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• 17.07.2026 - Arunima Arunima (ANU) & Han Wang (MPA)

  Strong lensing meets stellar dynamics: from cosmology to galaxy evolution
  Han Wang (MPA)

  Time-delay cosmography with strongly lensed quasars measures the Hubble constant independently of the distance ladder and the CMB, but its accuracy is limited by the mass-sheet degeneracy (MSD), which lensing data alone cannot break. Stellar dynamics of the lens galaxy provides the missing information. I will present GLaD, a GPU-accelerated framework for self-consistent joint modeling of strong lensing and stellar dynamics, which reduces a full Bayesian analysis from months to days. Using simulated HST imaging and JWST-like IFU kinematics of the lensed quasar RXJ1131-1231, I will show that the MSD can be broken with a single lens, yielding 4% precision on H0, and I will discuss the first application to the real JWST observations of RXJ1131 and the practical challenges that dominate the real-data error budget. For the nearby lens ESO0286, the Einstein mass from HST extended-image modeling anchors triaxial Schwarzschild models of MUSE kinematics, tightening the outer mass profile and constraining the stellar initial mass function to be Kroupa-like, in contrast to the heavier IMFs reported at higher redshift.

   

  Their currents turn awry, and lose the name of action: evolution of stellar actions in a Milky Way-like simulation
  Arunima Arunima (ANU)

  The Milky Way disc preserves a record of its past in the motions and spatial distribution of stars. A central goal of Galactic archaeology is to use this information to reconstruct where stars formed. Many dynamical reconstruction techniques rely on the assumption that stellar orbital actions are conserved, which is true for axisymmetric and time-invariant potential. However, the Galactic disk is not static: transient spiral arms, giant molecular clouds (GMCs), and other non-axisymmetric structures continuously perturb stellar orbits, potentially erasing signatures of common birth environments. In this talk, I will present results from high-resolution magnetohydrodynamic simulations of a Milky Way–like galaxy to quantify how stellar orbital actions evolve in a realistic, time-dependent disc. I will show that stellar actions undergo stochastic diffusion on surprisingly short (~100 Myr) timescales with radial actions evolving more slowly due to spiral structure and vertical actions evolving more quickly due to perturbations from GMCs. This places fundamental limits on orbit reconstruction methods that assume long-term action conservation. Despite this, stars born together retain correlated evolution and remain clustered in action space for much longer, allowing disrupted stellar populations to still be identified. I will discuss how these results can be used to distinguish true co-natal groups from resonant structures in Gaia astrometric data. With increasingly precise Galactic surveys (Gaia DR4 in Dec!), these approaches offer new ways to study the dynamical evolution of stars and the Milky Way itself.

   

   
• 10.07.2026 - Noah Jäggi (TU Wien)

  Noah Jäggi

  Space Weathering of Rocky, Airless (Exo-)planets 
  
  Space weathering on airless bodies is governed by processes that eject and modify surface material, populate tenuous exospheres, and alter remote-sensing observables. The products of surface alteration processes we observe around the Moon, Mercury, and asteroids are thereby expected to form the tenuous envelopes of airless exoplanets. This seminar will cover the major space weathering processes, how their efficiency in altering surfaces varies based on environmental parameters, and what the state of research is when addressing uncertainties. A special focus is given to ion-surface interactions, how the state-of-the-art research affects the quantity and composition of the ejected species, and how this may or may not be relevant when altering an exoplanet over geological timescales. 
  
