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BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20250522T123000
DTEND;TZID=Europe/Paris:20250522T133000
DTSTAMP:20260521T012419
CREATED:20250521T085223Z
LAST-MODIFIED:20250523T084307Z
UID:25648-1747917000-1747920600@www.iaa.csic.es
SUMMARY:Galaxies Hidden in the Forest as a new BAO tracer (and other applications)
DESCRIPTION:The acceleration of the expansion rate of the Universe is yet to be explained. Several models\, including LCDM\, try to explain this acceleration. LCDM bases its explanation on a mysterious dark energy\, adding up to ~75% of the total energy density of the Universe. Other models present modified theories of gravity to explain this effect. But which one is correct? The expansion history of the Universe is a great observable to discriminate between these models. I will talk about measurements of this expansion history at redshift greater than 2 using BAO with the Lyman alpha forest\, and review the latest measurements. I will motivate how galaxies in absorption can be affecting our measurements and explain what do we need to extract them and use them as a new BAO tracers. I will end on a note on other possible applications of these galaxies including the creation of new IGM observables for simulations. \nFecha: 22/05/2025 – 12:30Dr. Ignasi Pérez RafolsFiliación: Universidad Politécnica de Cataluña (UPC)\, España \n 
URL:https://www.iaa.csic.es/evento/galaxies-hidden-in-the-forest-as-a-new-bao-tracer-and-other-applications/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20250527T123000
DTEND;TZID=Europe/Paris:20250527T133000
DTSTAMP:20260521T012419
CREATED:20250515T073924Z
LAST-MODIFIED:20250515T073926Z
UID:25610-1748349000-1748352600@www.iaa.csic.es
SUMMARY:Jets in Planetary Nebulae
DESCRIPTION:At the end of the 20th century\, we thought we had a solid understanding of how low-mass stars evolved into planetary nebulae. However\, by studying the stages leading up to these nebulae\, we discovered a puzzle: the energy needed to form them was too large to be explained by traditional models. This revelation led us to explore a more complex scenario: the interaction of binary stars. The gravitational energy and angular momentum of these stellar systems could provide the additional force needed to drive the formation of nebulae. \nIn this talk\, we will explore the exciting consequences of this new perspective\, such as the evolution of binary systems in which stars share a common envelope and the formation of powerful jets of stellar material. \nFecha: 27/05/2025 – 12:30Dr. Guillermo García SeguraFiliación: Instituto de Astronomía\, Universidad Nacional Autónoma de México\, Ensenada\, Baja California \n 
URL:https://www.iaa.csic.es/evento/jets-in-planetary-nebulae/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20250603T123000
DTEND;TZID=Europe/Paris:20250603T133000
DTSTAMP:20260521T012419
CREATED:20250530T084051Z
LAST-MODIFIED:20250530T084054Z
UID:25721-1748953800-1748957400@www.iaa.csic.es
SUMMARY:Towards an observationally motivated AGN dusty torus model
DESCRIPTION:Several models of nuclear dust in active galactic nuclei (AGN) have been presented in the literature to determine its physical and geometrical properties\, usually assuming the dust density distribution as the main aspect producing differences in the mid-infrared (MIR) emission of AGNs. My PhD research investigates the physical and chemical properties of dust in the torus of AGNs using MIR spectral analysis and radiative transfer (RT) modeling. First\, we determined an observationally motivated dust composition by fitting a mineralogy model to Spitzer/IRS spectra of 49 nearby AGNs showing silicate emission at 10 μm. We found that porous alumina\, periclase\, and olivine grains of 0.1 μm dominate the fits\, while traditional astronomical silicates are rarely favored. Subsequently\, we constructed a large RT model grid that explores a parameter space defined by key physical properties of the torus. We focused on the effects of dust density distribution (smooth\, clumpy\, and two-phase) and dust composition on the MIR spectral energy distribution (SED). The resulting synthetic SEDs were analysed through model-to-model and model-to-observation comparisons. We found that both dust distribution and composition significantly influence the silicate feature strengths and spectral slopes. In this talk\, I will present the main results and discuss the principal effects of the density distribution and chemical composition of dust in the MIR SED. \nFecha: 03/06/2025 – 12:30Ulises Reyes AmadorFiliación: IRYA-UNAM\, México \n 
URL:https://www.iaa.csic.es/evento/towards-an-observationally-motivated-agn-dusty-torus-model/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20250703T123000
DTEND;TZID=Europe/Paris:20250703T133000
DTSTAMP:20260521T012419
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
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20250715T123000
DTEND;TZID=Europe/Paris:20250715T133000
DTSTAMP:20260521T012419
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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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20250722T123000
DTEND;TZID=Europe/Paris:20250722T133000
DTSTAMP:20260521T012419
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:20260521T012419
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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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20250910T123000
DTEND;TZID=Europe/Paris:20250910T133000
DTSTAMP:20260521T012419
CREATED:20250904T121548Z
LAST-MODIFIED:20250904T122504Z
UID:27039-1757507400-1757511000@www.iaa.csic.es
SUMMARY:Unveiling the transport of Galactic cosmic rays with diffuse γ-rays and neutrinos at the highest energies
