We present the Oscillating Stars with wIneRed near-Infrared Spectroscopy (OSIRIS) project, aimed at deriving accurate chemical abundances of primary distance indicators covering a wide age range from young Classical Cepheids to intermediate-age Anomalous Cepheids and Miras, old RR Lyrae stars, and Type-II Cepheids. High-resolution near-infrared

The James Webb Space Telescope offers astronomers the opportunity to observe the composition, structure, and dynamics of transiting exoplanet atmospheres with unprecedented detail. However, such observations require very precise time-series spectroscopic monitoring of bright stars and present unique technical challenges. The Transiting Exoplanet

This paper is the first in a series of two that deals with the physical and numerical grounds of stellar atmospheres modelling. After a phenomenological definition of a star and a stellar atmosphere, the physics that shapes the stellar atmosphere physical system is discussed and three alternative pictures are considered for its representation.

Post-starburst galaxies can be identified via the presence of prominent Hydrogen Balmer absorption lines in their spectra. We present a comprehensive study of the origin of strong Balmer lines in a volume-limited sample of 189 galaxies with 0.01 z 0.05, log (M_{\star }/M_{⊙})>9.5 and projected axial ratio b/a > 0.32. We explore their structural

For the same stellar mass, physically smaller star-forming galaxies are also metal richer. What causes the relation remains unclear. The central star-forming galaxies in the EAGLE cosmological numerical simulation reproduce the observed trend. We use them to explore the origin of the relation assuming that the physical mechanism responsible for the

We present the first proper motion measurement for an ultra-faint dwarf spheroidal galaxy, Segue 1, using data from the Sloan Digital Sky Survey (SDSS) and the Large Binocular Camera (LBC) as the first and second epochs separated by a baseline of ∼10 years. We obtain a motion of μ α cos(δ) = ‑0.37 ± 0.57 mas yr‑1 and μ δ = ‑3.39 ± 0.58 mas yr‑1