Recent Talks

El Telescopio Solar Europeo espera alcanzar el diseño preliminar de todo el telescopio en 2023. Algunos subsistemas han pasado la Revisión de Diseño Preliminar (PDR) como es el caso de la Estructura del Telescopio, la Cubierta y Pilar, subsistemas en los que se centrará este seminario repasando su estado actual y sus prestaciones principales, así como los análisis y test con los que se han comprobado dichas prestaciones.

Enlace de youtube:

https://youtu.be/o9UwtmJL1IY

The formation of the first galaxies in the Universe is the new frontier of both galaxy formation and reionization studies. In fact, we will soon directly observe primeval galaxies thanks to the James Webb Space Telescope, and witness the reionization process through 21cm intensity mapping experiments. This unique moment in human history creates a fierce new challenge, i.e. to simultaneously understand in a unique and coherent picture the processes of galaxy formation and reionization, and – crucially – their connection. The latter, in particular, has escaped past numerical efforts. In this talk I will present the first results on this front from an years-long effort geared toward achieving such comprehensive picture, culminated in the Thesan suite of cosmological radiation-magneto-hydrodynamical simulations. I will briefly introduce the features of Thesan, highlighting the successes and failures of its physical model. Thesan produces realistic galaxy populations thanks to state-of-the-art physics, including self-consistent dust production+destruction and radiation transport. I will then show how Thesan can, for the first time, reproduce the connection between IGM and galaxies, as measured from the modulation of the Lyman-alpha flux around galaxies. Finally, I will chart the way forward towards and even deeper understanding of the emergence of the first structures in the Universe.

En esta sesión, cada uno/a de los/as becarios/as de desarrollo tecnológico de la convocatoria de 2022 hará una breve exposición del trabajo realizado durante los tres meses de duración de la beca:

10.00 - 10.10: Diego Portero Rodriguez: "Diseño de un circuito integrado analógico con una tecnología microelectrónica CMOS"

10.10 - 10.20: Elena Reyes Rodriguez: “Desarrollo y diseño óptico de un sistema de comunicaciones ópticas de distribución de clave cuántica QKD en protocolo BB 84 y un sistema de comunicaciones ópticas clásicas”

10.20 - 10.30:  Sara Muñoz Torres: “ Puesta en funcionamiento, pruebas y puesta a punto del sistema de adquisición de datos (SAD) para detectores MKIDs de LISA”

10.30 - 10.40: Daniel Pascual Rios: “Diseño, fabricación e integración del espectrómetro de microondas de Tenerife (TMS) y montaje, integración, verificación y comisionado del instrumento multifrecuencias mejorado (MFI2), que operaran en condiciones ambientales y criogénicas"

10.40 - 10.50: Guillermo Fuentes Morales: “Diseño del software para la simulación de la estrategia de optica adaptativa del telescopio solar europeo"

10.50 - 11.00: Victoria Vera Cañete: “Calibración de dos maquinas de recubrimientos ópticos del IAC"

11.00 - 11.10: Carlos Marrero De la Rosa: “Desarrollo de software de un modulo procesado para la utilización de la cámara plenóptica en óptica adaptativa, que se integre en el simulador DASP y en el controlador de tiempo real DARC”

Massive stars (at least eight times as massive as the Sun) possess strong stellar winds driven by radiation. With the advent of the so called MiMeS collaboration, an increasing number of these massive stars have been confirmed to have global magnetic fields. Such magnetic fields can have significant influence on the dynamics of these stellar winds which are strongly ionized. Such interaction of the wind and magnetic field can generate copious amount of X-rays, they can spin the star down, they can also help form large scale disk-like structures. In this presentation I will discuss the nature of such radiatively-driven winds and how they interact with magnetic fields.

https://youtu.be/jKmifm17bno

The first Gigayears of our Galactic halo can be probed by using ancient stellar populations as traced by RR Lyrae stars. Today, with the advancement in our knowledge of RR Lyrae properties belonging to the Halo and to Milky Way satellite systems (Globular clusters and dwarf galaxies) we are able
to provide solid constraints on the link between these stellar systems. Here, we present some recent results concerning the Halo formation by using a detailed evolutionary analysis of RR Lyrae stars for which chemical abundances are available.

