List of all the talks in the archive, sorted by date.
Kepler photometry was so precise that new ways could be developed to harvest the great wealth of quasi-continuous data that has never been accessible from the ground. We initiated a project that we dubbed The Kepler Pixel Project in order to explore approaches and to discover new pulsating stars and other time-variable objects. During the project we examined individual pixels of the original Kepler mission to find interesting objects around the main Kepler targets. Specifically we launched a subproject to find background, faint RR Lyrae stars that are missing from the original Kepler sample. Altogether we found 26 new RR Lyrae stars, increasing the Kepler original RR Lyrae sample by 50%. In this talk I'll present the latest results of this project. In addition to RR Lyrae stars I will also show results on ~1000 new eclipsing binaries found in the framework of the same project.
Vera C. Rubin Observatory's Legacy Survey of Space and Time (LSST) is one of the most important ground-based astronomy projects of the coming decade. In the second half of this talk I will present my research group's work on classification of variable stars with machine learning methods which is part of the Hungarian in-kind LSST contribution. The novelty of our method is that we use images of light curves, such as a human classifier would do. The method gives surprisingly good results based on the shape of light curves only, but can be further improved if additional astrophysical parameters (distance, amplitude, colors, etc.) are taken into account.
Only recently, thanks to the Gaia, have we been able to directly measure how our own Galaxy was formed since its infancy, by cannibalizing smaller galaxies formed at the core of dark matter subhalos. These accretion events can be seen as kinematic groups and may have brought their own group of globular clusters, some of which are only seen today as their remnant cold stellar streams. Here I will discuss how the main accretion events unveiled by Gaia can be linked to previously known halo substructures, mainly large stellar clouds identified more than a decade ago in large photometric surveys. Additionally I will discuss the Jhelum stellar stream in the light of its interaction with the Sagittarius stream, which can give us insight on the details of this ongoing accretion event. Finally, I will briefly discuss how the new Gaia XP DR3 spectra is aiding in the identification of metal-poor unmixed halo substructures in the solar neighbourhood, highlighting the case of ED-2, a [Fe/H] = -2.5 cold stellar stream in which the Sun is embedded in.
In this talk, I'll describe the full upgrade of OSIRIS at GTC telescope, once installed in the Cassegrain focal station including a new monolithic blue-sensitive detector. Changes in the standard operation of the instrument will be detailed, as well as a brief summary of the short-term instrumentation plan for GTC in 2023.
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ID de reunión: 869 8574 0449
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La finalidad del proyecto TTNN es realizar la mejora del sistema de control de los telescopios IAC-80 y Carlos Sánchez con el objetivo que el nuevo entorno de software y hardware que se diseñe sea robusto
versátil, permitan controlar los telescopios de forma remota y facilitar, a posteriori, su operación automática. Para el cumplimiento de estos requerimientos en la parte software se está diseñando e implementando un sistema de control de alto nivel basado en ROS y una aplicación de escritorio escrita en pyQt5.
MAAT is a mirror-slicer integral field unit that will be installed in OSIRIS in 2024, breathing new life into the GTC's work horse instrument. As well as the opportunity to perform spatially-resolved spectroscopy over a field of 10"x7", MAAT will also offer increased signal-to-noise and resolution for point sources with respect to the standard long slit mode. As part of the preparations for the arrival of MAAT, we have implemented support for the reduction of OSIRIS data into the open-source, python-based spectroscopic reduction package PypeIt. Indeed, with the arrival of the new blue-sensitive CCD, PypeIt is now the only publicly available pipeline that continues to work for OSIRIS. With very little human intervention, PypeIt produces fully calibrated and coadded spectra that are near the Poisson limit for point sources. In this talk, I will present a brief overview of the philosophy behind PypeIt and demonstrate the ease with which OSIRIS data (and soon MAAT data) can be reduced.
I present a detailed analysis of the scaling relations of ETGs and suggest a way to predict the evolution of the distributions of galaxies in these planes. This new approach is able to account of several features observed in the FP projections and of the tilt of the Fundamental Plane.
El próximo proyecto en estudiar es fondo cósmico de microondas (CMB) es LiteBIRD, un satélite de la JAXA que pretende estudiar la polarización de los modos-B. En él se encuentran integrados tres telescopios que recorren un rango frecuencial desde los 34 hasta los 448 GHz, donde se encuentran los Transition-Edge Sensor Detectors (TES), que operan a una temperatura de 100mK y que requieren de una estabilidad térmica estricta. En el Instituto de Astrofísica de Canarias se están estudiando mecanismos de control de la temperatura para convertir los requisitos térmicos en una realidad.
Meeting ID: 817 0462 3667
Dwarf galaxies are powerful tools of near-field cosmology and galactic archaeology: their numbers, distribution, and star formation can be linked to both the tenets of LCDM (the missing satellite "problem," their (an)isotropic distribution, their dark matter content) and to the build up of their hosts and their environment (accretion, quenching). The exquisite detail offered by observation of the nearby Milky Way dwarf galaxies has built a picture of what dwarf galaxies are and how they evolved through time. In this talk, I will review the increasingly sharp view we are building of the dwarf-galaxy system of the Milky Way's "sister" galaxy, Andromeda, and emphasize key similarities and differences between these two systems of satellites in the hope to learn what features are common or, on the contrary, driven by the different pasts of the Milky Way and Andromeda.
Meeting ID: 841 1580 773
- Temperature inhomogeneities cause the abundance discrepancy in H II regionsDr. J. Eduardo Méndez-DelgadoTuesday June 13, 2023 - 12:30 GMT+1 (Aula)
- TBDDr. Doug RennehanThursday June 15, 2023 - 10:30 GMT+1 (Aula)