BEGIN:VCALENDAR VERSION:2.0 PRODID:-//https://astronomia.uc.cl/2jucext1/institutoastrofisica///NONSGML kigkonsult.se iCalcreator 2.10.15// METHOD:PUBLISH BEGIN:VEVENT UID:20260519T015144-04-819769Ktvs@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION:Lisa Kewley (Australian National University\; Director\, ASTRO 3D)\nASTRO 3D and Galaxy Evolution\n \;\nThe ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) is a $40M Centre of Ex cellence\, which is producing a comprehensive picture of the build up of m ass\, angular momentum\, and the chemical elements from the first stars\, to (and including) the Milky Way. Our surveys include the measurement of t he power spectrum at the Epoch of Reionization with the Murchison Widefiel d Array (MWA)\, large HI surveys with the Square Kilometre Array Pathfinde r (ASKAP)\, the ongoing Australian optical integral field surveys of 10^5 galaxies (SAMI\, followed by HECTOR)\, a large galaxy evolution program co mbining HST\, Keck\, and ESO spectroscopy of galaxies from z=6 to z=0.5\, and the major Australian Galactic Archaeology program (GALAH) to track the chemical history and accretion history of our Milky Way through GAIA and the HERMES instrument on the Anglo Australian Telescope. \; I will des cribe the recent discoveries made in ASTRO 3D\, our preparation for JWST s pectral analysis\, as well as providing an update on our ambitious equity and diversity programs\, and our nationwide education and public outreach programs.\n \; https://astronomia.uc.cl/2jucext1/institutoastrofisica/ es/instituto/coloquios/evento/445-astro-3d-and-galaxy-evolution-dr-lisa-ke wley DTSTART:20210316T200000Z DTEND:20210316T210000Z LOCATION:Santiago Chile () SUMMARY:ASTRO 3D and Galaxy Evolution - Dr. Lisa Kewley URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/445-astro-3d-and-galaxy-evolution-dr-lisa-kewley END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8209IOh7nU@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION:Marcelo Gleiser (University of Dartmouth)\nEmergent Complexity in the Universe: \; An Information-Entropic Approach\n \;\nFrom at oms to stars\, physically-bound systems result from the interplay between attractive and repulsive interactions. In this lecture\, I will introduce a new measure of complexity called 'Configurational Entropy'. Inspired by Shannon's information entropy\, I will show how the configurational entrop y encodes information about the shape and the stability of various physica l objects\, and how it can be used as an efficient measure of emerging com plexity for static and dynamic phenomena. Applications will include solito ns\, compact astrophysical objects\, spontaneous symmetry breaking\, and i nflationary cosmology.\n \;\n \;\n \; https://astronomia.uc.cl /2jucext1/institutoastrofisica/es/instituto/coloquios/evento/447-emergent- complexity-in-the-universe-an-information-entropic-approach-marcelo-gleise r DTSTART:20210323T193000Z DTEND:20210323T203000Z LOCATION:Santiago Chile () SUMMARY: Emergent Complexity in the Universe: An Information-Entropic Appr oach -Marcelo Gleiser URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/447-emergent-complexity-in-the-universe-an-information-entro pic-approach-marcelo-gleiser END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-82193pHvdV@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION:Marcin Sawicki (Saint Mary's University)\nCLAUDS: The CFHT Larg e Area U-band Deep Survey\n \;\nThe CFHT Large Area U-band Deep Survey (CLAUDS) uses ~70 nights of dedicated dark-time imaging (plus significant additional archival data) to map a representative 18.6 square degrees of the Universe to a median depth of U = 27.1 AB (5?). \; These are the d eepest U-band images ever assembled over this large \; area.\nThese CF HT MegaCam data are combined with the optical (grizy + narrowband) imaging being taken to comparable depths by Subaru’s HSC camera in the same field s. Combining the U and optical data allows the selection of \; z~2-3 s tar-forming galaxies and greatly improves photometric redshift performance at z<\;1\, allowing science projects that explore 85% of cosmic time wi th excellent statistics and that are virtually free of cosmic variance.\nW ith the CLAUDS and Subaru HSC data now in hand and merged\, we have entere d the scientific exploitation phase\, and I will show some example science applications of this unmatched dataset\, including galaxy stellar mass fu nctions\, galaxy-galaxy mergers\, and satellite distributions around massi ve central galaxies.