Hydrodynamic simulations of black hole evolution in AGN discs II: inclination damping for partially embedded satellites
Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 543:4 (2025) 3768-3782
Abstract:
PowerBin: Fast Adaptive Data Binning with Centroidal Power Diagrams
Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2025) staf1726
Abstract:
High-Order Stellar Kinematic in MaNGA integral-field spectroscopy survey: classification, stellar population, and the impact of galaxy bars and mergers
Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2025) staf1760
Abstract:
Impact of Cosmic Ray-driven Outflows on Ly α Emission in Cosmological Simulations
The Astrophysical Journal American Astronomical Society 992:1 (2025) 67
Abstract:
Cosmic ray (CR) feedback has been proposed as a powerful mechanism for driving warm gas outflows in galaxies. We use cosmological magnetohydrodynamic simulations to investigate the impact of CR feedback on neutral hydrogen (H i) in a 1011 M⊙ dark matter halo at 2 < z < 4. To this end, we postprocess the simulations with ionizing radiative transfer and perform Monte Carlo Lyman-α (Lyα) transfer calculations. CR feedback reduces H i column densities around young stars, thereby allowing more Lyα photons to escape and consequently offering a better match to the Lyα luminosities of observed Lyα emitters. Although galaxies with CR-driven outflows have more extended H i in the circumgalactic medium, two Lyα line properties sensitive to optical depth and gas kinematic—the location of the red peak relative to the Lyα line center in velocity space (vred) and relative strength of the blue-to-red peaks (B/R)—cannot distinguish between the CR-driven and non-CR simulations. This is because Lyα photons propagate preferentially along low H i density channels created by the ionizing radiation, thereby limiting the scattering with volume-filling H i. In contrast, the observed low flux ratios between the valley and peak and the surface brightness profiles are better reproduced in the model with CR-driven outflows because the Lyα photons interact more before escaping, rather than being destroyed by dust as is the case in the non-CR simulation. We discuss the potential cause of the paucity of sightlines in simulations that exhibit prominent red peaks and large vred, which may require the presence of more volume-filling H i.The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. I. Highly Ionized Gas
The Astrophysical Journal American Astronomical Society 992:1 (2025) 48