Combinando por primera vez datos de radiotelescopios precursores a SKA (Rotación de Faraday) con datos de Planck (efecto Sunyaev-Zeldovich), se ha detectado el campo magnético en el supercúmulo de Shapley. Mediante diferentes modelos para el campo magnético, se ha podido obtener la intensidad del mismo en el puente que une sus dos cúmulos más masivos: A3558 y A3562. 

Characterization of dwarf galaxies using AI for the ARRAKIHS mission.

In this talk, I will present the first results from MEGARA/GTC observations of the Narrow-Line Seyfert 1 (NLSy1) galaxy IRAS 17020+4544. This galaxy hosts an Ultra-Fast Outflow (UFO) detected in the X-ray band, as well as a molecular outflow. These two gas phases suggest that the outflow conserves its energy while propagating through the ISM in an 'energy-conserving regime.' Our analysis will further investigate whether this energy conservation extends to the ionized phase of the outflow. A larger sample of NLSy1 galaxies will be analyzed in future studies.

CATARSIS is a legacy project that will utilize six years of dark time from the 3.5 m telescope at Calar Alto using the TARSIS instrument. The goal of CATARSIS is to obtain unbiased 2D spectroscopy across the entire extent of a sample of 16 galaxy clusters with redshifts in the range 0.15 < z < 0.23. To optimize CATARSIS, this thesis aims to derive the mass profiles of the galaxy clusters included in the project by leveraging the advantages of hydrodynamic simulations. For this purpose, the Three Hundred simulation was used, encompassing a total of 324 clusters and 128 snapshots. To estimate the mass profiles of the clusters, the caustic method was applied, which allows mass profiles to be calculated using the line-of-sight velocities and the projected distances to the cluster center. Additionally, the limitations of the method are examined by analyzing cluster anisotropy, observational biases due to sample selection, and other factors that could significantly affect the caustic method, such as rotation and cluster substructures.

Se describe la aplicación de una técnica llamada 0-padding para la determinación de la energía de los fotones de rayos X que serán observados por el instrumento X-IFU del futuro observatorio espacial New Athena. Esta técnica permite obtener resoluciones espectrales tan buenas como las proporcionadas por métodos más tradicionales pero necesita un menor número de operaciones matemáticas, lo cual supone un importante ahorro de CPU y memoria durante la operación del instrumento en el espacio.

El estudio de las primeras galaxias que contribuyeron a la Reionización del universo será posible con un espectrógrafo de campo integral y multiobjeto como MOSAIC (con el que contribuye GUAIX), que será instalado en el Extremely Large Telescope (ELT) de 39 metros, actualmente en construcción. Como estudio piloto para ello, se está llevando a cabo un análisis bidimensional detallado de las propiedades físicas de una muestra de galaxias de baja masa (enanas) y alta formación estelar a bajo redshift. Este proyecto forma parte del programa ITP Dwarfs4MOSAIC (IP Jesús Gallego), que fue seleccionado mediante un proceso competitivo en la primavera de 2023 y ampliado en la primavera de 2024. Presentaremos los primeros resultados del procesamiento y análisis de datos de espectroscopía de campo integral bidimensional de alta resolución espectral obtenidos con MEGARA en el Gran Telescopio Canarias (GTC). Las galaxias estudiadas incluyen SBS 0335-052 W, Mrk 1486 y J1105+4444, para las cuales hemos analizado mapas bidimensionales de propiedades físicas, estructuras espaciales, propiedades cinemáticas del gas ionizado y avances en el proceso de reducción de datos.

GUAIX facts 2024.

Usando espectros y fotometría, estamos entrenando una red neuronal para predecir historias de formación estelar y evolución química. En esta presentación explico brevemente lo que hemos hecho para entrenar nuestros modelos y cómo estamos solventando el problema del "Synthetic Valley".

Se presenta un status del grupo, así como un resumen de sus recursos y obligaciones

Utilizando una simulación de un sistema galáctico similar al de la Vía Láctea, Andrómeda y satélites, se ha desarrollado un código capaz de corregir errores e inconsistencias del combo Rockstar-Consistent trees, especialmente en el caso de los mergers de halos, mediante el trackeo de las partículas de los halos fusionados. Gracias a esto, podemos obtener el tiempo de caída y de destrucción de los satélites en los "minor mergers". Ahora desarrollamos un criterio basado en el tensor de inercia de las partículas anteriormente ligadas al satélite para poder detectar las corrientes formadas durante los mergers y discernir si se han virializado con la galaxia anfitrión o no, obteniendo así el tiempo de fusión típico de un "minor merger". 

We investigate several panchromatic scaling relations (SRs) for the dwarf irregular galaxies NGC 4214, NGC 1569, NGC 3077 and the spiral NGC 2976, using IFU data from the Metal-THINGS Survey.

Among the spatially resolved properties analyzed, we explore SRs between the stellar mass, SFR, molecular gas, total gas, baryonic mass, gas metallicity, gas fraction, SFE and effective oxygen yields. Such multiwavelength SRs are analyzed at a spatial resolution of ~150-200 pc, by combining our IFU observations with data from the surveys THINGS, CARMA, HERACLES, and archival data from DustPedia. Although we recover several known relations, our slopes are different to previously reported ones.

Since we use the dust mass as a tracer of gas mass, we derive the Dust-to-Gas Ratios and the CO luminosity-to-molecular gas mass conversion factors locally, and we also explore their dependence with the metallicity. The most important result is seen for NGC 2976 in which the global shapes were recovered locally.

