The field centered approximately on
the center of NGC 288 was monitored at Las Campanas Observatory
with the 1-m Swope telescope and with the 2.5-m duPont telescope.
The observational data
were collected during several runs conducted between December 1990 and
September 1992. The data were taken on 25 nights and on 7 nights
the cluster was monitored continuously for at least
4.5 hours. Three different cameras were used:
a) 10242 Tektronix CCD with scale 0.61 
- TEK2
camera, 1-m telescope;
b) 20482 Ford Aerospace CCD with scale 0.435 - FORD
camera, 1-m telescope;
c) 20482 Tektronix CCD with scale 0.23 - TEK3
camera, 2.5-m telescope.
Most of data were taken with the V filter, with only occasional exposures
taken in the B and I bands. We obtained a total of 462 useful
images in the V-band.
The exposure time ranged from 7 minutes to 10 minutes.
For the prevailing number of images the seeing was better than 1.5 arcsec.
A detailed log of all observations was submitted to the editors of
A&A (see Appendix A).
Figure 1: Finding chart for NGC 288 variables.
Each chart is 30 arcsec on a side with
north up and east to the left
The preliminary processing of the raw data was made with IRAF
.
Stellar photometry was extracted using DAOPHOT/ALLSTAR (Stetson 1987)
and DoPHOT (Schechter et al. 1993) programs.
We followed procedures described in some details in
Kaluzny et al. (1995).
The instrumental photometry was transformed to the V system
with the zero point defined by the data set from CTIO (Paper I).