  Noah Jäggi is an experimental space physicist with an MSc in geochemistry and petrology. He wrote his thesis on solar wind ion space weathering at the University of Bern and spent the last two years at the University of Virginia on the peculiarities of weathering radiation-resistant sulfide minerals thought to be found on Mercury. Until 2029, he focuses on researching the underlying physics of solar wind-relevant, highly charged ions interacting with minerals at the Institute for Applied Physics at the TU Wien, funded by an ÖAW APART-USA fellowship.
• 26.06.2026 - Paul Beck (Instituto de Astrofísica de Canarias) & Diego Salvador (Macquarie University)

  Tales of stellar and binary co-evolution (and stellar cannibalism) 

  Paul Beck (Instituto de Astrofísica de Canarias)
  
  Asteroseismology of solar-like oscillators has undergone a remarkable transformation over the past decade, propelled by high-precision photometric data from Kepler, K2, and TESS, alongside significant advances in stellar modeling. These developments have enabled detailed investigations of stellar interiors across a broad range of evolutionary stages – from the main sequence, through the subgiant phase, to the red giant branch. 

  In this talk, we explore how stellar oscillations, combined with binary dynamics, allow us to trace changes in orbital period, eccentricity, and stellar activity driven by evolution and tidal interactions. We show how asteroseismology reveals the impact of star-star interactions on activity and mass loss and the presence of stellar cannibalism in the giant phase. However, the lack of solar-like oscillators in eclipsing binaries limits our ability to calibrate models. We highlight how data from ESA's Gaia and the upcoming PLATO mission will address this gap, offering benchmark systems to improve seismic scaling relations and stellar evolution models.

   

  Linking the low- and high-mass ends of the initial mass function in star-forming galaxies

  Diego Salvador (Macquarie University)
  
  The physical properties of galaxies and their evolution are fundamentally shaped by the type and number of stars they form throughout their history. The initial mass function (IMF) is therefore a key assumption linking the observed light of galaxies to their intrinsic properties (e.g. stellar mass), in galaxy evolution models for inferring their star formation and chemical enrichment histories, and in the construction of stellar population models. Yet, direct empirical constraints on the full IMF shape remain rare beyond the Milky Way: the low-mass regime is well constrained only in quiescent galaxies, while the high-mass end has been studied exclusively in star-forming systems. In this talk, I will present the first main science results from the Hector Galaxy Survey, providing the first simultaneous constraints on both the low- and high-mass ends of the IMF for 214 star-forming galaxies at z~0.01–0.07. By combining low-mass end IMF-sensitive absorption features with high-mass end IMF nebular diagnostics we find substantial diversity in IMF shapes across our sample. Both the low- and high-mass IMF slopes correlate strongly with galaxy properties, where galaxies with higher stellar mass, metallicity, and star formation activity tend to be more bottom- and top-heavy. These results provide direct evidence for IMF variability and demonstrate our current ability to empirically constrain the full IMF.

   
• 19.06.2026 - FÖP Public Presentations

  • Lilly Kormann: Physical Characterization of Superclouds in the Local Milky Way
  • Nora Wagner: Young Stars within 100 pc from Earth

   

  Find all FÖP public presentations.
• 12.06.2026 - Institute Assembly
• 05.06.2026 - Stefanie Reiter (University of Vienna) & Meet Vyas (University of Vienna)

  Linking merger debris to past satellite orbits - What can we learn from simulations?

  Stefanie Reiter (University of Vienna)

  Stellar dynamics provide a fossil record of galaxy formation, containing information on a galaxy’s internal evolution and its accretion history. Applying orbit-based dynamical modelling on spectroscopic data of extragalactic systems enables us to disentangle their stellar orbit distributions, separating dynamically cold (rotation dominated), warm, hot (random motion dominated), and counter-rotating orbits. Investigating the link between a galaxy’s current stellar orbit distribution and its formation history requires knowledge of the galaxy’s past, necessitating the use of cosmological simulations.
  Using the simulation suite TNG50, Zhu et al., 2022, found that from measuring outer regions of the hot stellar component (with orbit-based modelling) we can infer the stellar mass of the most massive satellite in a galaxy’s merger history. I am exploring this link between present stellar dynamics and past satellite properties further by investigating whether we can also infer details of the satellite dynamics. In this talk, I will present my work on constructing orbit distributions from simulations similar to those extracted from observations by dynamical modelling and discuss my findings on tentative correlations in orbit circularities and radius between the satellite and the stellar debris originating from the merger event.

