In my talk I will present some of the main results achieved during my first year of “Maria Zambrano” contract. I will present: 1) the results published in a Letter (in 2023) using ALMA data to study the emission of the earliest phase of the formation and evolution of super star cluster (SSCs) in the composite galaxy NGC 4945; 2) the works in progress using MEGARA/GTC data (e.g., the kinematic analysis applied to specific targets drawn from the MEGADES survey). The development of multi-component gaussian techniques is key to properly analyze such high spectral resolution data. 

Objetivos: CATARSIS es el proyecto de legado que usará 6 años de tiempo oscuro del telescopio de 3.5m de Calar Alto usando el instrumento TARSIS. El objetivo de CATARSIS es obtener espectroscopía 2D no sesgada de toda la extensión de una muestra de 16 cúmulos de galaxias a desplazamientos al rojo 0.15 < z < 0.23. A fin de optimizar CATARSIS esta tesis tiene como objetivo principal derivar los perfiles de masa de los cúmulos de galaxias de CATARSIS empleando las ventajas de las simulaciones hidrodinámicas. Para ello se ha usado las simulaciones de cúmulos The Three Hundred Project que cuenta con un total de 324 cúmulos. El código de simulación empleado es GIZMO-Simba.

Método: En primer lugar, se ha empleado el método de la cáustica para los 324 cúmulos a un redshift z = 0.267 y usado 3 líneas de visión diferentes (X, Y, Z). El código que se ha empleado es el de Gifford et al 2013 que nos permite obtener los perfiles radiales de masa y compararlos con los perfiles reales de la simulación. Para obtener un resultado óptimo se ha realizado un método iterativo dentro del propio código considerando primero un perfil de anisotropía constante y posteriormente ajustando a un perfil radial. Este método se ha llevado a cabo para diferentes cortes en magnitud r: 22, 21 y 20 y usando 2 perfiles radiales diferente. Por último, se ha tenido en cuenta la combinación del corte en magnitud y la SFR. 

Resultados: Los resultados obtenidos para la M200 se ajustan mejor a los datos reales de la simulación si tenemos en cuenta un perfil no constante de anisotropía. Por otro lado, hemos obtenido que el resultado no mejora sustancialmente si utilizamos un perfil radial propio o el perfil de Mamon & Lokas. Además, hemos encontrado que hay una diferencia para magnitud 20 y el resto de las magnitudes consideradas, pero no de forma significativa entre los cortes 21 (límite para CATARSIS) y 22. Para el caso donde tenemos en cuenta la SFR, los resultados son prácticamente los mismos. 

Trabajo futuro: El paso siguiente es estudiar qué efecto tiene la rotación y el alineamiento de spin de los cúmulos en la estructura de estos y cómo afecta a la anisotropía y los resultados obtenidos.

I will give a brief overview of my research career and the skills developed in it before explaining my current research line into how galaxies have evolved, probing their history using IFU observations. I employ mainly surveys such as CALIFA and MaNGA and apply full spectral fitting to recover the properties of their stellar populations which I use to derive how several parameters have changed through time. Mainly I focus on SFR and [Z/H] and derived parameters.

I would like to present a brief summary of the efforts spent by our group in the last few years to derive reliable RGB calibrated RGB sources that can be employed to calibrate images obtained with common digital cameras.

I would like to talk about a project to study the presence and characterization of outflows in a representative sample of nearby star forming galaxies by means of high resolution IFU observations with MEGARA of interstellar absorption (NaD) and emission (Ha, NII, SII) lines. Integral field spectroscopy let us simultaneously study the complex kinematics and morphology of several phases of the wind material in order to estimate the amount of gas/dust/metals in the wind, how much of this material is put into the IGM, and how the production/efficiency of the wind relates to properties of the host galaxies.

In this presentation, I will present the Agile and Cognitive Cloud-edge Continuum management (AC3) project. This EU-funded project aims to create a dynamic framework for the effective management of data in the cloud-edge computing spectrum and to reduce energy consumption using AI/ML algorithms. The basic idea will be to place microservices efficiently on the CECC infrastructure based on application profiles. I will focus on the details of Use Case (UC) 3. The goal of this UC will be to demonstrate the CECCM’s capabilities to deploy and run astronomical software to process data cubes. Finally, I will as well review my current and near future line research in the context of the GUAIX group. 

MEGADES (MEGARA galaxy disc evolution survey) is the scientific legacy project of the MEGARA instrument, the integral field and multi-object spectrograph installed on the 10.4 m telescope GTC. The galaxy sample consists of 43 nearby galaxies and we currently count with observations of their central regions taken with the low-resolution VPHs of the instrument (R ~ 6000). All observations from the survey are publicly available on the project website (www.megades.es) and are included in the first data release of the project. In this short talk I will present the current status of the scientific exploitation of the data observed so far within the MEGADES project including studies on the ionised gas, the dynamical state and the properties of the stellar populations in the central regions of the galaxies in the sample. 

