  We present imaging results from a high Galactic latitude survey designed to
examine the structure of the Galactic halo. The objective of the survey is to
identify candidate halo stars which can be observed spectroscopically to obtain
radial velocities and confirm halo membership. The Washington filter system is
used for its ability to distinguish between dwarfs and giants, as well as
provide a metallicity indicator. Our most successful imaging run used the BTC
camera on the CTIO 4m telescope in April 1999. Photometric conditions during
these observations provided superb photometry, with average errors for a star
at $M=18.5$ of 0.009, 0.008, 0.011, and 0.009 for $C$, $M$, $DDO51$, and $T2$
respectively. These data are available with the electronic version of this
paper, as well as through ADC (http://adc.gsfc.nasa.gov/). We use these data as
a template to describe the details of our photometric reduction process. It is
designed to perform CCD reductions and stellar photometry automatically during
the observation run without the aid of external packages, such as IRAF and IDL.
We describe necessary deviations from this procedure for other instruments used
in the survey up to June 2000. Preliminary results from spectroscopic
observations indicate a 97% efficiency in eliminating normal dwarfs from halo
giant candidates for $M<18.5$. Unfortunately, low-metallicity subdwarfs cannot
be photometrically distinguished from giants using the Washington filters.
These major contaminates unavoidably reduced the overall giant identification
efficiency to 66% for $M<18.5$. Our improved knowledge of these stars will
increase this efficiency for future spectroscopic observations.