\n \;\n \;\n \; https://astronomia.uc.cl/2 jucext1/institutoastrofisica/es/instituto/coloquios/evento/449-clauds-the- cfht-large-area-u-band-deep-survey-marcin-sawicki DTSTART:20210330T193000Z DTEND:20210331T014600Z LOCATION:Santiago Chile () SUMMARY: CLAUDS: The CFHT Large Area U-band Deep Survey - Marcin Sawicki URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/449-clauds-the-cfht-large-area-u-band-deep-survey-marcin-saw icki END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8230egeUPr@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION:Anne Marie Madigan (University of Colorado)\nCollective Gravity in the Outer Solar System\n \;\nThere’s something odd going on in our solar system. While the planets move on nearly-circular orbits in a well- defined plane\, the minor planets beyond Neptune appear to cluster togethe r in a highly-inclined\, eccentric\, and tilted structure. Astronomers hav e invoked the presence of an additional planet (Planet 9) or even a primor dial black hole in explanation. In this talk I will show that these theori es may be unnecessary. In analogy with spiral arms and bars in galaxies\, the collective gravity of individually small but collectively massive bodi es can create such structures in the outer solar system.\n \;\n \; \n \; https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instit uto/coloquios/evento/451-collective-gravity-in-the-outer-solar-system-anne -marie-madigan DTSTART:20210406T193000Z DTEND:20210406T203000Z LOCATION:Santiago Chile () SUMMARY: Collective Gravity in the Outer Solar System - Anne Marie Madigan URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/451-collective-gravity-in-the-outer-solar-system-anne-marie- madigan END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8239zBtAN8@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION: \;\nFrancoise Combes (Observatory of Paris)\nCircumnuclear molecular disks: role in AGN fueling and feedback\n \;\n \;\nThe gas inflows directly fueling AGN are now traceable with current high-resol ution observations with ALMA and NOEMA.\nDynamical mechanisms are essentia l to exchange angular momentum and drive the gas to the super-massive blac k hole. \nWhile at 100pc scale\, the gas is sometimes stalled in nuclear r ings\, recent observations reaching ~10pc scale (or 50mas)\, \ninside the sphere of influence of the black hole\, may bring smoking gun evidence of fueling\, within a randomly oriented nuclear molecular disk.\nObservations of AGN feedback will be presented\, together with the suspected responsib le mechanisms. Molecular outflows are frequently \ndetected in active gala xies\, and the ALMA and NOEMA resolution gives clues to their origin\, eit her radiative of kinetic AGN mode\, or starburst. \nWhen driven by AGN wit h near escape velocity\, these outflows are therefore a clear way to moder ate or suppress star formation.\n \;\n \;\n \; https://astrono mia.uc.cl/2jucext1/institutoastrofisica/es/instituto/coloquios/evento/455- circumnuclear-molecular-disks-role-in-agn-fueling-and-feedback-francoise-c ombes DTSTART:20210413T200000Z DTEND:20210413T210000Z LOCATION:Santiago Chile () SUMMARY: Circumnuclear molecular disks: role in AGN fueling and feedback - Francoise Combes URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/455-circumnuclear-molecular-disks-role-in-agn-fueling-and-fe edback-francoise-combes END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8249zCToPb@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION: \;\nStefano Andreon (INAF-OA Brera)\n \;\nGas-poor clu sters: what kind of beasts are they?\n \;\n \;\n \;\nThe known variety of galaxy clusters is constantly increasing with our \; progr ess in understanding the severity of selection effects on observational sa mples and with obvious implications on cosmology and cluster physics. In t he talk\, after a general introduction on galaxy clusters and a reminder o n \; selection effects\, I present perhaps the first X-ray unbiased sa mple of clusters with known masses and X-ray follow-up\, its more variegat e nature compared to clusters selected by the intracluster medium (X-ray o r SZ)\, and first results based on a deeper X-ray follow-up of a few of th em.\n \;\n \;\n \;\n \; https://astronomia.uc.cl/2jucext1/ institutoastrofisica/es/instituto/coloquios/evento/457-gas-poor-clusters-w hat-kind-of-beasts-are-they-stefano-andreon DTSTART:20210420T153000Z DTEND:20210420T163000Z LOCATION:Santiago Chile () SUMMARY:Gas-poor clusters: what kind of beasts are they? - Stefano Andreon URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/457-gas-poor-clusters-what-kind-of-beasts-are-they-stefano-a ndreon END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8259S4aw1p@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION: Amelia Stutz \nUniversidad de Concepcion\nCluster formation an d gas kinematics in high mass clouds.