Estudio 2D y multilongitud onda de las propiedades físicas de galaxias con formación estelar, que serán utilizadas como referencia para los estudios de galaxias a muy alto redshift que está detectando JWST. Además todo esto se utilizará para contribuir en el diseño y construcción del instrumento MOSAIC que se instalará en el telescopio gigante europeo(ELT).

Utilizando Redes Neuronales Convolucionales, estamos identificando historias de formación estelar y metalicidad. Para ello, hemos generado datos sintéticos con EMILES que simulan observaciones de diferentes historias de formación estelar. Estas observaciones coinciden con MUSE (VLT) y los filtros del WCS-HST. El objetivo será utilizar este modelo con el catálogo de PHANGS-MUSE y PHANGS-HST para generar mapas de formación estelar.

Presentaré un resumen del estado actual del instrumento MOSAIC, la contribución española (y del grupo GUAIX en concreto) al desarrollo del instrumento, y el progreso del Science Team

We use a MW model from a suite of high-resolution hydrodynamical cosmological simulations named GARROTXA to establish the relationship between the vertical disturbances seen in its galactic disk and multiple perturbations, from the dark matter halo, satellites and gas. We calculate the bending modes in the galactic disk in the last 6 Gyr of evolution. To quantify the impact of dark matter and gas we compute the vertical acceleration exerted by these components onto the disk and compare them with the bending behavior with Fourier analysis. We find complex bending patterns at different radii and times, such as an inner retrograde mode with high frequency, as well as an outer slower retrograde mode excited at different times. We find that the infall o satellite galaxies leads to a tilt of the disk, and produces strong anisotropic gas accretion with a misalignment of 8º, creating significant vertical accelerations onto the disk plane. The misalignment between the disk and the inner stellar/dark matter triaxial structure, formed during the ancient assembly of the galaxy, also creates a strong vertical acceleration on the stars. We also find dark matter sub-halos that temporally coincide with the appearance of bending waves in certain periods. We conclude that several agents trigger the bending of the stellar disk in this simulation, including satellite galaxies, dark sub-halos, misaligned gaseous structures, and the inner dark matter profile. These phenomena coexist and influence each other, sometimes making it challenging to establish direct causality.

We investigate the relation between the stellar mass, SFR, molecular gas, total gas, baryonic mass, gas metallicity, gas fraction, SFE and effective oxygen yields. We combine our IFU observations with data from the surveys THINGS, CARMA, and archival data from DustPedia.

Although we recover the shape of several known relations, our slopes are different to previously reported ones. Our star formation main sequence, Kennicutt-Schmidt (KS) and molecular KS relations show higher SFRs, lower scatter, and higher correlations, with steeper (1.21), and flatter slopes (0.96, 0.58) respectively. The shape of the SRs including metallicity, stellar mass, and gas fraction are flat, with an average value of 12+log(O/H) ~8.12 dex.

Finally, we find higher dispersions and lower correlations for the baryonic mass vs effective oxygen yields, and the stellar, gas and baryonic mass vs SFE.

En esta breve charla presentaré el estado de diseño y construcción del instrumento TARSIS, la futura IFU de gran campo (2.8x2.8 arcmin^2) para el 3.5m de Calar Alto. Me centraré en la parte del desarrollo instrumental desde un punto de vista general, así como los beneficios que el mismo traerá al grupo GUAIX y sus miembros, tanto a corto como a largo plazo. También mencionaré el impacto logístico potencial de TARSIS de cara a su integración en laboratorio allá por el 2027.

Se resumirán los objetivos de la misión espacial y las distintas fases de desarrollo hasta su lanzamiento.

The Metal-THINGS survey is observing a selected sample of nearby galaxies with IFU spectroscopy (using VIRUS-P and MUSE). I will provide an update on the Metal-THINGS survey status, from observations to science.