DESCRIPTION:The Tibet-ASγ and LHAASO collaborations recently provided the first evidence of diffuse γ-ray emission from the Galactic plane up to the PeV range. Due to the challenges this poses to current theoretical models\, it is crucial to carefully study different scenarios of diffuse γ-ray production\, specially towards the centre of the Galaxy. Moreover\, IceCube achieved the first measurements of the neutrino emission from the Galactic plane\, offering a complementary tool to study the distribution of Galactic cosmic rays up to the knee. Remarkably\, these observations provide a unique tool to study the origin of the most energetic Galactic cosmic rays\, the propagation of these particles in different regions of the Galaxy and their composition. \nIn this talk\, I’ll discuss how measurements of the gamma-ray and neutrino diffuse emissions are correlated to the production and transport of cosmic rays in the Galaxy and what the implications of these recent observations are in our theoretical models. In particular\, I’ll show that current observations are compatible with the expected emission from diffuse cosmic rays\, with unresolved sources playing a subdominant role\, and the first hints that seem to favor scenarios of non-uniform propagation of cosmic rays in the Galaxy. \nFecha: 10/09/2025 – 12:30Pedro de la Torre LuqueInstituto de Física Teórica UAM-CSIC \n  \n 
URL:https://www.iaa.csic.es/evento/unveiling-the-transport-of-galactic-cosmic-rays-with-diffuse-%ce%b3-rays-and-neutrinos-at-the-highest-energies/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20251003T123000
DTEND;TZID=Europe/Paris:20251003T133000
DTSTAMP:20260521T012420
CREATED:20250912T084237Z
LAST-MODIFIED:20250930T090827Z
UID:27166-1759494600-1759498200@www.iaa.csic.es
SUMMARY:Reducing the Uncertainty on the Hubble Constant up to 35% with an Improved Statistical Analysis
DESCRIPTION:Reducing the Uncertainty on the Hubble Constant up to 35% with an Improved Statistical Analysis: Different Best-fit Likelihoods for Type Ia Supernovae\, Baryon Acoustic Oscillations\, Quasars\, and Gamma-Ray Bursts \nCosmological models and their parameters are widely debated\, especially about whether the current discrepancy between the values of the Hubble constant\, H 0\, obtained by Type Ia supernovae (SNe Ia) and the Planck data from the cosmic microwave background radiation could be alleviated when alternative cosmological models are considered. Thus\, combining high-redshift probes\, such as gamma-ray bursts (GRBs) and quasi-stellar objects (QSOs\, or quasars)\, together with baryon acoustic oscillations and SNe Ia is important to assess the viability of these alternative models and whether they can cast further light on the Hubble tension. \nIn this work\, for GRBs\, we use a three-dimensional relation between the peak prompt luminosity\, the rest-frame time at the end of the X-ray plateau\, and its corresponding luminosity in X-rays: the 3D Dainotti fundamental plane relation. Regarding QSOs\, we use the Risaliti-Lusso relation among the UV and X-ray luminosities for a sample of 2421 sources. We correct both the QSO and GRB relations by accounting for selection and evolutionary effects with a reliable statistical method. We here use both the traditional Gaussian likelihoods ( LG ) and the new best-fit likelihoods ( LN ) to infer cosmological parameters of nonflat Lambda cold dark matter (LambdaCDM) and flat wCDM models. We obtain for all the parameters reduced uncertainties\, up to 35% for H0\, when applying the new LN likelihoods in place of the Gaussian ones. \nOur results remain consistent with a flat LambdaCDM model\, although with a shift of the dark energy parameter w toward w < -1 and a curvature density parameter toward Omega k < 0. \nFecha y lugar: 03/10/2025 – 12:30 | Salón de ActosMaria Giovanna DainottiNational Astronomical Observatory of Japan (NAOJ) \n  \n 
URL:https://www.iaa.csic.es/evento/reducing-the-uncertainty-on-the-hubble-constant-up-to-35-with-an-improved-statistical-analysis/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20251009T123000
DTEND;TZID=Europe/Paris:20251009T133000
DTSTAMP:20260521T012420
CREATED:20250925T082843Z
LAST-MODIFIED:20251002T105940Z
UID:27406-1760013000-1760016600@www.iaa.csic.es
SUMMARY:Unveiling Water Vapor Transport in the Martian Atmosphere: Unexpected discoveries by NOMAD/TGO
DESCRIPTION:Water is a key component of planetary atmospheres\, shaping their climate and habitability. On Earth\, Venus or Mars\, water vapor drives their atmospheric chemistry\, and serves as a crucial indicator for potential habitability. Understanding its transport\, condensation/sublimation\, and loss to space is essential for planetary evolution. In this context\, Mars offers a compelling case. Despite its current cold and dry state\, geological evidence suggests a wetter past. Today\, on Mars\, water vapor exists in trace amounts but plays a crucial role in many chemical and radiative processes. \nUntil recently\, knowledge of the vertical distribution of water vapor was limited to models and column density estimates. With the advent of the Trace Gas Orbiter (TGO)\, it has become possible to systematically probe the Martian atmosphere using the solar occultation technique. Already well established on Earth\, solar occultations provide detailed information on both the geographic and vertical distribution of trace species such as water vapor.TBD \nFecha y lugar: 09/10/2025 – 12:30 | Salón de ActosAdrián BrinesInstituto de Astrofísica de Andalucía (IAA-CSIC) \n  \n  \n 
URL:https://www.iaa.csic.es/evento/unveiling-water-vapor-transport-martian-atmosphere/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20251016T123000
DTEND;TZID=Europe/Paris:20251016T133000
DTSTAMP:20260521T012420
CREATED:20250915T112430Z
LAST-MODIFIED:20251007T154724Z
