We present CO (J = 1 → 0 3 → 2 5 → 4 10 → 9) and 1.2 kpc resolution [C II] line observations of the dusty star-forming galaxy (SFG) HXMM05—carried out with the Karl G. Jansky Very Large Array, the Combined Array for Research in Millimeter-wave Astronomy, the Plateau de Bure Interferometer, and the Atacama Large Millimeter/submillimeter Array

Context. The Gaia-ESO Public Spectroscopic Survey using FLAMES at the VLT has obtained high-resolution UVES spectra for a large number of giant stars, allowing a determination of the abundances of the key chemical elements carbon and nitrogen at their surface. The surface abundances of these chemical species are known to change in stars during

There are two main types of photoionized gaseous nebulae that exist in the universe: H II regions and Planetary Nebulae (PNe). They mark the endpoints of stellar evolution and understanding their composition will lead to a better understanding of stellar evolution processes and galactic chemical nucleosynthesis. Elemental abundances are estimated

Forthcoming large-scale spectroscopic surveys will soon provide data on thousands of galaxy clusters. It is important that the systematics of the various mass estimation techniques is well understood and calibrated. We compare three different dynamical mass estimators using the C-EAGLE galaxy clusters, a set of high-resolution simulations with

Context. The physical processes driving the evolution of star formation (SF) in galaxies over cosmic time still present many open questions. Recent galaxy surveys allow now to study these processes in great detail at intermediate redshift (0 ≤ z ≤ 0.5). Aims: We build a complete sample of star-forming galaxies and analyze their properties, reaching

Context. Solar active regions show a wide variety of oscillatory phenomena. The presence of the magnetic field leads to the appearance of several wave modes whose behavior is determined by the sunspot thermal and magnetic structure. Aims: We aim to study the relation between the umbral and penumbral waves observed at the high photosphere and the