1 Introduction

As discussed in Rosenberg et al. (2000, hereafter Paper I), the heterogeneity of the data often used in the literature for large scale studies of the Galactic globular cluster (GGC) properties has induced us to start a large survey of both southern and northern GGCs by means of 1-m class telescopes, i.e. the 91 cm European Southern Observatory (ESO)/Dutch telescope and the 1 m Isaac Newton Group (ING)/Jacobus Kapteyn telescope (JKT). We were able to collect the data for 52 of the 69 known GGCs with $(m-M)_{V}\leq 16.15$. Thirty-nine objects have been observed with the Dutch Telescope and the data have been already presented in Paper I. The images and the photometry of the remaining 13 GGCs, observed with the JKT are presented in this paper. A graphical representation of the spatial distribution of our cluster sample is given in Fig. 1.

Figure 1: Galactocentric distribution of all the GGCs with $(m-M)_{V}\leq 16.15$ mag. In the upper panel, the projection of the GGC location over the Galactic plane is presented. The open circles represent the GGCs presented in Paper I, the open squares the GGCs whose photometry and CMDs are discussed in this paper, and the asterisk indicates the position of the GGC Pal 1 (Rosenberg et al. 1998). The clusters which are not presented in our catalog are marked by open triangles. The lower panel shows the location of the same GGCs in a plane perpendicular to the Galactic plane. The Milky Way is also schematically represented

As a first exploitation of this new data base, we have conducted a GGC relative age investigation based on the best 34 CMDs of our catalog (Rosenberg et al. 1999, hereafter Paper III), showing that most of the GGCs have the same age. We have also used the data base to obtain a photometric metallicity ranking scale (Saviane et al. 2000, hereafter Paper IV), based on the red giant branch (RGB) morphology.

There are many other parameters that can be measured from an homogeneous, well calibrated CMD data base: the horizontal branch (HB) level, homogeneous reddening and distance scales, etc. We are presently working on these problems. However, we believe it is now the time to present to the community the complete data base to give to anyone interested the opportunity to take advantage of it.

In the next section, we will describe the observations collected at the JKT in 1997. The data reduction and calibration is presented in Sect. 3, where a comparison of the calibration of the northern and southern clusters is also discussed for three objects observed with both telescopes. In order to assist the reader, in Sect. 4 we present the main parameters characterizing our clusters. Finally, the observed fields for each cluster, and the obtained CMDs are presented and briefly discussed in Sect. 5.