UID:27208-1760617800-1760621400@www.iaa.csic.es
SUMMARY:The Stellar Halos of Galaxies and Outskirts of Galaxy Clusters: Clues to their Accretion History
DESCRIPTION:Understanding mass assembly at different scales is key to improving our knowledge on galaxy formation and evolution in general. Stellar halos of galaxies\, primarily formed through the accretion and merger of smaller objects\, preserve memory of their assembly history\, offering unique insight into the accretion and mass growth history of galaxies. During the last decade there has been significant progress\, both from the observational and numerical side\, to characterize stellar halos of Milky Way-mass galaxies. And more recently the outskirts of low-mass galaxies have also started to be explored. On the high mass end\, outskirts of galaxy clusters are also important observational probes of how these systems grow in a cosmological context and can provide insights into their accretion history. \nIn this talk\, I will present the main results both from observations and cosmological simulations that allow us to link the observed properties of stellar halos with the accretion history of their host galaxies. Additionally\, I will present the first kinematical measurement of a diffuse stellar halo beyond the Local Group\, the stellar halo of the edge-on galaxy NGC 4945\, using a novel technique. We couple new deep MUSE spectroscopic observations with existing HST imaging data to spectroscopically measure the radial line-of-sight heliocentric velocity and velocity dispersion in a field at 40 kpc (stellar halo field) along NGC 4945 major axis. If time permits\, I will introduce the 4MOST/CHANCES survey\, aimed at observing the outskirts of ~150 galaxy clusters. \nFecha y lugar: 16/10/2025 – 12:30 | Salón de ActosAntonela MonachesiUniversidad de La Serena\, Chile \n  \n 
URL:https://www.iaa.csic.es/evento/the-stellar-halos-of-galaxies-and-outskirts-of-galaxy-clusters-clues-to-their-accretion-history/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20251021T123000
DTEND;TZID=Europe/Paris:20251021T133000
DTSTAMP:20260521T012420
CREATED:20250925T083021Z
LAST-MODIFIED:20251001T091143Z
UID:27410-1761049800-1761053400@www.iaa.csic.es
SUMMARY:Breaks in radial metallicity gradients of spiral galaxies
DESCRIPTION:Radial abundance gradients in spiral galaxy disks provide key constraints on chemical evolution and galaxy formation. While inside-out growth predicts negative gradients\, observations often reveal deviations such as inner drops or outer flattenings. \nI will present recent results from our group on O/H gradients in spiral galaxies using H II region data from the CALIFA survey. We apply an automated fitting procedure to explore correlations between the physical properties of galaxies and bulges and the presence of these inner drops\, seeking possible explanations for the observed variations. We also examine how ionization source classification and diffuse ionized gas (DIG) contamination influence the inner gradient. \nFinally\, I will present new results for the Milky Way based on planetary nebulae with improved distances from a recalibrated Hα surface brightness–radiusrelation and Gaia DR3 parallaxes. These indicate a flatter O/H gradient than previously reported\, with a slope change near 8 kpc\, coinciding with the corotation radius. \nFecha y lugar: 21/10/2025 – 12:30 | Salón de ActosProf. Oscar CavichiaInstituto de Fisíca e Química\, Universidade Federal de Itajubá\, Brasil \n  \n  \n 
URL:https://www.iaa.csic.es/evento/breaks-in-radial-metallicity-gradients-of-spiral-galaxies/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20251104T123000
DTEND;TZID=Europe/Paris:20251104T133000
DTSTAMP:20260521T012420
CREATED:20250912T084701Z
LAST-MODIFIED:20251015T105331Z
UID:27172-1762259400-1762263000@www.iaa.csic.es
SUMMARY:The role of groups in galaxy evolution: the importance of the pre-processing effect
DESCRIPTION:We present clear and direct evidence of the pre-processing effect of group galaxies falling into clusters in the local Universe (z ≲ 0.1). We start with a sample of 238 clusters\, from which we select 153 with N200 ≥ 20. We considered 1641 groups within the turnaround radius (~ 5 × R200) of these 153 clusters. \nThere are 6654 individual cluster galaxies and 4133 group galaxies within this radius. We considered two control samples of galaxies\, in isolated groups and in the field. The former comprises 2601 galaxies within 1606 isolated groups\, and the latter has 4273 field objects. The fraction of star-forming galaxies in infalling groups has a distinct clustercentric behaviour in comparison to the remaining cluster galaxies. Even at 5 × R200 the group galaxies already show a reduced fraction of star-forming objects. At this radius\, the results for the individual cluster galaxies are actually compatible with the field. That is strong evidence that the group environment is effective to quench the star formation prior to the cluster arrival. The group star-forming fraction remains roughly constant inwards\, decreasing significantly only within the cluster R200 radius. \nWe have also found that the pre-processing effect depends on the group mass (indicated by the number of members). The effect is larger for more massive groups. However\, it is significant even for pairs and triplets. \nFecha y lugar: 04/11/2025 – 12:30 | Sala de JuntasPaulo Afranio LopesObservatorio do Valongo\, Rio de Janeiro\, Brasil \n 
URL:https://www.iaa.csic.es/evento/the-role-of-groups-in-galaxy-evolution-the-importance-of-the-pre-processing-effect/
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:20251111T123000
DTEND;TZID=Europe/Paris:20251111T133000
DTSTAMP:20260521T012420
CREATED:20250930T090018Z
LAST-MODIFIED:20251103T085232Z
UID:27502-1762864200-1762867800@www.iaa.csic.es