For first time, SRs that involve properties such as baryonic mass, effective oxygen yields, stellar mass, gas mass, SFE and gas fraction were computed locally.

Finally, a particular and detailed analysis is made for the galaxy NGC 1569, probing the level of information that can be extracted from a single galaxy.

Se hará un resumen de las actividades, capacidades y equipamiento con el que cuenta el LICA (Laboratorio de Instrumentación Científica Avanzada) así como sus planes de uso futuro. 

Se presentan las distintas iniciativas hechas por el grupo en el ámbito del estudio de la contaminación lumínica, los instrumentos desarrollados y los proyectos que las han vertebrado.

CATARSIS will survey 16 galaxy clusters in the redshift range 0.15 ≤ z ≤ 0.23 to understand the formation of structures and the evolution of galaxies in their dynamic and growing environment using TARSIS, the future wide-field Integral Field Spectrograph to be installed at the CAHA 3.5m telescope in 2028, with spectral coverage 320-810 nm and resolving power R ∼ 1000. We are collecting deep multi-wavelength optical and near-infrared imaging from existing surveys (SDSS, LS, EUCLID, 2MASS, WISE) to achieve specific scientific objectives, among others: to quantify the influence of the environment in galaxies and determine the SEDs of galaxies within the region R≤ Rvir but also well into their outskirts. The lack of deep u-band and nIR data of CATARSIS clusters has led to a long-term program using the CAHA telescopes to complement and extend the TARSIS wavelength range and allow for the building and modeling of the cluster galaxies’ SEDs and corresponding SFHs and SFRs.

Presentaré un resumen del proyecto AtLAST, qué se ha conseguido hasta la fecha y el trabajo que queda por delante, en particular para el nodo UCM, nuevo socio de AtLAST a contar de este año.

I will talk about recent simulations showing the effect of primordial magnetic fields on the matter power spectrum on small scales, and the subsequent evolutionary effect on dwarf galaxies. 

Algunos de los recursos disponibles de hardware disponibles en el grupo GUAIX.

The core question driving this work is how to automate the georeferencing of nighttime images captured by the ISS, especially wide-field images, which present unique challenges due to orbital motion, distortion, and limited metadata. Automating this process is essential to unlock the full potential of these images for studying light pollution, a growing environmental issue with significant impacts on biodiversity and ecosystems. By providing georeferenced data, this work supports the development of precise maps, enabling better understanding and mitigation strategies for light pollution's adverse effects on our planet.

Satellite galaxies experience multiple physical processes when interacting with their host halos, often leading to the quenching of star formation. In the Local Group, satellite quenching has been shown to be highly efficient, affecting the majority of satellites except the most massive ones. While recent surveys are studying Milky Way analogs to assess how representative our Local Group is, the dominant physical mechanisms behind satellite quenching in Milky Way-mass halos remain under debate. 

In this talk, I will present our analysis on satellite quenching within the same Milky Way-mass halo, simulated using various widely-used astrophysical codes, each using different code architecture and implementing different supernovae feedback recipes. The goal is to determine whether quenched fractions, quenching timescales and the dominant quenching mechanisms are consistent across codes or if they show sensitivity to the specific hydrodynamic method and supernovae feedback physics employed in the AGORA CosmoRun suite of simulations. 

In general, we have observed convergence across codes regarding the overall trends in quenching timescales and quenched fractions, despite the use of different approaches for SNe feedback: the less massive the satellite, the faster its quenching occurs. We also found that ram pressure stripping and strangulation are the most dominant mechanisms driving satellite quenching in MW-mass halos. Nevertheless, the efficiency of these quenching mechanisms varies between models. The main factor influencing satellite quenching efficiency is the restoring pressure of each satellite, which is highly sensitive to the code and supernova feedback implemented, ultimately determining its ability to resist stripping mechanisms.

In this talk, I will provide an overview and update on the CATARSIS project.

In this talk, I will provide an overview and update on the "Cities at Night" project.

Breve resumen de los aspectos administrativos/ burocráticos a tener en cuenta, en especial  para las nuevas incorporaciones

The abundance of neutron-capture elements provide an important fossil signature in Galactic archaeology for tracing the chemical evolution of the Milky Way stellar populations. We employ the automated abundance estimation procedure GAUGUIN, developed in the Gaia/RVS analysis pipeline, for Eu abundances for stars observed by the ESO spectrographs HARPS (R ~ 115000), FEROS (R ~ 48000) and UVES (R ~ 40000),  and parametrised within the AMBRE Project. We derived heavy element abundances (r- process element as Eu) for a sample of 778 Milky Way stars, homogeneously characterised using Gaia data, to chemically and dynamically identify potential accreted stellar populations and study their different signatures with respect to the in-situ population formed in the Galaxy. In agreement with previous works, r-process element enhancements have been observed in some metal-poor stars ([M/H] < -1.0 dex), turning them into a crucial key to investigate the early stages of the formation and chemical evolution of a galaxy.

Comprender los mecanismos que gobiernan la formación estelar en las galaxias es clave para desentrañar la evolución de estos sistemas. Este trabajo usa estadística bayesianas y técnicas de minería de datos para analizar gradientes de metalicidad, los cuales brindan información sobre el procesamiento y enriquecimiento del gas. Una tendencia notable es la manifestación del efecto del "downsizing" en las propiedades de las galaxias, donde galaxias masivas forman estrellas más rápidamente que sus contrapartes de menor masa.

Instrumentación y utilidades del Observatorio Astronómico