The Gaia-Sausage-Enceladus merger occurred 11.2 ± 0.1 Gyr ago, coinciding with the formation of a group of globular clusters and potentially leaving ω Centauri as its remnant, while placing disk formation at z ≳ 4.
B., Kawata D., Gibson B
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Simulations show that observed rotation in 13.5-Gyr-old alpha-rich stars constrains the Gaia-Sausage-Enceladus merger to mass ratios below 1:4, with interaction and starburst times both near 11 Gyr.
Early kinematically persistent planes of satellite galaxies are fossil remnants of high-redshift anisotropic mass collapse along the principal directions of the local cosmic web during the fast assembly phase of host halos.
Local disk galaxies have thin vertical structures with median scale heights of 0.22 kpc and negligible flaring, consistent with the Milky Way thin disk and positively correlated with stellar mass down to 10^7 solar masses.
citing papers explorer
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The Last Galactic Firework: Timing the last significant merger with stars, globular clusters and $\omega$Centauri
The Gaia-Sausage-Enceladus merger occurred 11.2 ± 0.1 Gyr ago, coinciding with the formation of a group of globular clusters and potentially leaving ω Centauri as its remnant, while placing disk formation at z ≳ 4.
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Build-up and survival of the disc: From numerical models of galaxy formation to the Milky Way
Simulations show that observed rotation in 13.5-Gyr-old alpha-rich stars constrains the Gaia-Sausage-Enceladus merger to mass ratios below 1:4, with interaction and starburst times both near 11 Gyr.
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A statistical look on kinematic planes of satellite galaxies II: The physics behind their early formation in TNG50 MW/M31-like galaxies
Early kinematically persistent planes of satellite galaxies are fossil remnants of high-redshift anisotropic mass collapse along the principal directions of the local cosmic web during the fast assembly phase of host halos.
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Vertical Structure of Local Disk Galaxies revealed by DESI Imaging Data
Local disk galaxies have thin vertical structures with median scale heights of 0.22 kpc and negligible flaring, consistent with the Milky Way thin disk and positively correlated with stellar mass down to 10^7 solar masses.