Over the past decade, observations of the cool interstellar medium (ISM) in distant galaxies
via molecular and atomic fine structure line (FSL) emission have gone from a curious look …

Giant molecular clouds (GMCs) and their stellar offspring are the building blocks of galaxies.
The physical characteristics of GMCs and their evolution are tightly connected to galaxy …

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

It remains a major challenge to derive a theory of cloud-scale (pc) star formation and
feedback, describing how galaxies convert gas into stars as a function of the galactic …

As they grow, galaxies can transition from irregular/spheroidal with 'bursty'star formation
histories (SFHs), to discy with smooth SFHs. But even in simulations, the direct physical …

We present the KMOS 3D survey, a new integral field survey of over 600 galaxies at 0.7< z<
2.7 using KMOS at the Very Large Telescope. The KMOS 3D survey utilizes synergies with …

There is a large consensus that gas in high-z galaxies is highly turbulent, because of a
combination of stellar feedback processes and gravitational instabilities driven by mergers …

We measure the velocity dispersion, σ, and surface density, Σ, of the molecular gas in
nearby galaxies from CO spectral line cubes with spatial resolution 45–120 pc, matched to …

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 …

We present an end-to-end, two-phase model for the origin of globular clusters (GCs). In the
model, populations of stellar clusters form in the high-pressure discs of high-redshift (z> 2) …