\n \;\n \;\nBy observationall y scrutinizing the nearest high mass clouds and\nprotoclusters\, we gain n ew insights into cluster formation physics.\nThe Integral Shaped Filament (ISF) is home to the nearest significant\nprotocluster\, the Orion Nebula Cluster (ONC/M42). \; Based on a high\ndensity of observables of both the gas and stars\, we previously\nproposed the 'slingshot' mechanism\, re quiring that the gas ISF\noscillate ejecting stars. The B-field morphology (possibly helical)\nand strength\, compared with the gas mass distributio n\, indicates that\nmagnetic instabilities may be propagating through the cloud driving\nthe oscillations in the ISF. These may be responsible for t he\nslingshot. \; The gas kinematics exhibit twisting and turning feat ures\nthat may be consistent with rotation and helical structures in the\n dense gas. \; We show that the stellar density follows a Plummer profi le\nwhile the gas follows a cylindrical power law. \; The stellar\ncon tribution to the gravitational field is nearly equal to that of the\ngas a t r=a. \; At all other radii the field is gas-dominated. \; The\nc luster crossing time is ~ 0.5 Myr\, nearly identical to the filament\nosci llation timescale. \; These results reveal an intimate connection\nbet ween the stars and the gas\, such that tidal effects due to filament\nosci llations may set the protocluster structure. \; That is\, the gas\nden sity regulates the star density in the ONC. Meanwhile\, in\nCalifornia clo ud\, which has the same mass as Orion but is at an\nearlier evolutionary s tage (~1/10th the protostars)\, we detect\nrotation in cluster-forming fil ament L1482. \; Results in extragalactic\nsystems show that cloud rota tion is set by the overall galaxy rotation\nand not consistent with e.g. c loud-collision models. Combined\, these\nresults may indicate that velocit y gradients in Milky Way\nprotoclusters are naturally explained by rotatio n (and helicity)\,\nwhich is established on large scales of galaxy disks a nd then\npercolates down to protocluster and possibly even to the tiny sca les\nof protostars.\n \;\n \; https://astronomia.uc.cl/2jucext1/in stitutoastrofisica/es/instituto/coloquios/evento/465-cluster-formation-and -gas-kinematics-in-high-mass-clouds-amelia-stutz DTSTART:20210427T193000Z DTEND:20210427T203000Z LOCATION:Santiago Chile () SUMMARY: Cluster formation and gas kinematics in high mass clouds -Amelia Stutz URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/465-cluster-formation-and-gas-kinematics-in-high-mass-clouds -amelia-stutz END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8274ae9dgP@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION: \;\nYanchuan Cai (University of Edinburgh)\nCosmology with the Cosmic Web\n \;\nOn large scales\, the matter distribution of the Universe follows a web-like pattern\, consisting of knots\, filaments\, s heets and voids. The cosmic-web is a non-Gaussian field\, containing inval uable information about cosmology and astrophysics. I will summarise recen t research activities in trying to extract some of this information\, and how we can use statistics of the cosmic-web to tackle some of the major pr oblems in modern-day cosmology.\n \;\n \;\n \; https://astrono mia.uc.cl/2jucext1/institutoastrofisica/es/instituto/coloquios/evento/467- cosmology-with-the-cosmic-web-yanchuan-cai DTSTART:20210504T193000Z DTEND:20210504T203000Z LOCATION:Santiago Chile () SUMMARY:Cosmology with the Cosmic Web - Yanchuan Cai URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/467-cosmology-with-the-cosmic-web-yanchuan-cai END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-828288rp8W@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION: https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/inst ituto/coloquios/evento/469-jason-dexter-university-of-colorado DTSTART:20210518T193000Z DTEND:20210518T203000Z LOCATION:Santiago Chile () SUMMARY:Jason Dexter - University of Colorado URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/469-jason-dexter-university-of-colorado END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8288LhEX4o@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION: \;\nSara Ellison (University of Victoria)\nGas and star fo rmation in the nearby universe with the ALMA-MaNGA QUEnching and STar form ation (ALMaQUEST) survey.