Últimas charlas

The Javalambre Photometric Local Survey (J-PLUS) is an ongoing 12-band photometric optical survey, observing thousands of square
degrees of the Northern hemisphere from the dedicated JAST/T80 telescope at the Observatorio Astrofísico de Javalambre.
The larger field of view (FoV), high spatial resolution, contiguous narrow band filters cover a wide wavelength (330-1100 nm)
of J-PLUS/J-PAS surveys act like a low resolution IFU, which is suitable for spatially resolved studies of galaxies. J-surveys have
large Field of view (FoV) and can offer large contiguous observing areas to understand the complete structure of all galaxies
and trace their environment without any pre-selection. In my talk, I will present the results from the spatially resolved study of Halpha 
emission line maps of nearby galaxies at z < 0.017 using JPLUS DR3. We validate our method to build the J-PLUS IFU (J-IFU) emission line maps 
with other IFUs such as CALIFA, MANGA and MUSE. I will also present spatially resolved star-forming regions, its photospectra and star formation maps 
of JPLUS galaxies.

Diseño, construcción y primera luz del EMO-1, un observatorio casero con estación meteorológica integrada, monitoreo permanente del cielo y colaboración científica.

Youtube:
https://youtube.com/live/0PFICuLjOAE?feature=share

En esta charla se va a presentar los telescopios ATLAS y su integración en la red ATLAS dirigida por la Universidad de Hawaii. Vamos a hablar del estado actual del proyecto, tecnología que se utiliza en los telescopios y el stack software que lleva asociado.

Link Youtube:

https://youtube.com/live/37xMArgvyfI?feature=share

In the field of modern cosmological studies, we like to think that we live in an era of "precision cosmology." However, our understanding of matter distribution on small scales is not quite there yet. This limitation stems from the feedback effects of supernovae and supermassive black holes, which alter the matter distribution on scales smaller than a few Mpc and impact star formation and galaxy evolution. I will discuss how surveys such as Subaru-PFS and DESI will enhance our understanding of the Universe's matter distribution. By observing galaxies and AGNs, we can infer the distribution of dark matter, gas, and metals with the support of theoretical modeling and numerical simulations. Specifically, I will explain how we can tighten the constraints on matter distribution on small scales and further refine our understanding of the Lambda-CDM model through IGM/CGM tomography and Lyman-alpha forest analysis. 

Activity of cool dwarf stars can reveal itself in the form of high-energy radiation (eg, enhanced X-ray coronal emission, flares) and particles (eg, winds, coronal mass ejections). Together, these phenomena shape the space weather around (exo)planets. Because most of the known exoplanets have significantly closer orbital distances than solar system planets, they are often embedded in much harsher particle and radiation environments, leading to stronger interactions between the exoplanet and its surrounding environment. In this talk I will present an overview of how stellar activity and outflows can induce and shape atmospheric escape in exoplanets. I will focus mostly on close-in gas giant planets, whose escaping atmospheres are somewhat easier to observe. I will then discuss how the observability of atmospheric escape, through spectroscopic transits, evolve on billions of years timescales.

The coupling between the baryonic cycle of galaxies and dark matter halo assembly is central to our understanding of galaxies, and yet, it remains a challenge for theoretical models and elusive to observations. In this talk, I report observational evidence demonstrating that different baryonic properties of nearby galaxies are controlled by their host halos. We map galaxy ages, metallicities and star formation histories across the stellar-to-halo mass relation for SDSS central galaxies using absorption optical spectra. In addition to stellar populations, we also investigate the stellar angular momentum, star formation rates and galaxy morphology across the stellar-to-total dynamical mass relation for CALIFA galaxies. We find that the scatter of both relations correlates with these galaxy properties, which are determined by the combined role of stellar and halo/total mass. Galaxies become older, more metal-rich and less rotationally supported, form the bulk of their stars earlier on and faster, have lower star formation rates and earlier-type morphologies as their stellar mass increases (at fixed halo/total mass). Furthermore, we also observe that the scatter of the star-forming main sequence is driven by galaxies that have experienced different evolutionary histories. We interpret our results as being driven by halo evolution, with galaxies/halos at different evolutionary stages modulating the variety of galaxy properties observed at fixed stellar mass. Our findings call for a revision of the sub-grid physics implementation in cosmological numerical simulations, in particular during the early stages of galaxy formation, and warn observational studies to account for the profound effect that halo formation time may have on measured galaxy properties.

Zoom Link: https://rediris.zoom.us/j/96210828127?pwd=Z25JdFg1bnpRTVBSQUdpTVlwUDgyQT09

El objetivo de esta charla es presentar los recientes avances del sistema de Óptica Adaptativa de GTC (GTCAO). Se resumirán los resultados de las pruebas de aceptación en la sala AIV en abril de 2023; las dificultades y el éxito del transporte al ORM y la instalación en GTC en junio de 2023; la integración del sistema con el control del telescopio y los primeros resultados de las campañas de commissioning en cielo. Se repasará también brevemente el estado del resto de proyectos del programa, en concreto el sistema de Estrella Guía Láser y el instrumento GRANCAIN.

Youtube: https://youtube.com/live/T1TQNju3eEw

Zoom link: https://rediris.zoom.us/j/99761131815?pwd=QUN0ckRSZWJZQkh1aUxvSU9UNmtJUT09
Meeting ID: 997 6113 1815

Passcode: 164994