FIRE-2 simulations show per-galaxy tidal disruption rates peak near z=2.5 at 4e-4 per year, correlate with SFR and central density, and remain high in satellite galaxies at early times.
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Cosmic ray transport in molecular cloud simulations boosts star formation efficiency by up to 43% and yields a top-heavier IMF with a high-mass slope shallower by ~20%.
Advection-only galactic wind models fail to reproduce observed vertical radio profiles without unrealistic velocities, synchrotron spectra are biased toward young electrons in dense regions, and bremsstrahlung/Coulomb losses cannot be neglected even when subdominant.
The cosmologically integrated neutrino emission from supermassive black hole coronae in Seyfert galaxies can account for the sub-PeV diffuse extragalactic neutrino flux observed by IceCube.
The paper identifies underproduction of oxygen in low-mass simulated dwarf galaxies as the likely cause of missing OVI in the CGM, based on comparisons across two simulation suites.
FIRE-2 simulations show that stellar radial redistribution scatter saturates at ~2 kpc for stars older than ~3 Gyr, with net orbital changes depending on age and current radius, broadly matching Milky Way observations.
Varied cosmic ray feedback models from AGN in FIRE-3 simulations all quench massive galaxies consistently with observations but produce vastly different circumgalactic medium properties.
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.
SKA-mid AA4 will enable deep, spatially resolved HI imaging over hundreds of square degrees at column densities down to 10^18 cm^{-2} to study environmental gas processes from isolated galaxies to clusters.
citing papers explorer
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TDEs on FIRE: Illuminating the Cosmic Evolution of Tidal Disruption Rates
FIRE-2 simulations show per-galaxy tidal disruption rates peak near z=2.5 at 4e-4 per year, correlate with SFR and central density, and remain high in satellite galaxies at early times.
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Gauging the Impact of Cosmic Ray Feedback on the Stellar Initial Mass Function
Cosmic ray transport in molecular cloud simulations boosts star formation efficiency by up to 43% and yields a top-heavier IMF with a high-mass slope shallower by ~20%.
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Revisiting radio synchrotron diagnostics in star-forming galaxies
Advection-only galactic wind models fail to reproduce observed vertical radio profiles without unrealistic velocities, synchrotron spectra are biased toward young electrons in dense regions, and bremsstrahlung/Coulomb losses cannot be neglected even when subdominant.
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Particle Acceleration, Coronal Neutrino Production, and the Diffuse Extragalactic Neutrino Background from Supermassive Black Holes
The cosmologically integrated neutrino emission from supermassive black hole coronae in Seyfert galaxies can account for the sub-PeV diffuse extragalactic neutrino flux observed by IceCube.
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The Simulated Oxygen Shortage (SOS): Mapping the Missing OVI in Simulated Dwarf Galaxies to Subgrid Physics
The paper identifies underproduction of oxygen in low-mass simulated dwarf galaxies as the likely cause of missing OVI in the CGM, based on comparisons across two simulation suites.
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Radial redistribution of stellar orbits in FIRE simulations of Milky-Way-mass galaxies
FIRE-2 simulations show that stellar radial redistribution scatter saturates at ~2 kpc for stars older than ~3 Gyr, with net orbital changes depending on age and current radius, broadly matching Milky Way observations.
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Effects of Varied Cosmic Ray Feedback from AGN on Massive Galaxy Properties
Varied cosmic ray feedback models from AGN in FIRE-3 simulations all quench massive galaxies consistently with observations but produce vastly different circumgalactic medium properties.
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Cosmic Rays on Galaxy Scales: Progress and Pitfalls for CR-MHD Dynamical Models
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.
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Resolved HI and Environmental Dynamics
SKA-mid AA4 will enable deep, spatially resolved HI imaging over hundreds of square degrees at column densities down to 10^18 cm^{-2} to study environmental gas processes from isolated galaxies to clusters.