SUMMARY:Extreme gamma-ray pulsars (and what CTAO can say about them)
DESCRIPTION:At the dawn of the century only a handful of pulsars had been found to pulse in gamma-rays\, and certainly none was supposed to emit beyond the GeV scale. \nOver the past two decades\, thanks to the Fermi-LAT\, the situation has dramatically changed: we now know more than 300 such objects\, and the number keeps increasing. Behaving as lepton factories and natural particle accelerators\, the physics of gamma-ray pulsars still lacks a complete\, coherent description. As was first realized in early MAGIC observations of the Crab\, some of these objects elude the strong spectral cutoff imposed by their own gargantuan magnetic field and find a way to emit well beyond the tens of GeV\, into (and beyond!) the TeV scale. This makes these «extreme» pulsars targets for imaging atmospheric Cherenkov telescopes and has prompted a progressive «migration» of the emission scenarios farther away from the neutron star. \nIn this talk I will briefly introduce some basic concepts of pulsar physics\, review current results and discuss present hot topics. Finally\, I will also show how the upcoming CTAO has the potential to spark a second-revolution in gamma pulsars\, its consequences stretching even beyond the usual boundary of astrophysics. \nFecha y lugar: 11/11/2025 – 12:30 | Sala de JuntasGiovanni CeribellaMax Planck for Physics (MPP) \n 
URL:https://www.iaa.csic.es/evento/extreme-gamma-ray-pulsars-and-what-ctao-can-say-about-them/
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:20251113T123000
DTEND;TZID=Europe/Paris:20251113T133000
DTSTAMP:20260521T012420
CREATED:20251001T085011Z
LAST-MODIFIED:20251110T101049Z
UID:27526-1763037000-1763040600@www.iaa.csic.es
SUMMARY:A SITELLE overview of interacting galaxies and supernova remnants
DESCRIPTION:The purpose of this talk\, separated into three « chapters »\, is to present an overview of the capabilities of SITELLE\, a wide-field imaging Fourier transform spectrometer built by our team and attached to the Canada-France-Hawaii telescope. \nAfter a brief technical introduction to this instrument\, I will summarize the collaborative work started a few years ago between IAA\, Universidad de Granada and Université Laval on interacting galaxies (which is the main reason for my two-months sabbatical stay in Granada): Arp82\, Arp 143 and\, more recently\, a sample of Hickson compact groups (a project led by Salvador Duarte Puertas\, from UGR). The last chapter is dedicated to an ongoing work on supernova remnants\, both in the Milky Way (the Crab Nebula and Cassiopeia A)\, and then in nearby galaxies\, using data obtained as part of the SIGNALS survey. \nFecha y lugar: 13/11/2025 – 12:30 | Salón de ActosProf. Laurent DrissenUniversité Laval\, Québec \n  \n  \n  \n 
URL:https://www.iaa.csic.es/evento/a-sitelle-overview-of-interacting-galaxies-and-supernova-remnants/
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:20251120T130000
DTEND;TZID=Europe/Paris:20251120T143000
DTSTAMP:20260521T012420
CREATED:20251020T133324Z
LAST-MODIFIED:20251118T113833Z
UID:27805-1763643600-1763649000@www.iaa.csic.es
SUMMARY:SO Colloquium: Pre-CTAO Science with LST: Current and Expected Results
DESCRIPTION:The Large-Sized Telescope prototype (LST-1) is the first and the larger of a new generation of instruments that will form the Cherenkov Telescope Array Observatory (CTAO) in the island of La Palma (CTAO-North). CTAO is designed to explore; with unprecedented sensitivity\, angular resolution\, field of view\, and energy coverage; the Universe at very-high-energy gamma rays. Since beginning its observations\, LST-1 has been studying the northern sky in an energy range between about a few tens of GeV up to a few TeV. Thanks to its high sensitivity and its ability to quickly point toward flaring targets\, LST-1 is particularly well suited to detect and follow up on rapidly changing cosmic sources. \nIn this seminar\, I will present the first scientific results obtained with LST-1 as well as the expectations for the full LST northern array (involving an total of 4 LST telescopes in La Palma\, that will become the most sensitive instrument of its class along 2026) regarding new discoveries in the very-high-energy gamma-ray sky. \nFecha y lugar: 20/11/2025 – 13:00 | Salón de ActosProf. Pol BordasIEEC – ICC – Universitat de Barcelona \n 
URL:https://www.iaa.csic.es/evento/pre-ctao-science-with-lst-current-and-expected-results/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios,SO Colloquium
ATTACH;FMTTYPE=image/png:https://www.iaa.csic.es/wp-content/uploads/2025/07/SO-COLLOQUIUM.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20251125T123000
DTEND;TZID=Europe/Paris:20251125T133000
DTSTAMP:20260521T012421
CREATED:20250930T090140Z
LAST-MODIFIED:20251118T113754Z
UID:27506-1764073800-1764077400@www.iaa.csic.es
SUMMARY:SO Colloquium: The future science of CTAO
DESCRIPTION:In this talk\, I will review the plans for construction\, and the current status of the Cherenkov Telescope Array Observatory\, CTAO\, as well as the current plans for its scientific exploitation through the Key Science Program as described in the latest CTA Science Book. Moreover\, I will also present the opportunities that the future CTAO imply for the entire scientific community in general. \nFecha y lugar: 25/11/2025 – 12:30 | Sala de JuntasGiacomo BonnoliINAF – Istituto Nazionale di Astrofisica\, Osservatorio Astronomico di Brera – Sede di Merate \n 
URL:https://www.iaa.csic.es/evento/the-future-science-of-ctao/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios,SO Colloquium
ATTACH;FMTTYPE=image/png:https://www.iaa.csic.es/wp-content/uploads/2025/07/SO-COLLOQUIUM.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20251127T123000
DTEND;TZID=Europe/Paris:20251127T133000