\n\nUnderstanding the processes that regulate sta r formation in galaxies remains at the heart of modern extra-galactic astr onomy\, and debate continues as to why some galaxies exhibit powerful star bursts whilst others are largely dormant. \; The key to progress in th is arena lies with assembling large\, diverse samples of galaxies for whic h we can measure all of the critical ingredients\, such as the current sta r formation rate (SFR) and gas content. \; However\, it is insufficien t to simply measure global galactic quantities\, as we know that a given g alaxy will manifest considerable internal diversity in its star formation activity. \; It is therefore essential to study gas and star formation on spatially resolved scales. \; The ALMA-MaNGA QUEnching and STar fo rmation (ALMaQUEST) survey combines maps of stellar properties obtained fr om the MaNGA (optical) integral field unit survey with ALMA CO (1-0) maps on a common kpc-scale grid\, in order to tackle questions of star formatio n in local galaxies. \; The 46 galaxies in the ALMaQUEST sample span a wide range of SFRs\, including both normal star forming galaxies\, as wel l as those both on their way to quenching\, and those undergoing starburst s. \; In this talk\, I will present the ALMaQUEST view of understandin g the interplay of gas and star formation across this broad galactic lands cape.\n \; https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/i nstituto/coloquios/evento/471-gas-and-star-formation-in-the-nearby-univers e-with-the-alma-manga-quenching-and-star-formation-almaquest-survey-sara-e llison DTSTART:20210525T193000Z DTEND:20210525T203000Z LOCATION:Santiago Chile () SUMMARY:Gas and star formation in the nearby universe with the ALMA-MaNGA Q UEnching and STar formation (ALMaQUEST) survey - Sara Ellison URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/471-gas-and-star-formation-in-the-nearby-universe-with-the-a lma-manga-quenching-and-star-formation-almaquest-survey-sara-ellison END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8301ddkgUS@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION:How do galaxies form? New insights from the FIRE and the role o f the circumgalactic medium\n \;\nClaude-André Faucher-Giguère \; \nNorthwestern University\n \;\n\nAbstract: Galaxies are remarkably di verse in their properties\, ranging from irregular to disky to elliptical in morphology\, and from blue to red in color. At the same time\, when ana lyzed systematically\, galaxy populations exhibit striking regularities\, with clear trends with mass and redshift. How does this 'regular complexit y' emerge from the hot Big Bang? I will present results from the FIRE simu lations which shed some light onto the processes that shape galaxies. The FIRE zoom-in simulations resolve the multiphase interstellar medium of gal axies and model several different feedback processes (including Type II/Ia supernovae\, stellar winds\, and radiation) while including the cosmologi cal environment. I will highlight recent results on the formation of disk galaxies\, the 'burstiness' of star formation\, and galactic winds. Our ne w results indicate that transitions in each of these important phenomena c an be simultaneously explained by a phase transition in the inner circumga lactic medium\, 'inner CGM virialization' (ICV)\, and arise from the inter play between feedback energy produced on small scales and the physics of h alo gas on larger scales. https://astronomia.uc.cl/2jucext1/institutoastro fisica/es/instituto/coloquios/evento/473-how-do-galaxies-form-new-insights -from-the-fire-and-the-role-of-the-circumgalactic-medium-claude-andre-fauc her-giguere DTSTART:20210601T193000Z DTEND:20210601T203000Z LOCATION:Santiago Chile () SUMMARY:How do galaxies form? New insights from the FIRE and the role of th e circumgalactic medium - Claude-André Faucher-Giguère URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/473-how-do-galaxies-form-new-insights-from-the-fire-and-the- role-of-the-circumgalactic-medium-claude-andre-faucher-giguere END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-83130VhJaI@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION:The thermodynamics of rotating black hole clusters\nYuri Levin \nCenter for Computational Astrophysics\, Flariton Institute\n \;\nSta tistical physics has a bad track record in describing large-N gravitationa l systems.\nIt has become clear over the last several years that there is a remarkable exception\nto this rule. Resonant relaxation due to orbit-ave raged secular dynamics in galactic nuclei\ndrives them to states of therma l and rotational equilibria on an astronomically short timescale.\nStatist ical physics becomes a powerful\, yet under-appreciated tool to study such systems.\nI will introduce the general formalism (due mostly to Touma and Tremaine\, but going as far back as Lynden-Bell)\, \;\nas well as a n ovel numerical algorithm for finding equilibria due to Andrei Gruzinov.