Recent Talks

 PyCOMPSs is a task-based programming in Python that enables simple sequential codes to be executed in parallel in distributed computing platforms. It is based on the addition of python decorators in the functions of the code to indicate those that can be executed in parallel between them. The runtime takes care of the different parallelization and resource management actions, as well as of the ditribution of the data in the different nodes of the computing infrastructure. It is installed in multiple supercomputers of the RES, like MareNostrum 4 and now LaPalma. The talk will present an overview of PyCOMPSs, two demos with simple examples and a hands-on in LaPalma on how we can parallelize EMCEE workloads.

Slides and Examples: https://gitlab.com/makhlaghi/smack-talks-iac

Desde el 2019, en el Departamento de Electrónica del Área de Instrumentación del Instituto de Astrofísica de Canarias (IAC) se ha estado trabajando para tener la capacidad de diseñar y medir circuitos integrados con diferentes procesos tecnológicos. Gracias al proyecto EMIAC (Equipamiento Microelectrónica IAC) del Plan Nacional de Infraestructuras y posteriormente en menor medida al Plan de Recuperación, Transformación y Resiliencia, se está avanzando en la creación y puesta en marcha del Laboratorio de Circuitos Integrados (LABIC). El objetivo de esta presentación es mostrar el estado actual del laboratorio así como las líneas futuras.

Unirse a ZOOM:

https://rediris.zoom.us/j/84979227061

Emisión en Youtube:

https://youtu.be/Ec3Ktstx32o

Uno de los principales problemas que afecta no solo a la astrofísica sino a otros sectores de investigación e industria a nivel nacional, es la fabricación de elementos ópticos. De esta forma el CSOA se concibe para cubrir parte de esa demanda, no solo para fabricar elementos óptico tradicionales (esféricos y cónicos) y superficies u elementos ópticos no convencionales (asféricas, formas caprichosas, etc.). Para ello, debe contar con toda la infra estructura de última generación en cuanto a fabricación respecta, tales como sierras, generadoras, pulidoras, equipos de metrología y de recubrimientos ópticos para entregar un producto completamente funcional según se requiera. En esta breve charla hablaré de gran parte del equipo que se ha adquirido y ha sido entregado, lo que va situando al CSOA con la capacidad de ir ofreciendo ya algunos servicios.

Se hará una revisión de la tecnología de imágenes médicas, y de los métodos para su análisis y visualización. También se prestará atención a modelos de transferencia de tecnología a empresas en este campo. La computación de imágenes médicas es un campo multidisciplinar que involucra a médicos, ingenieros y científicos. Los campos que destacaremos son los métodos automáticos y semiautomáticos de procesado e interpretación de imágenes médicas, destacando en los últimos años la inteligencia artificial, que ha dado lugar a nuevos campos de investigación y aplicación, tales como la radiómica y la radiogenómica. También se discutirán las sinergias con la tecnología astrofísica y algunas posibilidades de I+D y trasnferencia desde el IAC.

Youtube: https://youtu.be/E_AVrcyqrO0

Recent years have seen impressive development in cosmological simulations for spiral disc galaxies like the Milky Way. I present a suite of high-resolution magneto-hydrodynamic simulations that include many physical processes relevant for galaxy formation, including star formation, stellar evolution and feedback, active galactic nuclei and magnetic fields. I will discuss how these processes affect the formation of galactic discs, and what these simulations can tell us about the formation of the Milky Way, such as the properties of the Galaxy's putative last significant merger and its effect on the formation of the thick disc and stellar halo. 

On the Sun, the presence of magnetic flux at the photosphere is closely linked to (1) steady heating of the overlying atmosphere and (2) transient brightenings, the largest of which are flares.   I will discuss statistical properties of both phenomena, with an emphasis on aspects of each that might apply to other astrophysical objects, such as other stars or stellar remnants, and perhaps AGNs.  Regarding heating, power-law scalings have been found to relate magnetic flux with steady coronal emission in both soft X-ray (SXR) and EUV ranges.  A key observation is that the details of magnetic structure (field strengths and their spatial gradients, including measured electric currents) appear not to affect heating rates. Similar SXR scalings have been reported for G,K, and M dwarfs and classical T-Tauri stars.  Departures from such scalings, whether on the Sun, other stars, or other objects, might reveal important aspects of the heating mechanisms that drive steady emission, and should be sought.   Regarding flaring, again a power-law scaling between magnetic flux and flare SXR emission has been found, but with a different exponent.  Differences in these scalings suggest that steady heating fundamentally differs from flare heating, disfavoring the “nanoflare” hypothesis (i.e., that steady coronal heating arises from many weak, unresolved flares that are essentially scaled-down versions of larger flares).  Analogous differences in the scalings of steady vs. flaring luminosities with magnetic flux on other objects could constrain processes driving each type of emission.  Another key property of flares is that they extract energy from the magnetic field, which in the solar case leads to measurable changes in field strengths after flares – photospheric field strengths tend to increase, coronal fields tend to decrease.  It is possible that analogous changes could be observed on other stars or objects (via, e.g., Zeeman or synchrotron  methods). 

Se cuenta la historia de la integración del subsistema Fiber Link (FL) en el telescopio de 3.6 m del Observatorio de La Silla para alimentar el espectrógrafo NIRPS. NIRPS es un espectrógrafo de alta resolución y ultraestabilidad optimizado para el rango infrarrojo cercano del espectro. Compartirá foco con el instrumento HARPS y su finalidad principal es el estudio de exoplanetas. El subsistema FL permitirá alimentar al espectrógrafo con la luz procedente del telescopio y optimizará la estabilidad de todo el sistema.

Over the past decade, our understanding of the Large Magellanic Cloud (LMC) and its relationship to the Milky Way (MW) has undergone a paradigm shift. The LMC now appears to be on the order of 20% of the MW mass. At this mass, the LMC creates large dynamical effects, opening up new avenues for studying the MW in cosmic context, time-dependent dynamics in general, and even the nature of dark matter. I will discuss (1) how the LMC is strongly deforming the MW by displacing the MW stellar disc, (2) how the MW-LMC pair fits in our understanding of hierarchical galaxy assembly, and (3) what the LMC can tell us about terrestrial searches for dark matter. I will also present the theoretical tools driving the science, including methods for flexibly parameterising time-dependent dynamics, as well as robust methods for studying the stability of dynamical systems.

Zoom: 

https://rediris.zoom.us/j/81076006712?pwd=VWNHSS94dFBPS3YyNlpsellIdG1hUT09

Meeting ID: 810 7600 6712            Passcode: 304299

Youtube: https://youtu.be/Puv8s0j7HwY