Galaxies on FIRE (Feedback In Realistic Environments): stellar feedback explains cosmologically inefficient star formation
Why is this work in the frame?
A frame that forgets how it found something cannot be audited. These are the routes that admitted this work.
Machine scores (provisional)
Baseline scores from an immature model (maturity gate not passed, 7 training rounds). Scores rank; they never assert a category.
The two teacher heads of the student model, read on this work. A score orders the frame for review; it never asserts a category, and the validation status ships verbatim with every row.
- Teacher spread
- 0.179 · how far apart the two teachers sit on this one work
- Validation status
score_only:v0-immature-baseline· verbatim from the scoring run: score_only means the number may rank works, and no category label ships from it
Abstract
We present a series of high-resolution cosmological simulations1 of galaxy formation to z = 0, spanning halo masses ∼108–1013 M⊙, and stellar masses ∼104–1011 M⊙. Our simulations include fully explicit treatment of the multiphase interstellar medium and stellar feedback. The stellar feedback inputs (energy, momentum, mass, and metal fluxes) are taken directly from stellar population models. These sources of feedback, with zero adjusted parameters, reproduce the observed relation between stellar and halo mass up to Mhalo ∼ 1012 M⊙. We predict weak redshift evolution in the M*–Mhalo relation, consistent with current constraints to z > 6. We find that the M*–Mhalo relation is insensitive to numerical details, but is sensitive to feedback physics. Simulations with only supernova feedback fail to reproduce observed stellar masses, particularly in dwarf and high-redshift galaxies: radiative feedback (photoheating and radiation pressure) is necessary to destroy giant molecular clouds and enable efficient coupling of later supernovae to the gas. Star formation rates (SFRs) agree well with the observed Kennicutt relation at all redshifts. The galaxy-averaged Kennicutt relation is very different from the numerically imposed law for converting gas into stars, and is determined by self-regulation via stellar feedback. Feedback reduces SFRs and produces reservoirs of gas that lead to rising late-time star formation histories, significantly different from halo accretion histories. Feedback also produces large short-time-scale variability in galactic SFRs, especially in dwarfs. These properties are not captured by common ‘sub-grid’ wind models.
Fetched live from OpenAlex and de-inverted. Abstracts are not stored in this database: the inverted indexes are 8.6 GB of the frame’s 9.3 GB of text, and the host has 13 GB free.
The record
- Venue
- Monthly Notices of the Royal Astronomical Society
- Topic
- Galaxies: Formation, Evolution, Phenomena
- Field
- Physics and Astronomy
- Canadian institutions
- Canadian Institute for Theoretical AstrophysicsUniversity of Toronto
- Funders
- Smithsonian Astrophysical ObservatorySmithsonian InstitutionUniversity of California, San DiegoJohns Hopkins UniversityAdolph C. and Mary Sprague Miller Institute for Basic Research in Science, University of California BerkeleyGordon and Betty Moore FoundationSimons FoundationCalifornia Institute of TechnologyNational Aeronautics and Space AdministrationDavid and Lucile Packard FoundationMinisterio de Ciencia e InnovaciónNational Science Foundation
- Keywords
- PhysicsAstrophysicsHaloGalaxyStar formationSupernovaAccretion (finance)RedshiftGalaxy formation and evolutionStellar massGalactic haloRadiative transferAstronomy
- Has abstract in OpenAlex
- yes