&nb sp\;\nThere are fun applications: phase transitions leading to lopsided pr ecessing equilibria (such as the nucleus of\nAndromeda)\, and strong clust ering in eccentricity and inclination of stellar-mass black holes.\nI will use statistical physics to argue that secular-dynamical friction must exi st and that moreover\, it\nplays a huge role in galactic nuclei\, turning rotating clusters into \;\nflywheels that control the orbits of all he avy objects inside them\, such as stellar discs and IMBHs.\nI will specula te on its effect on the spin of the supermassive black hole itself.\n  \; https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/477-the-thermodynamics-of-rotating-black-hole-clusters-yuri- levin DTSTART:20210615T040000Z LOCATION:Santiago Chile () SUMMARY:The thermodynamics of rotating black hole clusters - Yuri Levin URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/477-the-thermodynamics-of-rotating-black-hole-clusters-yuri- levin END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8324vg5nPU@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION: Stellar clustering connecting the formation and evolution of g alaxies to the formation and evolution of us\nDiederik Kruijssen \n(Heidel berg University)\n \;\nThe clustered nature of star formation leaves a long-term imprint on galaxies\, stars\, and planets. At young ages\, stel lar clustering subdivides galaxies into individual building blocks undergo ing vigorous\, feedback-driven life cycles that vary with the galactic env ironment. These units structure the interstellar medium spatially\, dynami cally and chemically\, and collectively define how galaxies form stars. At old ages\, the relics of clustered star formation persist as ancient glob ular clusters\, which hold a wealth of information allowing us to reconstr uct the assembly histories of galaxies\, culminating in the reconstruction of the Milky Way’s merger tree. Towards smaller scales\, stellar clusteri ng has a measurable impact on the evolution of protoplanetary discs\, the architectures of planetary systems\, and the properties of planets themsel ves. I will discuss how this web of physical processes across a hierarchy of scales defines the cosmic ecosystem that we live in\, and demonstrate t hat stellar clustering is at its focal point.\n \; https://astronomia. uc.cl/2jucext1/institutoastrofisica/es/instituto/coloquios/evento/479-stel lar-clustering-connecting-the-formation-and-evolution-of-galaxies-to-the-f ormation-and-evolution-of-us-diederik-kruijssen DTSTART:20210622T193000Z DTEND:20210622T203000Z LOCATION:Santiago Chile () SUMMARY:Stellar clustering connecting the formation and evolution of galaxi es to the formation and evolution of us - Diederik Kruijssen URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/479-stellar-clustering-connecting-the-formation-and-evolutio n-of-galaxies-to-the-formation-and-evolution-of-us-diederik-kruijssen END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8335OFeSrr@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION: \;Planet-forming disks in the era of ALMA\nLaura Perez\nUn iversidad de Chile\nThe process of disk evolution and planet formation wil l leave an imprint on the distribution of solid particles at different loc ations in a protoplanetary disk\, resulting in \;a variety of substruc ture over large and small scales. The focus of recent ALMA observations at high angular resolution has been to characterize the underlying \;sub structure of these disks\, from dust continuum and gas tracer images with spatial resolution of a few to tens of astronomical units. In this colloqu ium\, I will discuss \;recent results related to observing these subst ructures at multiple wavelengths\, studying the origin of spiral arms in a particular protoplanetary disk\, and ongoing \;searches for the plane ts that may cause the observed substructure. These results gives us new in sights into planet-forming disk in the era of ALMA.