The observations were made from September 7, 1992, through September 9, 1995, using the ESO 0.50 m telescope at the European Southern Observatory, La Silla, Chile. A single channel photometer with the R 943-02 photomultiplier, Hamamatsu, and the ESO UBVRI filters have been used.
A total of 73 nights were granted in 6 observing runs, and of these, 43 nights were totally or partially photometric. Both the observing and the reduction methods are described by Moreno & Carrasco (1986).
The program stars observations were always done as close to the meridian as possible. For the brightest objects, an annular diaphragm fixed at the entrance pupil of the telescope was used to prevent saturation of the detector.
In order to have an homogeneous set of photometric data together
with all the
FK5 Stars of the declination zone ranging from 
to
, 31 stars taken from the E-regions (Graham
1982) were
used as standard stars. To determine the transformation to the
standard
system, 3 or 4 stars were observed hourly.
The mean number of observations for the program stars is 7.6, with a minimum of 3 observations per star. About 30% of the observed stars correspond to standard stars in every night of observation. Depending on the period of the year, this is a total of 15 to 25 standard stars a night.
The reductions of the observations were done using the computing facilities at La Silla with the Snopy General Purpose Photometric Reduction Program. Zero-point corrections, extinction determinations, color transformations and the final colors and the magnitudes were determined for each night separately.