide true iron abundances, with an
uncertainty of less than $ 0.2$ dex over the range of metallicity found in the
Galactic thick and thin disks, from spectra obtained with fiber-fed
spectrographs.
