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X-WR-CALNAME:Instituto de Astrofísica de Andalucía
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X-WR-CALDESC:Eventos para Instituto de Astrofísica de Andalucía
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BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20250121T090000
DTEND;TZID=Europe/Paris:20251030T170000
DTSTAMP:20260413T143241
CREATED:20241219T121029Z
LAST-MODIFIED:20250912T080532Z
UID:22550-1737450000-1761843600@www.iaa.csic.es
SUMMARY:Academic Spanish Course for Foreigners (2025)
DESCRIPTION:The Academic Spanish course for foreigners is designed to facilitate effective communication in academic and profesional contexts. Through a practical and personalized focus\, the participants will develop essential linguistic abilities to discuss scientific articles\, participate in conferences\, give presentations\, and collaborate in international projects. The program includes technical vocabulary\, beginner and advanced grammar\, and simulations of real-life situations. Moreover\, it will promote the cultural immersion to strengthen the comprehension of the Hispanic world\, and their impact on interdisciplinary investigation and collaboration. \nThis course will be taught throughout in the following blocks: \nJanuary 21st – February 27thApril 22nd – May 29thSeptember 23rd – October 30thThe course is taught by Prof. Nazira Ruíz
URL:https://www.iaa.csic.es/evento/academic-spanish-course-for-foreigners-2025/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:SO Training
ATTACH;FMTTYPE=image/jpeg:https://www.iaa.csic.es/wp-content/uploads/2024/12/academicspanish.jpg
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BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20250703T123000
DTEND;TZID=Europe/Paris:20250703T133000
DTSTAMP:20260413T143241
CREATED:20250623T102023Z
LAST-MODIFIED:20250702T120548Z
UID:25870-1751545800-1751549400@www.iaa.csic.es
SUMMARY:New clues about how Mars lost its water
DESCRIPTION:I will talk about a recent study led by IAA-CSIC focused on the atmospheric H escape during high obliquity period in recent Mars (average ~35º in last millions of years). Observations show that current thermal H escape (major water loss process) varies seasonally\, with considerable increases during dust storms of both  water abundance in the upper atmosphere and H escape rate. Present H-loss rates agree with 3D simulations by the Mars Planetary Climate Model used in this study\, varying with season between 1-11 x1026 atoms/s. However\, if we apply current escape rates to Mars’ entire history\, those values cannot fully explain the large volumes of ancient surface water suggested by several geological and mineralogical observatios. \nOur simulations with an obliquity of 35º indicate that the H escape rate could have been up to 20 times larger than today. The accumulated H loss over Mars history would translate into ~80 m Global Equivalent Layer\, aligning with the lower range of geological estimates and highlighting atmospheric H loss as a key factor in Mars’ desiccation. \nFecha: 03/07/2025 – 12:30Dr. Gabriella GilliIAA-CSIC \n 
URL:https://www.iaa.csic.es/evento/increased-hydrogen-escape-from-mars-atmosphere-during-periods-of-high-obliquity/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios
ATTACH;FMTTYPE=image/png:https://www.iaa.csic.es/wp-content/uploads/2023/11/seminarscover-e1752660087307.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20250715T123000
DTEND;TZID=Europe/Paris:20250715T133000
DTSTAMP:20260413T143241
CREATED:20250707T114712Z
LAST-MODIFIED:20250707T114745Z
UID:26020-1752582600-1752586200@www.iaa.csic.es
SUMMARY:A UV-to-IR view of a nearby high-z analog with JWST and HST to interpret the first galaxies
DESCRIPTION:In the current JWST era\, detailed observations of the first generation of galaxies have started to revolutionize our knowledge of the early Universe\, with outstanding but also puzzling discoveries. In particular\, high-z systems in the epoch of reionization (z>6) are generally found to be low-mass\, compact and metal-poor\, and show prominent emission lines\, indicating extreme radiation fields. However\, their properties are not trivial to be determined\, some seem to show intriguing chemical inhomogeneities and an unprecedented number of them may host massive accreting black holes (i.e.\, Active Galactic Nucleus\, AGN\, activity) already in the first billion years. Nearby blue compact dwarf galaxies such as SBS 0335-052 E share similar properties\, and thus represent the perfect local laboratories for the multi-wavelength detailed studies required to understand the properties and mechanisms driving such intriguing scenarios. In this talk\, I will show new MIRI/MRS data of SBS 0335-052 E\, mapping MIR lines (e.g.\, [NeII]\, [SIV]\, [NeIII]\, [OIV]\, [NeV])\, in combination with UV spectroscopy and imaging. These data map the ionized gas at different level of ionization and dust attenuation at sub-kpc scales in this system for the first time. Thus\, they allow us to investigate the main ionization sources of the gas (massive stars\, shocks or AGN) in this high-z analog\, revealing the presence of an extended very high ionization emission possibly due to an accreting intermediate massive black hole. Overall\, this study provides us with an extremely powerful toolkit\, pivotal for understanding the gas conditions and feedback from different ionization sources in the earliest galaxies that reionized the universe. \nFecha: 15/07/2025 – 12:30Dr. Matilde MingozziSpace Telescope Science Institute\, Baltimore\, USA \n 
