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Using $N$-body simulations, we demonstrate that satellite dwarf galaxy pairswhich undergo significant mixing ($\sim 6$ Gyr) can have their respective mostbound particles separated great distances upon subsequently merging with a moremassive host. This may provide an explanation as to the origin of the complexglobular cluster NGC 2149, which is found within the tail of the Sagittariusdwarf spheroidal galaxy, yet separated from its central remnant by over 100kpc. Dynamical investigations could support the chemical evidence which alreadypoints to the NGC 2419 being a nuclear star cluster. Motivated by the distinctnature of NGC 2419, we run a suite of simulations whereby an initial pre-infallmerger of two satellites is followed by a post-infall merger of the remnantinto a MW-like host potential. We present a striking example from our suite inthis work, in which this separation is reproduced by the most bound particlesof the two pre-infall satellites. Additionally, this double merger scenario caninduce unusual on-sky features in the tidal debris of the post-infall merger,such as clouds, overdensities, and potentially new arms that could resemble thebifurcation observed in Sagittarius.

Disrupted dwarf binary merger as the possible origin of NGC 2419 and Sagittarius stream substructure