THE STAR CLUSTER SYSTEM OF THE MERGER REMNANT NGC-7252

We present new U, B, V, and I images of the prototypical merger remnan t NGC 7252 obtained with the WFPC2 instrument of the Hubble Space Tele scope. The photometry reaches about 3 mag deeper than the previous obs ervations with WF/PCl and we detect 499 cluster candidates, most of th em previously undiscovered. We can distinguish three populations of st ar clusters. We confirm the existence of a very luminous, blue populat ion of clusters with a narrow range in color. Comparisons with Bruzual & Charlot (1996, in preparation) models incorporating a Salpeter stel lar IMF show that the mean ages of these clusters are 650 Myr for [Fe/ H] = 0.0 and 750 Myr if [Fe/H] = -0.3. Therefore, these are the cluste rs that formed during the merger event. The upper limit to the effecti ve radii of these objects is 4.8+/-0.4 pc (for D = 64.4 Mpc, H-0 = 75) , suggesting that they have physical properties like Galactic globular clusters. The second population of clusters is associated with the in ner disk. Their (U-B) colors and reddening-free Q values indicate that their light is dominated by O stars and that they have ages less than 10 Myr. However, with [R-eff] = 8.3 +/- 0.6 pc, these objects may be more like stellar associations and they may not survive for a signific ant time. Finally, there is also evidence for the presence of the most luminous of the old, metal-poor globular clusters that belonged to th e progenitor galaxies. The cluster luminosity function is a single pow er law with slope alpha approximate to -1.8 down to a limiting magnitu de of V = 26. The current specific cluster frequency is S-N = 0.6 +/- 0.3 for old clusters and young clusters with M > 10(5) M., but after t he remnant has faded for about 15 Gyr S-N will have increased to about 2.5. The central disk is now resolved into mush finer detail than in earlier WF/PCl observations and the light profile of the nuclear regio n is consistent with a single power lay with slope gamma= -1.26+/-0.03 . After both the main body and the cluster system of NGC 7252 have age d for several Gyr it may have the properties of a field elliptical. (C ) 1997 American Astronomical Society. [S0004-6256(97)00512-8].