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The tangential velocity dispersion of stars belonging to the Milky Wayglobular cluster's tidal tails has recently been found from N-body simulationsto be a parameter that distinguishes between cored and cuspy profiles oflow-mass dwarf galaxy dark matter subhaloes where that globular cluster formed,and the in-situ formation scenario. In this context, we discovered that M5'stidal tails are composed by stars at two different metallicity regimes ([Fe/H]~ -1.4 dex and -2.0 dex). The more metal-rich tidal tail stars are of the samemetal content than M5's members and have a tangential velocity dispersion thatcoincides with the predicted value for a cuspy formation scenario (subhalo mass$\sim$ 10$^9$ M$_{\odot}$). The more metal-poor stars, that are found along theentire M5 tidal tails and have similar distributions to their more metal-richcounterparts in the M5 colour-magnitude diagram and orbit trajectory, have atangential velocity dispersion that refers to a cored subhalo (mass $\sim$10$^9$ M$_{\odot}$) or an in-situ formation scenario. In order to reconcile thedual distribution of M5 tidal tail stars, in kinematics and chemistry, wepropose that M5 collided with another more metal-poor and less massive globularcluster anytime before or after it was accreted into the Milky Way.

The dual nature of the tidal tails of NGC 5904 (M5)