DTSTAMP:20260521T012421
CREATED:20250912T085614Z
LAST-MODIFIED:20251127T111959Z
UID:27198-1764246600-1764250200@www.iaa.csic.es
SUMMARY:First Glimpses of the Extragalactic Gamma-ray Sky with LST-1: Paving the Way to CTAO
DESCRIPTION:The gamma-ray extragalactic sky is dominated by blazars\, radio-loud active galactic nuclei (AGN) with relativistic jets that are closely aligned with our line of sight. In the MeV range\, the Fermi-LAT satellite has led the efforts in studying this violent type of sources\, with more than 3000 known blazars discovered so far in the MeV range. In the GeV-TeV range\, the Cherenkov experiments MAGIC\, HESS and VERITAS have made significant advances in the field. However\, their sensitivity has only allowed us to discover ~300 sources in the most extreme Universe after two decades of operations\, with only ~90 being AGN and blazars. \nThe Cherenkov Telescope Array Observatory (CTAO) stems as the future of ground-based gamma-ray astronomy. Its improved capabilities promise to revolutionize the field in the near future. Its first telescope\, the Large-Sized Telescope prototype (LST-1)\, is already operating in La Palma (Spain) since 2018\, therefore being not only the future but also the present in the field. In this talk I will give an overview of some of the first scientific results on AGN and blazars obtained during LST-1’s first years of operation. The seminar will conclude with a discussion of future perspectives with the fully operating CTAO. \nFecha y lugar: 27/11/2025 – 12:30 | Salón de ActosJorge Otero-SantosINFN Sezione di Padova \n 
URL:https://www.iaa.csic.es/evento/first-glimpses-of-the-extragalactic-gamma-ray-sky-with-lst-1-paving-the-way-to-ctao/
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:20251202T123000
DTEND;TZID=Europe/Paris:20251202T133000
DTSTAMP:20260521T012422
CREATED:20250930T090312Z
LAST-MODIFIED:20251127T154254Z
UID:27510-1764678600-1764682200@www.iaa.csic.es
SUMMARY:MeerKAT imaging of nearby galaxies
DESCRIPTION:Star formation is one of the dominant internal processes that drive galaxy evolution. We investigate the environmental effects on star formation activity in three nearby galaxy groups: NGC 6221\, NGC 3263 and NGC 2434. These groups were chosen to represent an evolutionary sequence ranging from the early stages to the late stages: from an interacting pair with tidal debris to a loose pre-processing group and finally to a more evolved system dominated by an elliptical galaxy. \nWe use a combination of high-resolution MeerKAT radio continuum data and WISE infrared observations to locate and measure the star formation rate in all group members. We use PAH emission as a tracer of gas heated by young stars to achieve this. In-band spectral index maps constrain the physical mechanisms driving the radio emission\, while SED fitting yields the ages and masses of a subset of the galaxies. \nDepending on the evolutionary stage of their group\, we find that galaxies occupy distinct regions of the WISE colour–colour diagram. All systems except ESO 059–G012 follow the radio–W3PAH correlation; the latter’s deviation may indicate that it has already exhausted its gas reservoir. The data also support the idea that the Vela Cloud originated from an interaction\, likely involving NGC 3263\, NGC 3256B and NGC 3256C. Finally\, our results are consistent with the presence of low-luminosity active galactic nuclei (AGN) in NGC 6221 and NGC 3256\, as previously suggested in the literature. \nFecha y lugar: 02/12/2025 – 12:30 | Sala de JuntasJuliana SaponaraInstituto Argentino de Radioastronomia (IAR) \n 
URL:https://www.iaa.csic.es/evento/meerkat-imaging-of-nearby-galaxies/
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:20251204T123000
DTEND;TZID=Europe/Paris:20251204T133000
DTSTAMP:20260521T012422
CREATED:20251030T103159Z
LAST-MODIFIED:20251204T123759Z
UID:27976-1764851400-1764855000@www.iaa.csic.es
SUMMARY:SO Colloquium: The Earth 2.0 (ET) Space Mission
DESCRIPTION:The Earth 2.0 (ET) mission\, currently in Phase B and scheduled for launch in fall 2028\, aims to discover Earth-like exoplanets using a dedicated space observatory at the Earth-Sun L2 point. It will combine six wide-field transit telescopes and one microlensing telescope\, leveraging large-format CMOS detectors for ultra-precise photometry. Over its four-year primary mission\, ET will monitor ~3 million nearby dwarf stars for transits and ~30 million stars in the Galactic bulge for microlensing events. Simulations suggest the mission will detect ~17 Earth 2.0 analogs\, ~25 free-floating Earth-mass planets\, over 4000 terrestrial-like planets\, and tens of thousands of additional exoplanets. \nThis talk will present an overview of the mission design\, technical innovations\, and its potential for exoplanet\, stellar and time-domain sciences. \nFecha y lugar: 04/12/2025 – 12:30 | Salón de ActosJian GeShanghai Astronomical Observatory \n  \n 
URL:https://www.iaa.csic.es/evento/the-earth-2-0-et-space-mission/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios,SO Colloquium
ATTACH;FMTTYPE=image/png:https://www.iaa.csic.es/wp-content/uploads/2025/07/SO-COLLOQUIUM.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20251209T123000
DTEND;TZID=Europe/Paris:20251209T133000
DTSTAMP:20260521T012422
CREATED:20251015T110641Z
LAST-MODIFIED:20260107T100028Z
UID:27740-1765283400-1765287000@www.iaa.csic.es
SUMMARY:SO Colloquium: Planetesimal vs. Pebble Accretion
