How do galaxies shape their morphology through time? How many details of galaxies at cosmic noon are we going to unveil? This contribution aims at presenting the expected performance of JWST imaging observations in constraining the evolution of galaxies and the origin of the Hubble sequence. In particular, I describe NIRCam mock observations of

We present the results recently published by https://doi.org/10.1051/0004-6361/202141980 {Marfil et al. (2021, A&A, 656, A162)} regarding the determination of the stellar atmospheric parameters ($T_{\rm eff}$, $\log{g}$, and [Fe/H]) of 343 M dwarfs observed with CARMENES. We employed SteParSyn, a Bayesian spectral synthesis implementation

Extreme Emission Line Galaxies (EELGs) are characterized by their compact sizes and very high equivalent widths of certain optical emission lines (e.g. EW([OIII]) $>$ 500Å), indicative of very high specific star formation rates, similar to those detected in the reionization epoch galaxies. Many of them also present certain high-excitation emission

Luminous red novae (LRNe) are transients characterized by low luminosities and expansion velocities, and they are associated with mergers or common-envelope ejections in stellar binaries. Intermediate-luminosity red transients (ILRTs) are an observationally similar class with unknown origins, but they are generally believed to be either electron

FastCam is an instrument designed to obtain high spatial resolution images in the optical wave- length range from ground-based telescopes by using the Lucky Imaging technique. This technique is based on the idea of registering the instants of atmospheric stability, typically lasting just some milliseconds, using very short exposures. The instrument

Context The origin of phosphorus, one of the essential elements for life on Earth, is currently unknown. Prevalent models of Galactic chemical evolution (GCE) systematically underestimate the amount of P compared to observations, especially at low metallicities. The recently discovered P-rich ([P/Fe] ≳ 1.2 dex) and metal-poor ([Fe/H] ≃ −1.0 dex)