NGC 7293, the Helix nebula, represents one of the rare instances in which theoretical predictions of stellar evolution can be accurately tested against observations since the precise parallax distance and the velocity and proper motion of the star are well known. We present numerical simulations of the formation of the Helix PN that are fully

Recent integral-field spectroscopy observations have revealed that thick- and thin-disk star-formation histories are regulated by the interplay of internal and external processes. We analyze stellar-population properties of 24 spiral galaxies from the AURIGA zoom-in cosmological simulations, to offer a more in-depth interpretation of observable

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