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- W4385643977 abstract "Using $N$-body simulations, we demonstrate that satellite dwarf galaxy pairs which undergo significant mixing ($sim 6$ Gyr) can have their respective most bound particles separated great distances upon subsequently merging with a more massive host. This may provide an explanation as to the origin of the complex globular cluster NGC 2149, which is found within the tail of the Sagittarius dwarf spheroidal galaxy, yet separated from its central remnant by over 100 kpc. Dynamical investigations could support the chemical evidence which already points to the NGC 2419 being a nuclear star cluster. Motivated by the distinct nature of NGC 2419, we run a suite of simulations whereby an initial pre-infall merger of two satellites is followed by a post-infall merger of the remnant into a MW-like host potential. We present a striking example from our suite in this work, in which this separation is reproduced by the most bound particles of the two pre-infall satellites. Additionally, this double merger scenario can induce unusual on-sky features in the tidal debris of the post-infall merger, such as clouds, overdensities, and potentially new arms that could resemble the bifurcation observed in Sagittarius." @default.
- W4385643977 created "2023-08-08" @default.
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- W4385643977 date "2023-08-03" @default.
- W4385643977 modified "2023-09-26" @default.
- W4385643977 title "Disrupted dwarf binary merger as the possible origin of NGC 2419 and Sagittarius stream substructure" @default.
- W4385643977 doi "https://doi.org/10.48550/arxiv.2308.01958" @default.
- W4385643977 hasPublicationYear "2023" @default.
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