In this talk we will discuss host galaxy observations of Fast X-ray Transients (FXTs). FXTs are minute-to-hours long flashes of X-rays, discovered serendipitously in X-ray satellite data (mainly Chandra and XMM-Newton) and they have been associated with energetic extra-galactic phenomena. However, their exact nature has not yet been established

Spectral energy distributions (SEDs) encode information about the stellar populations within galaxies. By investigating the properties of these stars, such as their ages, masses, and metallicities, we can gain insights into the underlying physical processes that drive the growth and transformation of galaxies over cosmic time. For this purpose, we

Context: Bar formation and merger events can contribute to the rearrangement of stars within the Galaxy in addition to triggering star formation (SF) epochs. Super-metal-rich (SMR) stars found in the solar neighbourhood (SNd) can be used as tracers of such events as they are expected to originate only in the inner Galaxy and to have definitely

The application of cross-correlation techniques to JWST transmission spectra has opened an alternate pathway to study exoplanet atmospheres with JWST observations, which will contribute to pave the road for the first atmospheric studies with ELTs. JWST observed for the first time the hot-Jupiter WASP-39b on July 2022 as part of the JWST Transiting

Observational and theoretical evidence supports the idea that the influence of supermassive black hole growth on galaxies extends from the central tens of parsecs (localised, transient impact) to hundreds of kiloparsecs (global, long-term impact). Because of the completely different scales of these localised and global effects on the host galaxies

According to dynamo theory, stars with convective envelopes efficiently generate surface magnetic fields, which manifest as magnetic activity in the form of starspots, faculae, and/or flares, when their rotation period is shorter than their convective turnover time. Most red giants, having undergone significant spin down while expanding, have slow