The first generation of stars, often called Population III (or Pop III), form from metal-free
primordial gas at redshifts z∼ 30 and below. They dominate the cosmic star-formation …

Over the past decade, increasingly robust estimates of the dense molecular gas content in
galaxy populations between redshift z= 0 and the peak of cosmic galaxy/star formation (z∼ …

One characteristic trait of space plasmas is the multi-scale dynamics resulting from non-
linear transfers and conversions of various forms of energy. Routinely evidenced in a range …

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

Numerical simulations have become a major tool for understanding galaxy formation and
evolution. Over the decades the field has made significant progress. It is now possible to …

In the past twenty years, the reconnaissance of 12CO and 13CO emission in the Milky Way
by single-dish millimeter-wave telescopes has expanded our view and understanding of …

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 …

Outflows from accreting, rotating, and magnetized systems are ubiquitous. Protostellar
outflows can be observed from radio to X-ray wavelengths in the continuum and a multitude …

We review current understanding of star formation, outlining an overall theoretical framework
and the observations that motivate it. A conception of star formation has emerged in which …

We survey the theory and experimental tests for the propagation of cosmic rays in the Galaxy
up to energies of 1015 eV. A guide to the previous reviews and essential literature is given …