DESCRIPTION:A major issue in planet formation theory is whether the terrestrial planets formed mostly by accreting asteroid-sized (~100 km) planetesimals\, or mostly by accreting small (~cm) pebbles. In either theory\, planetesimals are the first steps in formation\, and these may accrete into Mars-sized planets within the ≈2 Myr lifetime of the inner disk. Pebble accretion has been rejected for various reasons\, but those reasons don’t actually discriminate between the theories. One objection is that even mm-sized objects are commonly thought to drift into the Sun in < 2 Myr due to aerodynamic drag. This would prevent terrestrial planets from accreting pebbles with «NC» (inner-disk) isotopic composition. But it would also be a problem for formation of planetesimal parent bodies of chondrites. \nHowever\, I’ll show that the combination of the pebble trap at the dead zone inner edge\, plus turbulent diffusion of chondrules\, is quite favorable for retention of chondrule-sized pebbles\, enabling both pebble accretion and planetesimal accretion. Another objection is the geochemical constraint from Hf-W dating that Earth’s core’s formed over ~10^8 yr\, consistent with planetesimal accretion. However\, nebular H\, He\, and Ne in Earth’s deep mantle demand ingassing into a magma ocean\, and rapid core formation in ~ 10^6 yr. This geochemical constraint demands the Earth’s Hf-W age was reset during the Moon-forming impact and does not discriminate between the scenarios. What might discriminate between the formation scenarios are moderately volatile element (MVE) abundances. Whereas Mars has MVE patterns consistent with planetesimal accretion of chondrites\, Earth is depleted in MVEs. I describe a scenario by which Earth’s embryos mostly grew by accretion of MVE-depleted chondrule-sized pebbles. While Mars might have grown from planetesimals\, growth of larger planets (proto-Earth\, possibly Theia and Venus\, and super-Earth exoplanets) likely is dominated by pebble accretion. \nFecha y lugar: 09/12/2025 – 12:30 | Salón de ActosSteve DeschArizona State University\, USA \n 
URL:https://www.iaa.csic.es/evento/so-colloquium-planetesimal-vs-pebble-accretion/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios,SO Colloquium
ATTACH;FMTTYPE=image/png:https://www.iaa.csic.es/wp-content/uploads/2025/07/SO-COLLOQUIUM.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20251211T123000
DTEND;TZID=Europe/Paris:20251211T133000
DTSTAMP:20260521T012422
CREATED:20251002T110437Z
LAST-MODIFIED:20260107T100033Z
UID:27568-1765456200-1765459800@www.iaa.csic.es
SUMMARY:SO Colloquium:  MOSAIC: the multi-object spectrograph for the ELT
DESCRIPTION:MOSAIC will be a multi-object spectrograph for the ELT. It is being designed to work at visible and NIR wavelengths\, and with different observing modes. During the first years of operation of the instrument it will carry out several surveys that will focus on the most relevant key-projects in Astronomy: first galaxies\, mass assembly along the Universe evolution\, exoplanets\, etc… \nThe IAA-CSIC is contributing to the development of the instrument\, as well as to the scientific team that is defining the first observations. The Principal Investigator of the project will update the progress of the project\, both from the technological and scientific points of view. \nFecha y lugar: 11/12/2025 – 12:30 | Salón de ActosRoser PellóLaboratoire d’astrophysique de Marseille (LAM) \n 
URL:https://www.iaa.csic.es/evento/mosaic-the-multi-object-spectrograph-for-the-elt/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios,SO Colloquium
ATTACH;FMTTYPE=image/png:https://www.iaa.csic.es/wp-content/uploads/2025/07/SO-COLLOQUIUM.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20251215T130000
DTEND;TZID=Europe/Paris:20251215T133000
DTSTAMP:20260521T012422
CREATED:20251015T110754Z
LAST-MODIFIED:20251203T120633Z
UID:27743-1765803600-1765805400@www.iaa.csic.es
SUMMARY:Simulations to unlock Micro-Arcsecond Astronomy with La Palma Quantum Interferometry (LPQI)
DESCRIPTION:Stars in the night sky\, even in nearby multi-star systems\, generally appear as unresolved points of light through conventional telescopes. Achieving sub-milliarcsecond resolution at optical wavelengths requires the use of interferometric techniques. While Michelson stellar interferometers now reach baselines of up to 300 m\, extending angular resolution to even finer scales demands a complementary approach: Intensity Interferometry (II). The recent global resurgence of II has opened new possibilities for high-precision studies of massive and evolved stars. \nThe Observatorio del Roque de los Muchachos (ORM) on La Palma\, with its large-aperture telescopes and long baselines\, offers a unique platform for advancing II. In this talk\, I will present simulated results for stellar systems within the framework of the La Palma Quantum Interferometry (LPQI) initiative. These simulations focus on identifying promising stellar targets and assessing achievable signal-to-noise ratios. The results demonstrate the potential to resolve binary systems at micro-arcsecond scales\, enabling precise measurements of stellar radii and orbital parameters in close massive binaries\, modeling Roche-lobe geometries in Wolf–Rayet systems\, and establishing the foundation for exoplanet astrometry in stellar systems\, where traditional detection methods are often limited. \nFecha y lugar: 15/12/2025 – 13:00 | Salón de ActosNitu RaiAryabhatta Research Institute of Observational Sciences (ARIES)\, Nainital \n  \n 
URL:https://www.iaa.csic.es/evento/simulations-to-unlock-micro-arcsecond-astronomy-with-la-palma-quantum-interferometry-lpqi/
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:20251216T130000
DTEND;TZID=Europe/Paris:20251216T133000
DTSTAMP:20260521T012423
CREATED:20251103T085904Z
LAST-MODIFIED:20251118T091359Z
UID:27989-1765890000-1765891800@www.iaa.csic.es
SUMMARY:KM3-230213A: the ultra-high-energy neutrino detected in KM3NeT
