Atomic hydrogen (Hi) is a critical stepping stone in the gas evolution cycle of the interstellar
medium (ISM) of the Milky Way. Hi traces both the cold, premolecular state before star …

We present a new cosmological, magnetohydrodynamical simulation for galaxy formation:
TNG50, the third and final instalment of the IllustrisTNG project. TNG50 evolves 2× 21603 …

Hydrodynamical cosmological simulations are increasing their level of realism by
considering more physical processes and having greater resolution or larger statistics …

We introduce a new model for the structure and evolution of the gas in galactic discs. In the
model the gas is in vertical pressure and energy balance. Star formation feedback injects …

The first JWST observations of nearby galaxies have unveiled a rich population of bubbles
that trace the stellar-feedback mechanisms responsible for their creation. Studying these …

We compare the observed turbulent pressure in molecular gas, P turb, to the required
pressure for the interstellar gas to stay in equilibrium in the gravitational potential of a …

We review the role that magnetic field may have on the formation and evolution of molecular
clouds. After a brief presentation and main assumptions leading to ideal MHD equations …

Dusty star-forming galaxies at high redshift (1< z< 3) represent the most intense star-forming
regions in the universe. Key aspects to these processes are the gas heating and cooling …

The Evolution and Origin of Ionized Gas Velocity Dispersion from z ∼ 2.6 to z ∼ 0.6 with
KMOS3D - IOPscience This site uses cookies. By continuing to use this site you agree to our …

We present magnetohydrodynamic (MHD) simulations of the star-forming multiphase
interstellar medium (ISM) in stratified galactic patches with gas surface densities Σgas= 10 …