In this work we used a series of open clusters and associations observed by the Gaia-ESO Survey (GES) to study the use of lithium abundances (Li I spectral line at 6708 $\angstrom$) as an age indicator for pre- and main-sequence FGKM late-type stars. Previous studies of open clusters have shown that lithium depletion is not only strongly age

OTELO is an ultradeep, 2D-spectroscopic (R$\sim$700) blind survey, defined on a window of 210 Å centred at 9175 Å targeting a region of the Extended Groth Field that is embedded in the Deep field 3 of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS). Is the deepest pointing of GALEX in imaging and spectroscopy. Such Pseudo-spectra(PS) were

In this contribution, we present the results of a study on the high abundance discrepancy factor (ADF $\sim$ 10) planetary nebula (PN) NGC 6153 with MUSE. We have constructed flux maps for dozens of emission lines, that allowed us to build spatially resolved maps of extinction, electron temperature ($T_{\rm e}$), electron density ($n_{\rm e}$), and

Disc galaxies are complex systems shaped by different stellar structures such as bulges, discs, and bars. Every galaxy structure keeps a unique memory of their past evolution, thus, understanding the mass assembly of disc galaxies can only be achieved by analysing separately all these independent footprints of past evolution. In this work, we have

The Isaac Newton Group of Telescopes is completing a strategic change for the scientific use of its two telescopes, the 4.2-m William Herschel Telescope (WHT) and the 2.5-m Isaac Newton Telescope (INT). After more than 30 years operating as multi-purpose telescopes, the telescopes will soon complete their shift to nearly-single instrument operation

The Cherenkov Telescope Array (CTA) will be the next generation ground-based very-high-energy (VHE) gamma-ray observatory. The first of the Large Size Telescopes (LST1), is already under commissioning at Roque de los Muchachos observatory, in La Palma. The unprecedented sensitivity at short timescales of CTA will make of this observatory the