DESCRIPTION:The detection by the KM3NeT neutrino telescope of the ultra-high-energy event KM3-230213A is a milestone in neutrino astrophysics. With an energy estimated of about 220 PeV\, it is the most energetic neutrino observed to date\, challenging the current understanding of the cosmic spectrum. Its observation opens the question of its astrophysical origin. \nIn this talk\, details on the KM3-230213A detection and observed signature will be presented\, describing the detection technique and significance assessment. Possible astrophysical sources\, including extragalactic and cosmogenic origins\, will be discussed. \nFecha y lugar: 16/12/2025 – 13:00 | Salón de ActosSergio Navas ConchaUniversidad de Granada \n 
URL:https://www.iaa.csic.es/evento/km3-230213a-the-ultra-high-energy-neutrino-detected-in-km3net/
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:20260108T123000
DTEND;TZID=Europe/Paris:20260108T133000
DTSTAMP:20260521T012423
CREATED:20251110T094048Z
LAST-MODIFIED:20260107T104840Z
UID:28715-1767875400-1767879000@www.iaa.csic.es
SUMMARY:SO Colloquium - First reallistic modeling of dust in protoplanetary disks: perspectives for future observations
DESCRIPTION:First results on modeling of light scattering by non-spherical and porous dust particles in protoplanetary disks have been obtained after a fruitful collaboration between IAA and IRyA backed by SO program: Daniel Guirado visiting IRyA\, Carlos Carrasco and Miguel Jesús Jáquez visiting IAA and Gonzalo Vargas’ SO FPI. First paper produced by this collaboration has been recently submitted for publication: «Modeling (Sub)-Millimeter Scattering Properties of Fractal and Consolidated Porous Particles: Applications to Protoplanetary Disks» and second paper is ready for submission in a few days a the time of this application: «Exploring the millimeter emission spectrum and polarization of protoplanetary disks with irregular dust particles» \nA detailed characterization of dust evolution within protoplanetary disks is essential to uncover how planets form. Only in the past decade\, with the advent of high-resolution radio interferometers such as the VLA and ALMA\, have we been able to map dust distributions in these disks with unprecedented precision. Early observations revealed an unexpected diversity of substructures —including rings\, gaps\, and asymmetric patterns— indicative of the onset of planet formation and its dynamical impact on the disk. After surveying hundreds of disks across various star-forming regions\, we are now beginning to outline multiple evolutionary pathways that may lead to planetary systems with markedly different architectures. \nBased new results of light scattering in disks produced by this SO collaboration\, basic properties of the dust such as their mass or size can be updated. And new perspectives on observations that may lead us to find out new details on the movie of the evolution of disks are open. These future observations must be matched with modelling efforts. New technological achievements and instruments to be developed and in service very soon must be matched with these modelling efforts as well: ngVLA and SKA \nFecha y lugar: 08/01/2026 – 12:30 | Salón de ActosCarlos CarrascoIRyA-UNAM \n  \n  \n  \n 
URL:https://www.iaa.csic.es/evento/first-reallistic-modeling-of-dust-in-protoplanetary-disks-perspectives-for-future-observations/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios,SO Colloquium
ATTACH;FMTTYPE=image/png:https://www.iaa.csic.es/wp-content/uploads/2025/07/SO-COLLOQUIUM.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Paris:20260113T123000
DTEND;TZID=Europe/Paris:20260113T133000
DTSTAMP:20260521T012423
CREATED:20251118T085849Z
LAST-MODIFIED:20260107T105027Z
UID:28793-1768307400-1768311000@www.iaa.csic.es
SUMMARY:Precise radial velocities with ESPRESSO: pushing the limit to 10 cm/s
DESCRIPTION:The ESPRESSO spectrograph\, mounted on the VLT\, was designed to achieve a long-term radial velocity (RV) precision of 10 cm/s\, enabling the detection of Earth-mass planets within the habitable zones (HZ) of their host stars. \nI present results from the instrument’s Guaranteed Time Observations campaign on three low-activity G\, K\, and M stars. We characterise the precision achievable from the timescales of minutes and dominated by pulsations\, to timescales of years as required for HZ planet detection. To achieve this\, we employ different RV calculation methods and activity indicators\, assessing the limiting factors of both instrumental precision and stellar RV stability. Using a comprehensive analysis\, we reach a RV floor level of 40 cm/s over a timescale of several years. \nInterestingly\, the ESPRESSO data shows no evidence for several previously announced planetary signals; we discuss the population of planets that\, while not directly observed\, remain consistent with ESPRESSO data. \nFinally\, we explore the stellar physical phenomena that can be studied to further improve RV precision and enhance our planet detection capabilities. This is key for the future precise RV campaigns as enabled by ESPRESSO and similar instruments. \nFecha y lugar: 13/01/2026 – 12:30 | Salón de ActosPedro FigueiraIAA-CSIC \n  \n 
URL:https://www.iaa.csic.es/evento/precise-radial-velocities-with-espresso-pushing-the-limit-to-10-cm-s/
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:20260115T123000
DTEND;TZID=Europe/Paris:20260115T133000
DTSTAMP:20260521T012423
CREATED:20251118T090542Z
LAST-MODIFIED:20260116T125349Z
UID:28810-1768480200-1768483800@www.iaa.csic.es
SUMMARY:From cluster detection to galaxy alignment: an overview of SCALE with S-PLUS survey
