From protogalaxy through thick and thin: Why did the Milky Way evolve in three kinematic phases?
Abstract
APOGEE and Gaia data suggest the Milky Way's kinematic structure evolved through three distinct phases: a disordered protogalaxy, which ``spun up'' into a thick stellar disk, and then ``cooled down'' to a final cold, thin stellar disk. We use a suite of FIRE-2 cosmological zoom-in simulations of Milky Way-mass galaxies to demonstrate that the same three phases arise in simulations, and we study their physical origin. In our simulations, the early protogalaxy phase occurs when the rate of cool gas (T ≤ 104 K) converting into stars is low, star formation is bursty, and the baryonic mass ``sloshes'' within the host potential with respect to the center of mass. The gas begins to spin coherently after sloshing ends, followed by the spin-up of young stars. The central potential is least concentrated just prior to gas spin-up. This second, thick disk phase coincides with the highest rate of cool gas converting into stars, though star formation remains bursty. The final transition to the thin disk phase occurs when the inner circumgalactic medium virializes, and is associated with steady star formation and intermediate consumption rates of cool gas converting into stars. Mergers do not appear to play a defining role in driving transitions between the three phases. The condition for thick disk formation appears to be minimal: a stable center of mass motion. Thin disk formation requires more: gas must accrete slowly enough for its angular momentum to mix and become coherent prior to joining the galaxy.
Related
- Model-Independent Measurement of Baryon Gas Fractions through Galaxy-Galaxy Lensing and the Kinematic Sunyaev-Zel'dovich Effect
- PRISMS/U13151. A Glimpse into the Earliest Phases of Galaxy Formation through an Ultra-Faint System ≈ 500 Myr after the Big Bang
- The X-ray--UV relation does not evolve in homogeneous quasar samples
- Dissecting the 3D chemo-dynamical structures of NGC 1381: A galaxy hosting an ancient slow bar with an accretion-related bulge and thick disc
- Shadow and Polarized Images of Schwarzschild-MOG Black Hole Illuminated by Thick Accretion Disk
BibTeX
@misc{myrtaj2026from,
title = {{From protogalaxy through thick and thin: Why did the Milky Way evolve in three kinematic phases?}},
author = {Olti Myrtaj and James S. Bullock and Michael Boylan-Kolchin and Vedant Chandra and Claude-André Faucher-Giguère and Robert Feldmann and Francisco J. Mercado and Jorge Moreno and Jonathan Stern and Andrew Wetzel and Pratik J. Gandhi and Luke Xia},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2605.22806},
eprint = {2605.22806},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2605.22806},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - From protogalaxy through thick and thin: Why did the Milky Way evolve in three kinematic phases?
AU - Olti Myrtaj
AU - James S. Bullock
AU - Michael Boylan-Kolchin
AU - Vedant Chandra
AU - Claude-André Faucher-Giguère
AU - Robert Feldmann
AU - Francisco J. Mercado
AU - Jorge Moreno
AU - Jonathan Stern
AU - Andrew Wetzel
AU - Pratik J. Gandhi
AU - Luke Xia
PY - 2026
DA - 2026/10/08
PB - arXiv
DO - 10.48550/arxiv.2605.22806
UR - https://arxiv.org/abs/2605.22806
AB - APOGEE and Gaia data suggest the Milky Way's kinematic structure evolved through three distinct phases: a disordered protogalaxy, which ``spun up'' into a thick stellar disk, and then ``cooled down'' to a final cold, thin stellar disk. We use a suite of FIRE-2 cosmological zoom-in simulations of Milky Way-mass galaxies to demonstrate that the same three phases arise in simulations, and we study their physical origin. In our simulations, the early protogalaxy phase occurs when the rate of cool gas (T ≤ 10^4 K) converting into stars is low, star formation is bursty, and the baryonic mass ``sloshes'' within the host potential with respect to the center of mass. The gas begins to spin coherently after sloshing ends, followed by the spin-up of young stars. The central potential is least concentrated just prior to gas spin-up. This second, thick disk phase coincides with the highest rate of cool gas converting into stars, though star formation remains bursty. The final transition to the thin disk phase occurs when the inner circumgalactic medium virializes, and is associated with steady star formation and intermediate consumption rates of cool gas converting into stars. Mergers do not appear to play a defining role in driving transitions between the three phases. The condition for thick disk formation appears to be minimal: a stable center of mass motion. Thin disk formation requires more: gas must accrete slowly enough for its angular momentum to mix and become coherent prior to joining the galaxy.
ER -