Proposes heavy-element paleodetectors in lead-rich ancient minerals to detect inelastic Higgsino dark matter up to mass splittings of ~920 keV, relaxing radiopurity and depth constraints.
The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time
8 Pith papers cite this work. Polarity classification is still indexing.
8
Pith papers citing it
abstract
We introduce a suite of thirty cosmological magneto-hydrodynamical zoom simulations of the formation of galaxies in isolated Milky Way mass dark haloes. These were carried out with the moving mesh code \textlcsc{AREPO}, together with a comprehensive model for galaxy formation physics, including AGN feedback and magnetic fields, which produces realistic galaxy populations in large cosmological simulations. We demonstrate that our simulations reproduce a wide range of present-day observables, in particular, two component disc dominated galaxies with appropriate stellar masses, sizes, rotation curves, star formation rates and metallicities. We investigate the driving mechanisms that set present-day disc sizes/scale lengths, and find that they are related to the angular momentum of halo material. We show that the largest discs are produced by quiescent mergers that inspiral into the galaxy and deposit high angular momentum material into the pre-existing disc, simultaneously increasing the spin of dark matter and gas in the halo. More violent mergers and strong AGN feedback play roles in limiting disc size by destroying pre-existing discs and by suppressing gas accretion onto the outer disc, respectively. The most important factor that leads to compact discs, however, is simply a low angular momentum for the halo. In these cases, AGN feedback plays an important role in limiting central star formation and the formation of a massive bulge.
citation-role summary
method 2
citation-polarity summary
years
2026 8verdicts
UNVERDICTED 8roles
method 2polarities
use method 2representative citing papers
Deep interferometric observations of a z≈1.12 barred spiral reveal bar-driven molecular inflows at a rate matching the galaxy's star formation rate of ~36 M⊙/yr.
AuriGLOBES is a new subgrid model implemented in Auriga simulations that incorporates compressive tides and compact-object mass loss to transform an initial Schechter mass function into observed globular cluster populations while reproducing the GC system mass-halo mass relation.
Galaxy size at fixed stellar mass encodes the link between long-term gas inflow histories, current inner gas reservoirs, and metallicity via differences in assembly timing.
PRFM-vol is a new subgrid star formation model for cosmological simulations that computes SFR from ambient densities via PRFM theory and a modified effective EOS, producing taller stellar scale heights, slightly higher stellar mass, and morphology changes including Toomre-driven clumps compared to p
Manticore-Deep uses tiled Bayesian field-level inference on SDSS and BOSS data to produce posterior ensembles of 3D cosmic fields that are consistent with LCDM and validated by 7.4σ CMB lensing and 3.5σ kSZ detections.
New hydrodynamical simulations show that dwarf galaxy stellar mass-halo mass relations and star formation histories are more influenced by host halo concentration than by the 5 cMpc scale environment.
Resolved stellar property gradients in Milky Way analog progenitors show inside-out assembly with minor, temporary disruption from major mergers.
citing papers explorer
-
NOEMA$^\rm{3D}$: A deep view of cold gas flows in a barred spiral galaxy at $z\sim1$
Deep interferometric observations of a z≈1.12 barred spiral reveal bar-driven molecular inflows at a rate matching the galaxy's star formation rate of ~36 M⊙/yr.
-
Learning the Universe with PRFM-vol: Introducing a new subgrid model for star formation in cosmological simulations
PRFM-vol is a new subgrid star formation model for cosmological simulations that computes SFR from ambient densities via PRFM theory and a modified effective EOS, producing taller stellar scale heights, slightly higher stellar mass, and morphology changes including Toomre-driven clumps compared to p