   

  From Simulations to Surveys: Characterizing Galaxy Morphologies using Domain Adaptation

  Meet Jigish Vyas (University of Vienna)

  With the upcoming next-generation time-domain survey facilities such as the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) and the Nancy Grace Roman Space Telescope, the volume of astronomical imaging data is expected to increase dramatically. This creates an inevitable need for fast, automated, and scalable methods for classifying galaxy properties directly from photometric imaging catalogues. 
  In this talk, I will present our work, where we developed a machine learning framework trained on cosmological magneto-hydrodynamical simulations from IllustrisTNG. These simulations provide controlled datasets free from observational systematics such as point spread function (PSF) effects, instrumental noise, background contamination, selection biases, and label priors. Using galaxies from the TNG50 SKIRT synthetic image dataset, we perform domain adaptation to bridge the gap between simulated and observational galaxy images and evaluate the model on real observational data from the SDSS Galaxy Zoo 2 dataset for three morphological classes: spiral, elliptical, and irregular galaxies. This work therefore paves the way for using models trained on simulated datasets for the automated classification of galaxy properties in the upcoming astronomical surveys. 
  I will also briefly discuss my broader work in cosmology, time-domain astronomy, and statistical inference using Machine Learning in the era of large-scale astronomical survey facilities.
• 29.05.2026 - Alvaro Hacar & Glenn van de Ven (University of Vienna)

  Explore the VISESS Doctoral School

  Alvaro Hacar & Glenn van de Ven (University of Vienna)

  Established in 2020, the Vienna International School of Earth and Space Sciences (VISESS) is the Doctoral School at FGGA (https://visess.univie.ac.at/about-visess/).  Different VISESS activities within its three branches - Cosmos, Earth, and Antroposphere - offer an open forum for students and supervisors to explore the scientific work within and beyond their specific field, provide training in transferable skills and career perspectives, and foster networking across our Faculty. VISESS supports our PhD students and provides the structural umbrella for the execution of their PhD projects.

  In this special Institute Seminar we will present an overview of the Cosmos branch at VISESS and discuss some key aspects of the PhD process. In particular:

  • 7-steps for a successful PhD
  • Rights and duties of PhDs & Supervisors
  • Who can supervise PhD students?
  • Teaching obligations for PhDs
  • Evaluation and grading of PhD thesis
  • Open discussion about VISESS related topics

  IMPORTANT: besides PhD students, especially (current/future) supervisors are encouraged to participate!

   

   
• 22.05.2026 - Shivam Joshi (University of Vienna) & Michelangelo Pantaleoni Gonzalez (University of Vienna)

  Can gas influence the ALMA observations of narrow debris discs?
  

  Shivam Joshi (University of Vienna)

  Debris discs are traditionally treated as gas-poor, optically thin dust rings -- similar to our Solar systems. Yet the growing number of gas detections is forcing us to rethink how dust – gas interactions shape the structure of planetesimal belts. HD 131488 is an especially interesting case as it is a remarkably narrow, bright ring with a substantial amount of CO gas comparable to that of old protoplanetary discs. We model HD131488 in both thermal emission and scattered light in a self-consistent approach to reproducing the disc as seen by ALMA and VLT. Our modelling shows that the large particles seen at ALMA wavelengths and often assumed to trace the planetesimal belt might be off-set from the actual parent belt. A sufficiently dense gas component could both (i) broaden the distribution of small grains seen in scattered light and (ii) trap and pull larger grains inwards towards the pressure maximum, naturally producing the narrow ring as seen with ALMA. Our model explains the morphology of HD 131488 and highlights how strong dust–gas coupling may operate in gas-rich debris discs.

