collaborators

11 papers

astro-ph.GA2026

Kennicutt-Schmidt relation of galaxies over 13 billion years in the COLIBRE hydrodynamical simulations

Claudia del P. Lagos, Joop Schaye, Matthieu Schaller +16

We investigate the correlation between star formation rate (SFR) surface density and gas surface density (known as the Kennicutt-Schmidt, KS, relation) at kiloparsec (kpc) scales a…

astro-ph.GA2026

Weighing gas-rich starless halos: dark matter parameters inference from their gas distributions

Francesco Turini, Alejandro Benitez-Llambay

Reionization-Limited Clouds (RELHICs) are starless dark matter halos retaining a significant neutral hydrogen( ) reservoir. The gas resides in near hydrostatic equil…

astro-ph.GA2026

A subgrid model for chemical enrichment in cosmological simulations

Camila A. Correa, Joop Schaye, Matthieu Schaller +6

We present the modules for stellar nucleosynthesis, stellar mass loss, and turbulent diffusion of the new COLIBRE subgrid model for cosmological hydrodynamical simulations of galax…

astro-ph.GA2026

Dynamical disequilibrium in dwarf galaxies: rethinking gas dynamics, rotation curves, and dark matter inference

Diego Dado, Kyle A. Oman, Katherine E. Harborne +9

We quantify departures from hydrodynamical and centrifugal equilibrium in the gas discs of low-mass () galaxies from the COLIBR…

astro-ph.GA2026

Non-explosive pre-supernova feedback in the COLIBRE model of galaxy formation

Alejandro Benítez-Llambay, Sylvia Ploeckinger, Joop Schaye +7

We present the implementation and testing of a subgrid non-explosive pre-supernova (NEPS) feedback module for the COLIBRE model of galaxy formation. The NEPS module incorporates th…

astro-ph.GA2026

Modelling the evolution and influence of dust in cosmological simulations that include the cold phase of the interstellar medium

James W. Trayford, Joop Schaye, Camila Correa +7

While marginal in mass terms, dust grains play an outsized role in both the physics and observation of the interstellar medium (ISM). However, explicit modelling of this ISM consti…