We study the temporal and spectral characteristics of the X-ray emission of the hard X-ray transient binary system IGR~J17503--2636 to characterize its variability and spectral properties. This source was observed by XMM-Newton on April 3, 2020 with an exposure time of ${\sim}27~\mathrm{ks}$. The light curves show variability on several timescales

Stars in galaxies form when baryons radiatively cool down and fall into dark matter-dominated gravitational wells. Eventually, star formation quenches as gas is depleted and/or perturbed by feedback processes that prevent the gas from collapsing and condensing. Here we report spatially resolved spectroscopic observations, using the JWST/NIRSpec

Context. We have previously studied several elements in 58 selected bulge spheroid stars, based on spectral lines in the H band. We now derive the abundances of the less studied elements phosphorus (P; Z=15), sulphur (S; Z=16), and potassium (K; Z=19). Aims. The abundances of P, S, and K in 58 bulge spheroid stars are compared both with the results

An increasing number of pulsar wind nebulae (PWNe) are being identified in the TeV band by ground-based Imaging Air Cherenkov Telescopes such that they constitute the dominant source class of Galactic TeV emitters. However, MeV–GeV PWN counterparts are still largely lacking. To date, only a dozen PWNe are identified by the Fermi–Large Area

An increasing number of pulsar wind nebulae (PWNe) are being identified in the TeV band by ground-based Imaging Air Cherenkov Telescopes such that they constitute the dominant source class of Galactic TeV emitters. However, MeV–GeV PWN counterparts are still largely lacking. To date, only a dozen PWNe are identified by the Fermi–Large Area

Context. The radial velocity (RV) method plays a key role in modern-day astrophysics. One of the most common techniques for extracting precise RVs from state-of-the-art spectrographs is template-matching (TM) algorithms. They have been shown to perform better than a cross-correlation function (CCF) approach in cases of cooler stars (e.g. M dwarfs)