\n \;\n \;\n&nb sp\;\n \; https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/in stituto/coloquios/evento/481-planet-forming-disks-in-the-era-of-alma-laura -perez DTSTART:20210629T193000Z DTEND:20210629T203000Z LOCATION:Santiago Chile () SUMMARY:Planet-forming disks in the era of ALMA - Laura Perez URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/481-planet-forming-disks-in-the-era-of-alma-laura-perez END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8345DzOwA4@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION:The multi-band survey S-PLUS - Southern Photometric Local Unive rse Survey\nClaudia Mendes de Oliveira\nUniversity of Sao Paulo\n \;\n  \;\n \;\n \;\nThis talk will describe S-PLUS\, done with the T80-South telescope\, the Brazilian robotic telescope located in Cerro Tol olo\, and will highlight the potential of the combination of a 12-band opt ical filter system and a wide-area coverage\, in several different areas o f study. We would like to specifically investigate possible S-PLUS collabo rations with the Chilean community. The T80-South telescope is equipped wi th a 9.2k$\times$9.2k 10$\micron$-pixel E2V detector giving a field of vie w of 2 deg$^2$ with a plate scale of 0\farcs55 pixel$^{-1}$. The filter sy stem used by S-PLUS consists of 5 SDSS filters and 7 narrowband filters ce ntered on prominent spectral features (i.e.\, O{\sc{ii}}\, Ca H$+$K\, D$_n $4000\, H$\delta$\, Mg$b$\, H$\alpha$ and CaT). S-PLUS will cover an area of about 8000 square degrees\, and it is ideal to find low-metallicity and blue-horizontal branch stars and high redshift quasars\, determine the ph ysical properties of the nearby galaxy population selected based on accura te 12-band photometric redshifts\, and to map the large scale structure in the nearby universe\, among other topics. S-PLUS will cover an additional $\sim$1300 deg$^2$ of the Galactic disk and bulge. Here we will describe the main characteristics of the survey and will highlight the science done so far and planned. \;Part of the survey data is already publicly ava ilable to the international community through the S-PLUS DR-2 at www.splus .cloud.\n \; https://astronomia.uc.cl/2jucext1/institutoastrofisica/es /instituto/coloquios/evento/483-the-multi-band-survey-s-plus-southern-phot ometric-local-universe-survey-claudia-mendes-de-oliveira DTSTART:20210803T193000Z DTEND:20210803T203000Z LOCATION:Santiago Chile () SUMMARY:The multi-band survey S-PLUS - Southern Photometric Local Universe Survey -- Claudia Mendes de Oliveira URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/483-the-multi-band-survey-s-plus-southern-photometric-local- universe-survey-claudia-mendes-de-oliveira END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8358gVPKvm@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION:Ricardo Amorin\nUniversidad de La Serena https://astronomia.uc. cl/2jucext1/institutoastrofisica/es/instituto/coloquios/evento/485-ricardo -amorin-universidad-de-la-serena DTSTART:20210817T193000Z DTEND:20210817T203000Z LOCATION:Santiago Chile () SUMMARY:Ricardo Amorin - Universidad de la Serena URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/485-ricardo-amorin-universidad-de-la-serena END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8364474erO@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION:Maria Argudo Fernandez\nPontificia Universidad Católica de Valp aríso https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/ coloquios/evento/487-maria-argudo-fernandez-pontificia-universidad-catolic a-de-valpariso DTSTART:20210831T193000Z DTEND:20210831T203000Z LOCATION:Santiago Chile () SUMMARY:Maria Argudo Fernandez - Pontificia Universidad Catolica de Valpari so URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/487-maria-argudo-fernandez-pontificia-universidad-catolica-d e-valpariso END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8370Vpu8aX@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION: Stellar variability in the Gaia Era: the Gaia DR3 harvest\n G isella Clementini INAF - Os servatorio di Astrofisica e Scienza dello Spazio (OAS)\, Bologna\n\n\nThe last couple of decades have seen a true revolution in the field of stellar variability thanks to the increasing number of ground/space-based facilit ies and surveys that have been collecting multi-epoch photometry over larg e portions of the sky.\n\nA leading role in this revolution is played by G aia\, the ESA cornerstone mission that monitors the whole sky since July 2014\, obtaining astrometric parameters (positions\, parallaxes and prope r motions) and multi-epoch photometry in three different pass-bands (Gaia G\, G_BP and G_RP) of sources down to a limiting magnitude G = 21 mag. Th e spacecraft also simultaneously collects spectroscopy with the Radial Vel ocity Spectrometer (RVS) of the sources brighter that V ? 16 mag.\n\nIn th e first half of 2022\, the second instalment of Gaia third data release (D R3)\, will publish time series multi-band photometry and parameters for ab out 14 million sources and more that 20 different variability types. Epoch RVS radial velocities will be also released for about 2000 RR Lyrae stars and Cepheids.