URL:https://www.iaa.csic.es/evento/a-uv-to-ir-view-of-a-nearby-high-z-analog-with-jwst-and-hst-to-interpret-the-first-galaxies/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios
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BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20250722T123000
DTEND;TZID=Europe/Paris:20250722T133000
DTSTAMP:20260413T143241
CREATED:20250721T083224Z
LAST-MODIFIED:20250721T083310Z
UID:26487-1753187400-1753191000@www.iaa.csic.es
SUMMARY:Using Artificial Intelligence to unveil the secrets of stars from their vibrations
DESCRIPTION:During all stages of evolution\, stars oscillate as a superposition of normal modes of certain frequencies that are indicative of their internal structures and compositions. These vibrations are visible as surface brightness fluctuations\, and have been observed by numerous telescopes. Despite the availability of an extensive sample of stars observed by the Kepler telescope\, and the anticipated influx of additional data from missions such as TESS and the forthcoming PLATO\, the full scientific exploitation of these datasets remains constrained by the conventional methods which require substantial computational time and resources for detailed analysis. \nIn this talk\, I will discuss about asteroseismology and demonstrate how we leverage advanced deep learning techniques to facilitate rapid analysis of these datasets\, especially those of post-main-sequence stars which have normal modes that enable us to investigate their interiors in significant detail\, including rotation rates and magnetic fields. \nFecha: 22/07/2025 – 12:30Shatanik BhattacharyaTata Institute of Fundamental Research\, Mumbai\, India \n 
URL:https://www.iaa.csic.es/evento/using-artificial-intelligence-to-unveil-the-secrets-of-stars-from-their-vibrations/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20250724T123000
DTEND;TZID=Europe/Paris:20250724T133000
DTSTAMP:20260413T143241
CREATED:20250703T153435Z
LAST-MODIFIED:20250721T083929Z
UID:26010-1753360200-1753363800@www.iaa.csic.es
SUMMARY:The assembly process of star clusters: ALMA-IMF protoclusters traced by N2H+
DESCRIPTION:In this talk I focus on the analysis of two of ALMA-IMF Large program protoclusters\, the G353.41 and the G351.77\, located at a distance of ∼2 kpc and with masses ∼2.5×10^3 M⊙ within 2pc^2 \, and both embedded in larger-scale (∼8 pc) «mother filaments». We analyze the dense gas kinematics a 4 kau resolution traced by N2H+ (1−0). Focusing on G353\, and from position-velocity (PV) diagrams we suggest that at large scales (~1 pc) the protocluster is undergoing slow gravitational. On small scales (~0.1 pc) we find multiple «V-shapes»\, or converging velocity gradients (VGs). These are consistent with gas flows toward «cores»\, which are small (~4 kau) condensations of mass representing the sites of formation of individual or a small number of stars. We find that V-shapes near the hub of G351 have the largest mass accretion rates in our sample (by a factor of ~77% compared to the mean)\, suggesting a faster collapse at the center relative to the outskirts. This indicates that the most massive stars are already forming at the center of the protocluster. Turning to G351\, we find similar results and the ubiquitous presence of V-shapes in the PV diagram analysis. Hence we suggest that the conditions in G353 and G351 are generic features of Milky Way disk protoclusters. Moreover we suggest that the V-shapes may represent a useful tool as an early star formation rate tracer\, although this hypothesis remains to be thoroughly tested. In more evolved protoclusters such as G012\, we witness the emergence of kinematic features consistent with rotation\, which are correlated with star formation indicators. In summary\, I highlight the power of dense gas kinematics to «pick apart» the Milky Way cluster formation process. \nFecha: 24/07/2025 – 12:30Prof. Dr. Rodrigo Alvarez GutiérrezUniversity of St Andrews\, Scotland; Universidad de Concepción\, Chile \n 
URL:https://www.iaa.csic.es/evento/the-assembly-process-of-star-clusters-alma-imf-protoclusters-traced-by-n2h/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios
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