The Origin of Stars in the Inner 500 Parsecs in TNG50 Galaxies

Abstract

We investigate the origin of stars in the innermost $500\mathrm{pc}$ of galaxies spanning stellar masses of $5\times 10^{8-12}{\mathrm{M}}_{\odot }$ at $\mathrm{z}=0$ using the cosmological magnetohydrodynamical TNG50 simulation. Three different origins of stars comprise galactic centers: 1) in-situ (born in the center), 2) migrated (born elsewhere in the galaxy and ultimately moved to the center), 3) ex-situ (accreted from other galaxies). In-situ and migrated stars dominate the central stellar mass budget on average with 73% and 23% respectively. The ex-situ fraction rises above 1% for galaxies $\gtrsim 10^{11}{\mathrm{M}}_{\odot }$. Yet, only 9% of all galaxies exhibit no ex-situ stars in their centers and the scatter of ex-situ mass is significant ($4-6\mathrm{dex}$). Migrated stars predominantly originate closely from the center ($1-2\mathrm{kpc}$), but if they travelled together in clumps distances reach $\sim 10\mathrm{kpc}$. Central and satellite galaxies possess similar amounts and origins of central stars. Star forming galaxies ($\gtrsim 10^{10}{\mathrm{M}}_{\odot }$) have on average more ex-situ mass in their centers than quenched ones. We predict readily observable stellar population and dynamical properties: 1) migrated stars are distinctly young ($\sim 2\mathrm{Gyr}$) and rotationally supported, especially for Milky Way mass galaxies, 2) in-situ stars are most metal-rich and older than migrated stars, 3) ex-situ stars are on random motion dominated orbits and typically the oldest, most metal-poor and $\alpha$-enhanced population. We demonstrate that the interaction history with other galaxies leads to diverse pathways of building up galaxy centers in a $\Lambda$CDM universe. Our work highlights the necessity for cosmological context in formation scenarios of central galactic components and the potential to use galaxy centers as tracers of overall galaxy assembly.

24 pages, 13 Figures, published in MNRAS

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• Disk flaring with TNG50: diversity across Milky Way and M31 analogs