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- W4387209854 abstract "We present a new scheme for the classification of the in-situ and accreted globular clusters (GCs). The scheme uses total energy $E$ and $z$-component of the orbital angular momentum and is calibrated using [Al/Fe] abundance ratio. We demonstrate that such classification results in the GC populations with distinct spatial, kinematic, and chemical abundance distributions. The in-situ GCs are distributed within the central 10 kpc of the Galaxy in a flattened configuration aligned with the MW disc, while the accreted GCs have a wide distribution of distances and a spatial distribution close to spherical. In-situ and accreted GCs have different $rm [Fe/H]$ distributions with the well-known bimodality present only in the metallicity distribution of the in-situ GCs. Furthermore, the accreted and in-situ GCs are well separated in the plane of $rm [Al/Fe]-[Mg/Fe]$ abundance ratios and follow distinct sequences in the age--$rm [Fe/H]$ plane. The in-situ GCs in our classification show a clear disc spin-up signature -- the increase of median $V_phi$ at metallicities $rm [Fe/H]approx -1.3div -1$ similar to the spin-up in the in-situ field stars. This signature signals the MW's disc formation, which occurred $approx 11.7-12.7$ Gyrs ago (or at $zapprox 3.1-5.3$) according to GC ages. In-situ GCs with metallicities of $rm [Fe/H]gtrsim -1.3$ were thus born in the Milky Way disc, while lower metallicity in-situ GCs were born during early, turbulent, pre-disc stages of the evolution of the Galaxy and are part of its Aurora stellar component." @default.
- W4387209854 created "2023-10-01" @default.
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- W4387209854 date "2023-09-27" @default.
- W4387209854 modified "2023-10-01" @default.
- W4387209854 title "In-situ vs accreted Milky Way globular clusters: a new classification method and implications for cluster formation" @default.
- W4387209854 doi "https://doi.org/10.48550/arxiv.2309.15902" @default.
- W4387209854 hasPublicationYear "2023" @default.
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