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We present a new formation scenario for NGC2419, which is one of the mostluminous,one of the most distant, and as well one of the most extended globularclusters of the Milky Way. We propose that NGC2419 is the remnant of a mergedstar cluster complex, which was possibly formed during an interaction between agas-rich galaxy and the Milky Way. To test this hypothesis, we performednumerical simulations of 27 different models of star cluster complexes (CCs)moving on a highly eccentric orbit in the Galactic halo. We vary the CC mass,the CC size, and the initial distribution of star clusters in the CC to analyzethe influence of these parameters on the resulting objects. In all cases, thevast majority of star clusters merged into a stable object. The derivedparameters mass, absolute V-band magnitude, effective radius, velocitydispersion and the surface brightness profile are, for a number of models, ingood agreement with those observed for NGC2419. Despite the large range of CCsizes, the effective radii of the merger objects are constrained to arelatively small interval. A turnover in the r_eff vs. M_encl space leads todegenerate states, i.e. relatively compact CCs can produce an object with thesame structural parameters as a more massive and larger CC. In consequence, arange of initial conditions can form a merger object comparable to NGC2419preventing us to pinpoint the exact parameters of the original CC, which formedNGC2419. We conclude that NGC2419 can be well explained by the merged clustercomplex scenario. Some of the recently discovered stellar streams in theGalactic halo might be related to the parent galaxy, which produced the clustercomplex in our scenario. Measurements of the proper motion of NGC2419 arenecessary to prove an association with one of the stellar streams.

A New Formation Scenario for the Milky Way Cluster NGC2419