We introduce (and test on real data) a new method based on Machine Learning techniques to quantitatively analyse observed microlensing light curves of lensed quasars. The method is aimed at providing a fast and robust procedure to estimate physical parameters from observed light curves, in order to be easily applied to the large quantities of light

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