The radiation from stars and active galactic nuclei (AGNs) creates photodissociation regions
(PDRs) and X-ray-dominated regions (XDRs), where the chemistry or heating is dominated …

Far-infrared and submillimeter wavelength surveys have now established the important role
of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of …

CO line emission represents the most accessible and widely used tracer of the molecular
ISM. This renders the translation of observed CO intensity into total H2 gas mass critical to …

We review progress over the past decade in observations of large-scale star formation, with
a focus on the interface between extragalactic and Galactic studies. Methods of measuring …

The role of turbulence and magnetic fields is studied for star formation in molecular clouds.
We derive and compare six theoretical models for the star formation rate (SFR)—the …

Molecular hydrogen is the most abundant molecule in the universe. It is the first one to form
and survive photo-dissociation in tenuous environments. Its formation involves catalytic …

Understanding the physics of turbulence is crucial for many applications, including weather,
industry and astrophysics. In the interstellar medium,, supersonic turbulence plays a crucial …

Abstract The SILCC (SImulating the Life-Cycle of molecular Clouds) project aims to self-
consistently understand the small-scale structure of the interstellar medium (ISM) and its link …

Star formation lies at the center of a web of processes that drive cosmic evolution:
generation of radiant energy, synthesis of elements, formation of planets, and development …

We study the star formation efficiency (SFE) in simulations and observations of turbulent,
magnetized, molecular clouds. We find that the probability density functions (PDFs) of the …