La tesis doctoral titulada “Distribuciones espectrales de energía de las galaxias de la muestra CATARSIS: observaciones y predicciones de diferentes simulaciones numéricas” se centra en el estudio de las propiedades de los 16 cúmulos de galaxias que componen la exploración CATARSIS (del inglés Calar Alto Tetra-Armed Super-Ifu Survey) que se observarán con el futuro instrumento TARSIS (del inglés Tetra-Armed Super-Ifu Spectrograph) que será instalado en el telescopio de 3.5m del Observatorio de Calar Alto. La tesis estará co-dirigida por las profesoras Cristina Catalán Torrecilla (PAD) y África Castillo Morales (PTU), ambas miembros del grupo GUAIX de la UCM. Durante la misma se procederá a la adquisición y análisis de los datos observacionales (desde observatorios de Tierra y del Espacio) que permitirán derivar las propiedades de las galaxias individuales y de la luz intra-cumular (tales como la morfología, masa estelar, tasa de formación de estrellas o contenido en gas) mediante la construcción de Distribuciones Espectrales de Energía (SEDs del inglés Spectral Energy Distributions). Posteriormente, estas propiedades se compararán con las predicciones dadas por simulaciones numéricas de formación y evolución de galaxias en cúmulos, con el objetivo tanto de inferir sus propiedades globales como de seleccionar los observables susceptibles de ser medidos con CATARSIS que sean más sensibles a los parámetros cosmológicos. Esto último permitirá sentar las bases para las futuras mediciones de CATARSIS ayudando a mejorar la determinación de constantes cosmológicas fundamentales y el proceso de evolución de galaxias en cúmulos.

After more than a decade working at the APEX sub-mm observatory in Chile I am now involved in the development studies of the succesor of APEX, a new 50-m dish called AtLAST. In particular, I am responsible for the data management plan as well as an important contributor to the science operations plan for this new facility. On the way, I became interested in the automatization of processes to improve scientific operations. This led me to getting interested and experimenting with basic ML/AI techniques. In the last year I have learned how Reinforcement Learning works and I believe it can help optimizing the scheduling of surveys. I plan to demonstrate it with the application to the CATARSIS survey to be done with TARSIS at the 3.5m telescope in CAHA.

Radio observations can probe regions of ionised (and magnetised) gas, such as in cosmic web filaments (ie. WHIM) and the halos of galaxies (CGM), that are very challenging to detect by other means. Combining the radio data with other tracers of matter (eg. galaxies) allows us to do many things; for example, to understand the role this diffuse gas plays in galaxy evolution, probe the origin of cosmic magnetic fields, and conduct unique tests for dark matter particle candidates.

I will show some known and some commonly unknown resources that are available to or group members

Evidence of radio synchrotron emission from bridges of low-density gas connecting pairs of galaxy clusters allows us to trace the filaments of the so-called cosmic web, along which the accretion of matter on galaxy clusters happens. We aim to a more comprehensive understanding of the processes behind this emission, by working on promising pairs of dynamically interacting galaxy clusters. In this respect, Abell 0399-Abell 0401 is a unique cluster pair found in an interacting state, where LOFAR detected a radio bridge emission. I will present the results of a multifrequency analysis on the bridge emission in A399-A401 using LOFAR and uGMRT data, and highlight the importance of discovering more systems hosting radio bridges.

My PhD consists of making a scientific and technical contribution to the MOSAIC project. In this talk I will focus on the most advanced part, which is the scientific section.

Our goal is to study the formation of a hot corona in the CGM of halos above the so-called 'Golden Mass' (M_halo ~ 10^12 Msun) that would be responsible for the quenching of star formation. Hydrodynamical simulations predict the formation of this hot corona due to the virial shock heating of the accreted gas, increasing its temperature up to the virial temperature.

Using hydrodynamical cosmological simulations (AGORA project) and GTC observations, we will study the properties of satellite galaxies around galaxies above (and below) the golden mass to characterize how their properties vary upon contact with the CGM of the main halo, with the aim of using them as tracers of virial shock formation. In addition, the comparison between the different feedback codes and models used in the AGORA simulation set will allow us to study how they influence the virial shock formation. Finally, we will try to constrain the feedback recipe with our observations.

I will summarize the work of Nelida Diaz-Fernandez, a part time PhD student working with data from the PHANGS survey to understand the nature of spiral arms in nearby galaxies. 

The abundance of alpha and neutron-capture elements provide an important fossil signature in Galactic archaeology for tracing the chemical evolution of the Milky Way stellar populations. I employ the automated abundance estimation procedure GAUGUIN, developed in the Gaia/RVS analysis pipeline, for deriving precise Mg, Eu and Sr abundances for stars observed by the ESO spectrographs HARPS (R ~ 115000), FEROS (R ~ 48000) and UVES (R ~ 40000), and also C, Mg and Ca from the X-shooter Spectral Library (XSL, R ~ 10000). On the one hand, I will briefly show my current work on deriving r-/s- process elements as Sr and Eu, homogeneously characterised using Gaia data, to chemically identify potential accreted stellar populations and study their different signatures with respect to the in-situ population in the Galaxy. On the other hand, I will present the project with Patricia Sánchez-Blázquez and Alexandre Vazdekis, which purpose is to use the XSL abundance catalogues that we are deriving as a benchmark to train the developed stellar population models by including alpha-enhancements and carbon variations in them, in order to study external galaxies’ abundances in the near future.

Breve exposición de la instrumentación disponible en el Observatorio UCM y del uso del nitrógeno líquido en proyectos de investigación.