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 …

The existence of∼ 109M⊙ supermassive black holes (SMBHs) within the first billion years
of the Universe has stimulated numerous ideas for the prompt formation and rapid growth of …

We describe the 2017 release of the spectral synthesis code CLOUDY, summarizing the
many improvements to the scope and accuracy of the physics which have been made since …

Galaxy formation is at the heart of our understanding of cosmic evolution. Although there is a
consensus that galaxies emerged from the expanding matter background by gravitational …

The formation of the first galaxies during cosmic dawn and reionization (at redshifts z= 5–
30), triggered the last major phase transition of our universe, as hydrogen evolved from cold …

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 …

We propose a set of standard assumptions for the modelling of Class II and III protoplanetary
disks, which includes detailed continuum radiative transfer, thermo-chemical modelling of …

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 simulate the growth of a Population III stellar system, starting from cosmological initial
conditions at z= 100. We follow the formation of a minihalo and the subsequent collapse of …