Cosmological observations (redshifts, cosmic microwave background radiation, abundance of light elements, formation and evolution of galaxies, large-scale structure) find explanations within the standard Lambda-CDM model, although many times after a number of ad hoc corrections. Nevertheless, the expression ‘crisis in cosmology’ stubbornly reverberates in the scientific literature: the higher the precision with which the standard cosmological model tries to fit the data, the greater the number of tensions that arise. Moreover, there are alternative explanations for most of the observations. Therefore, cosmological hypotheses should be very cautiously proposed and even more cautiously received.

There are also sociological and philosophical arguments to support this scepticism. Only the standard model is considered by most professional cosmologists, while the challenges of the most fundamental ideas of modern cosmology are usually neglected. Funding, research positions, prestige, telescope time, publication in top journals, citations, conferences, and other resources are dedicated almost exclusively to standard cosmology. Moreover, religious, philosophical, economic, and political ideologies in a world dominated by anglophone culture also influence the contents of cosmological ideas.

Astrophysical observations at (sub)mm wavelengths (from ~300 micron to ~3mm)
allow us to study the cold and dense material in the Universe, hence probing
the formation of stars and planets, and the interstellar and circumgalactic
medium within galaxies across cosmic time. The current generation of
15m-class single-dish telescopes has delivered some of the first surveys at
(sub)mm wavelengths, allowing to go far beyond the previously optical-biased
view of the Universe. Follow-up observations with interferometers then
revealed in exquisite detail the morphology and kinematics of such (sub)mm
sources. However, it is now clear that without a transformative change in
the capabilities of single-dish facilities in the 2030s, interferometers
will soon become source-starved. The current generation of 15m-class single-
dish telescopes, with their limited fields of view, spatial resolutions, and
sensitivities, can only reveal the "peak of the iceberg" of the (sub)mm
source population, both for Galactic and extragalactic studies. These
limitations cannot be fully mitigated by interferometers, which are all
intrinsically affected by a low mapping speed and by the loss of diffuse
extended signals. The Atacama Large Aperture Submillimeter telescope
(AtLAST) project is a concept for a 50m diameter single dish observatory to
be built near the ALMA site. With its extremely large field of view (the goal
is ~2 degrees), spatial resolution (up to ~1'' at 350 micron) and sensitivity
to both point sources and large-scale structures, AtLAST will be
transformational for all fields of astronomy in the 2030s. In this talk I
will describe the EU Horizon2020-funded project that aims to deliver a
comprehensive design study for such a next-generation single-dish facility.

We present a sample of 734 ultracool dwarfs using LAMOST DR7 spectra, i.e.,  those having a spectral type of or later than M6, including an L0.  All of these red or brown dwarfs are within 360 pc, with a Gaia G magnitude brighter than 19.2 mag, a BP-RP color redder than 2.5 mag  and an absolute G magnitude fainter than 9 mag. Their stellar parameters  (Teff, log g, and [M/H]) are consistent with being the Galactic thin-disk  population, which is further supported by their kinematics using LAMOST radial velocity plus Gaia proper motion and parallax.  A total of 77 are detected  with the lithium absorption line at 6708 A, signifying youth and substellar nature. We report on their kinematic ages estimated by the velocity dispersion. Thirty five close pairs are identified, of which the binarity of six is discovered for the first time.

With the aim of detecting cosmological gas accretion onto galaxies of the local Universe, we examined the Ha emission in the halo of the 164 galaxies in the field of view of MUSE-Wide (Urrutia+19) with observable Ha (redshift < 0.42).  An exhaustive screening of the Ha images led us to select 118 reliable Ha emitting gas clouds. To our surprise, around 38 % of the time the Ha line profile shows a double peak centered at the rest-frame of the corresponding galaxy. We have explored several physical scenarios to explain this Ha emission, among which accretion disks around rogue  intermediate mass black holes (IMBHs) fit the observations best. I will describe the data analysis (to discard, e.g, instrumental artifacts and high redshift interlopers), the properties of the Ha emitting clumps (their fluxes, peak separation, and spatial distribution with respect to the central galaxy), and the arguments leading to the IMBH hypothesis rather than other alternatives (e.g., cosmological gas, expanding bubbles, or shocks in the circum galactic medium).