The stellar mass – halo mass relationship is a fundamental scaling relationship connecting galaxies from dwarfs to giants to their dark matter halos. This relationship is currently key to our understanding of the complex interplay between the many modes of feedback (e.g., stellar winds, supernovae, AGN) and star formation in galaxies. However

In this seminar I will focus on how the avalanche of new data changes our views on how our Galaxy formed and evolved. Precise astrometric, spectroscopic, photometric and asteroseismic data can be combined to pin down different processes that have shaped the Milky Way. This data will be discussed and illustrated with examples of what is possible to

H II regions, ionized nebulae associated to massive star formation, exhibit a wealth of emission lines that are the fundamental basis for estimating the chemical composition of the Universe. For more than 80 years, a discrepancy of a factor of around two between heavy-element abundances derived with collisional excited lines (CELs) and the weaker

TFG sobre la aplicación de técnicas de aprendizaje automático para la predicción de la temperatura de punto de rocío y su implementación de el Sistema de Control de Telescopios Nocturnos del Observatorio del Teide Unirse a la reunión Zoom: https://rediris.zoom.us/j/83867830718 Youtube: https://youtube.com/live/db8r16OWqL8?feature=share

Extremely metal-poor or zero-metallicity very massive stars, with initial mass in the range 100 ≲ Mi/M⊙ ≲ 1000, have a broad astrophysical impact. Understanding how these population III stars evolve and die has implications for several key questions, including the nature of energetic transients such as pair-instability supernovæ and gamma-ray

Se profundizará sobre las tres funcionalidades para el sistema de control del IAC80 en las que se ha trabajado durante el periodo de las prácticas externas en el IAC. Unirse a la reunión Zoom https://rediris.zoom.us/j/87219167057 ID de reunión: 872 1916 7057 Youtube https://youtube.com/live/l3J7pRrcuFc?feature=share

TBD