DESCRIPTION:Galaxy clusters and groups are vital tools for exploring and understanding the Universe. \nThis presentation focuses on results based on the SCALE sample from the Southern Photometric Local Universe Survey (S-PLUS)\, including galaxy cluster detection\, membership estimation and characterization\, matching with eROSITA X-ray data\, and a detailed study of galaxy spatial alignments out to 6R200. \nWe discuss the purity and completeness of the resulting catalogs using X-ray comparisons\, potential biases introduced by the matching technique\, the preprocessing of galaxies associated with filaments\, and the parameters that enhance the alignment signal between brightest cluster galaxies (BCGs) and their satellite populations. Together\, these analyses demonstrate the potential of the S-PLUS survey for cluster identification and environmental studies. \nFecha y lugar: 15/01/2026 – 12:30 | Salón de ActosLia DoubrawaUniversity of Helsinki – Finland\, Universidade de São Paulo – Brazil \n  \n  \n  \n 
URL:https://www.iaa.csic.es/evento/from-cluster-detection-to-galaxy-alignment-an-overview-of-scale-with-s-plus-survey/
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:20260119T130000
DTEND;TZID=Europe/Paris:20260119T140000
DTSTAMP:20260521T012423
CREATED:20260113T104959Z
LAST-MODIFIED:20260113T114250Z
UID:29103-1768827600-1768831200@www.iaa.csic.es
SUMMARY:High energy blazar physics in the Multi-Messenger context
DESCRIPTION:Active galactic nuclei (AGN) are among the most powerful sources in the Universe\, dominating the non-thermal energy output across nearly all electromagnetic bands. Understanding the mechanisms behind this emission\, such as accretion onto supermassive black holes\, particle acceleration\, magnetic field generation\, and shock formation in relativistic plasma\, is essential for interpreting high-energy and multi-messenger observations. These processes can be best probed through coordinated studies combining very-high-energy and high-angular-resolution observations. \nI will present recent results from polarization VLBI studies that trace jet formation\, acceleration\, and magnetic field structure in AGN on parsec scales. Our observations provide clear evidence for a net toroidal magnetic field in a current-carrying blazar jet. We also find that blazars viewed at extremely small angles to the line of sight can naturally resolve the long-standing «Doppler factor crisis\,» reconciling the low apparent jet speeds from VLBI with the high Doppler factors inferred from very-high-energy observations. \nOur results highlight the central role of relativistic beaming in shaping the gamma-ray and neutrino emission of blazars. This suggests that parent PeV-scale protons exhibit relativistic bulk motion and offers new constraints for models of their multi-messenger output. \nFecha y lugar: 19/01/2026 – 13:00 | Salón de ActosYuri KovalevMax Planck Institute for Radio Astronomy \n 
URL:https://www.iaa.csic.es/evento/high-energy-blazar-physics-in-the-multi-messenger-context/
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:20260129T123000
DTEND;TZID=Europe/Paris:20260129T133000
DTSTAMP:20260521T012423
CREATED:20251201T092256Z
LAST-MODIFIED:20260123T095536Z
UID:28868-1769689800-1769693400@www.iaa.csic.es
SUMMARY:Fantastic PeVatrons and where to find them
DESCRIPTION:Cosmic rays with energies up to about 3 PeV corresponding to the ‘knee’ feature in the observed spectrum are believed to be of Galactic origin. There is however no indisputable evidence\, neither observational nor theoretical\, that Galactic sources can supply enough protons of these high energies. A long-standing paradigm constitutes that the bulk of Galactic cosmic rays at least at lower energies are produced in supernova remnants\, which is based mainly on the fact that supernova explosions can provide enough energy to explain the energy density of cosmic rays in the Galaxy. \nBut in recent years it becomes more and more evident that protons can reach PeV energies in supernova remnants only in some special and extreme cases. This together with recent discoveries (notably from the LHAASO experiment) of the gamma-ray emission at multi-PeV energies from a number of sources stimulated discussions of plausible alternatives among which compact massive star clusters and microquasars seem to be the most promising candidates. \nIn this talk I will discuss the current status of the search for PeVatrons from the perspective of theory and modeling focusing on capabilities of the supernova remnant paradigm also extending it to the supernovae explosions within compact stellar clusters. \nFecha y lugar: 29/01/2026 – 12:30 | Salón de ActosIurii SushchCentro de Investigaciones Energéticas\, Medioambientales y Tecnológicas (CIEMAT) \n 
URL:https://www.iaa.csic.es/evento/fantastic-pevatrons-and-where-to-find-them/
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:20260206T130000
DTEND;TZID=Europe/Paris:20260206T140000
DTSTAMP:20260521T012424
CREATED:20260107T095857Z
LAST-MODIFIED:20260205T083046Z
UID:29049-1770382800-1770386400@www.iaa.csic.es
SUMMARY:SO Colloquium - SDSS-V and beyond: status of the LVM and the new AS5 proposal
DESCRIPTION:We present here the state-of-the-art the Local Volume Mapper project and the new proposed After-Sloan-5 proposal (future SDSS-VI)\, making an emphasis in the stronger contributions in which me and my team has been involved: the development of the LVM-DAP\, the participation in the data analysis and science production\, the current and future DR\, and the upcoming new generation of the SDSS survey. \nThe possible participation of Spanish institutions\, and in particular the IAA and the Calar Alto observatory\, would be discussed. \nFecha y lugar: 06/02/2026 – 13:00 | Salón de ActosSebastián SánchezInstituto de Astronomía\, UNAM \n 
URL:https://www.iaa.csic.es/evento/sdss-v-and-beyond-status-of-the-lvm-and-the-new-as5-proposal/
LOCATION:IAA – CSIC\, Glorieta de la Astronomía\, Granada\, España
CATEGORIES:Seminarios,SO Colloquium
ATTACH;FMTTYPE=image/png:https://www.iaa.csic.es/wp-content/uploads/2025/07/SO-COLLOQUIUM.png
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END:VCALENDAR