\n\nWe discuss some of the Gaia DR3 variability results\, fo cussing more specifically on the RR Lyrae stars and Cepheids\, in light of the impact these variable stars have on the definition of the cosmic dist ance ladder and the study of resolved stellar\npopulations in and beyond t he Milky Way. Future perspectives opened by upcoming new facilities such a s the Vera Rubin Observatory and spectrographs such as WEAVE\, MOONS and 4 MOST will also be briefly considered. https://astronomia.uc.cl/2jucext1/in stitutoastrofisica/es/instituto/coloquios/evento/489-stellar-variability-i n-the-gaia-era-the-gaia-dr3-harvest-gisella-clementini DTSTART:20210914T193000Z DTEND:20210914T203000Z LOCATION:Santiago Chile () SUMMARY:Stellar variability in the Gaia Era: the Gaia DR3 harvest - Gisella Clementini URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/489-stellar-variability-in-the-gaia-era-the-gaia-dr3-harvest -gisella-clementini END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8384F0Luc6@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION: \;\nOur Astrochemical Origins\nPaola Caselli \;\n(Max- Planck-Institute for Extraterrestrial Physics)\nAll ingredients to make st ars like our Sun and planets like our Earth are present in dense cold inte rstellar clouds. In these 'stellar-system precursors' an active chemistry is already at work\, as demonstrated by the presence of a rich variety of organic molecules in the gas phase and icy mantles encapsulating the sub-m icrometer dust grains\, the building blocks of planets. Here\, I’ll presen t a journey from the earliest phases of star formation to protoplanetary d isks\, with links to our Solar System\, highlighting the crucial role of a strochemistry as a powerful diagnostic tool of the various steps present i n the journey.\n \; https://astronomia.uc.cl/2jucext1/institutoastrofi sica/es/instituto/coloquios/evento/475-our-astrochemical-origins-paola-cas elli DTSTART:20210928T193000Z DTEND:20210928T203000Z LOCATION:Santiago Chile () SUMMARY:Our astrochemical origins - Paola Caselli URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/475-our-astrochemical-origins-paola-caselli END:VEVENT BEGIN:VEVENT UID:20260519T015144-04-8393txcxt9@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260519T055144Z DESCRIPTION:Do dark-matter-deficient dwarf galaxies present a challenge to the LCDM paradigm?\nSugata Kaviraj\nUniversity of Hertfordshire\n \;\n In the standard LCDM paradigm\, dwarf galaxies are expected to be dark mat ter-rich\, as baryonic feedback is thought to quickly drive gas out of the ir shallow potential wells and quench star formation at early epochs. Rece nt observations of local dwarfs with extremely low dark matter content app ear to contradict this picture\, potentially bringing the validity of the standard model into question. We use New Horizon\, a high-resolution cosmo logical simulation\, to demonstrate that sustained stripping of dark matte r\, in tidal interactions between a massive galaxy and a dwarf satellite\, naturally produces dwarfs that are dark matter-deficient\, even though th eir initial dark matter fractions are normal. The process of dark matter s tripping is responsible for the large scatter in the halo-to-stellar mass relation in the dwarf regime. The degree of stripping is driven by the clo seness of the orbit of the dwarf around its massive companion and\, in ext reme cases\, produces dwarfs with halo-to-stellar mass ratios as low as un ity\, consistent with the findings of recent observational studies. ~30 pe r cent of dwarfs show some deviation from normal dark matter fractions due to dark matter stripping\, with 10 per cent showing high levels of dark m atter deficiency (M_halo/M_?<\; 10). Given their close orbits\, a signif icant fraction of dark matter-deficient dwarfs merge with their massive co mpanions (e.g. ~70 per cent merge over time-scales of ~3.5 Gyr)\, with the dark matter-deficient population being constantly replenished by new inte ractions between dwarfs and massive companions. The creation of these gala xies is therefore a natural by-product of galaxy evolution and their exist ence is not in tension with the standard paradigm.\n \; https://astron omia.uc.cl/2jucext1/institutoastrofisica/es/instituto/coloquios/evento/491 -do-dark-matter-deficient-dwarf-galaxies-present-a-challenge-to-the-lcdm-p aradigm-sugata-kaviraj DTSTART:20211026T183000Z DTEND:20211026T193000Z LOCATION:Santiago Chile () SUMMARY:Do dark-matter-deficient dwarf galaxies present a challenge to the LCDM paradigm? - Sugata Kaviraj URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/col oquios/evento/491-do-dark-matter-deficient-dwarf-galaxies-present-a-challe nge-to-the-lcdm-paradigm-sugata-kaviraj END:VEVENT END:VCALENDAR