@article{2b09eeeb-8c4f-48d0-9f93-4266bff8ff55,
  abstract     = {{<p>In response to recent observations from JWST and Atacama Large Millimeter Array, we explore a new class of dynamically self-consistent models that mimics a plausible progenitor of the Milky Way over a wide range of disk gas fractions, f<sub>gas</sub>. The high gas surface densities encourage vigorous star formation, which in turn couples with the gas to drive turbulence. We show that this coupling through momentum recoil drives a random walk of the baryonic potential minimum with respect to total gravitational potential, Φ<sub>tot</sub>(R, f, z). The amplitude of the bulk motion depends on the feedback strength, which in turn is directly associated with f<sub>gas</sub>. At its most extreme, when gas is the sole contributor to the disk potential (f<sub>gas</sub> = 100%), the amplitude of the walk can reach up to R ≈ 5 kpc within Φ<sub>tot</sub>. The disk dominates over dark matter (f<sub>disk</sub> ≳ 50%) within R<sub>s</sub> = 2.2R<sub>disk</sub>, where R<sub>disk</sub> is the exponential disk scale length. For a lower f<sub>disk</sub> and/or f<sub>gas</sub>, the 3D sloshing amplitude and velocity are reduced. The combination of strong feedback and sloshing leads to the newly formed stars being dynamically heated and settling to a more spatially extended disk population. The 3D heating process is roughly isotropic but its effects are more noticeable in |z| due to the initial dynamical coldness of the star-forming disk. Such a disk has enhanced [α/Fe] stellar abundances and a vertical (but no radial) gradient in stellar age and metallicity, both consistent with the Milky Way’s thick stellar disk.</p>}},
  author       = {{Bland-Hawthorn, Joss and Tepper-Garcia, Thor and Agertz, Oscar and Federrath, Christoph and Haywood, Misha and di Matteo, Paola and Bedding, Timothy R. and Tsukui, Takafumi and Wisnioski, Emily and Ness, Melissa and Freeman, Ken}},
  issn         = {{0004-637X}},
  language     = {{eng}},
  month        = {{11}},
  number       = {{1}},
  publisher    = {{American Astronomical Society}},
  series       = {{Astrophysical Journal}},
  title        = {{Turbulent Gas-rich Disks at High Redshift : Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”}},
  url          = {{http://dx.doi.org/10.3847/1538-4357/ae0931}},
  doi          = {{10.3847/1538-4357/ae0931}},
  volume       = {{994}},
  year         = {{2025}},
}