   

  Requiem for a Belt 

  Michelangelo Pantaleoni Gonzalez (University of Vienna)
  

  For 170 years, Gould's Belt was described as a nearby, tilted, expanding, ~1 kpc ring of young stars surrounding the Sun, perhaps created by an intergalactic cloud collision with the Milky Way's disc or an even more exotic event involving a dark matter clump. For decades, the study of the purported structure shaped our understanding of local star formation. But modern three-dimensional dust maps and precise astrometry obtained during the Gaia mission are revealing a very different picture. Here, I will present what we believe is a compelling alternative; that in fact Gould's Belt does not exist as a meaningful coherent physical structure. For this we will also review several biases and traps that might be involved in creating the illusion of a Belt.
• 15.05.2026 - Ivan Stanković (University of Vienna) & Nils-Martin Robeling (University of Vienna)

  Does chemistry alone significantly shape exoplanet atmospheres?

  Ivan Stanković (University of Vienna)

  The thermal structure, heating/cooling balance, and mass loss of exoplanet atmospheres are governed by a multitude of factors, including the host star's properties, the planet's formation history and size, and the chemical composition of the atmosphere itself. Given the chemical diversity already detected in exoplanet atmospheres, ranging from H₂O and CO₂ to SO₂, CH₄, and potentially CS₂, and knowing that nitrogen- and oxygen-rich atmospheres both exist in our own Solar System, the question of how much chemistry alone matters comes naturally.

  To put this to the test, we constructed a grid of upper atmospheric models for an Earth- and Venus-like planet by systematically varying the molar ratios of H, C, N, O, and S while keeping all other parameters fixed. We modelled each composition to a steady state using The Kompot Code, our first-principles, self-consistent 1D model combining atmospheric photochemistry with thermal structure, stellar irradiation, and vertical transport via eddy and molecular diffusion.

  The answer to the question in the title is a clear yes, but the extent to which chemistry has an impact, and over what range of conditions, is less obvious than one might expect. We find that the relative elemental abundances can drive atmospheric states ranging from stable and cool to hot atmospheres with very high mass loss. This sensitivity to chemistry also shifts with irradiation level, meaning the same composition can have very different implications on different planets.

   

  Self-consistent 1D modelling of gas giant upper atmospheres

  Nils-Martin Robeling (University of Vienna)

  Recent observations by the James Webb Space Telescope have revealed that disequilibrium chemistry plays a central role in shaping observed transmission spectra of exoplanet atmospheres. Hence, robust characterisation of exoplanet atmospheres requires a theoretical understanding of how disequilibrium processes shape the atmospheric thermal and chemical profiles and their observed signatures. This is particularly important for the upcoming ESA Ariel mission, which will observe a diverse population of exoplanets, for which our current understanding of disequilibrium processes at the population level is limited. In this talk, I will present my work on self-consistent modelling of gas giant atmospheres, which involves extending the upper atmospheric model Kompot to gas giants and benchmarking it against Jupiter. Kompot is a one-dimensional, first-principles, self-consistent thermo-chemical model that solves the coupled hydrodynamical, (photo-)chemical, and thermal balance equations without prescribing an input temperature profile, allowing the physical structure to emerge from the underlying processes. It also allows for feedback between the chemistry and the thermal structure. Our results establish the first benchmark of Kompot for Jupiter, demonstrating its ability to reproduce both model predictions and observations. By extending and benchmarking Kompot for gas giants, including full photochemistry, escape processes, and emergent temperature profiles, we provide a modelling framework that directly supports Ariel's population-level analyses and the interpretation of disequilibrium signatures across hundreds of planetary systems.

   
• 08.05.2026 - Juan Diego Soler (University of Vienna) & Katja Fahrion (University of Vienna)

  Something new in the Solar neighborhood: the atomic shell of the extended Orion nebula (EON)

  Juan Diego Soler (University of Vienna)

  The Orion Nebula is the nearest site of ongoing and recent high-mass star formation, a unique laboratory for studying the mass, energy, and momentum input from high-mass stars. We present observations of the 21-centimeter emission line that resolve, for the first time, the neutral atomic hydrogen (HI) gas in the shell of the Extended Orion Nebula (EON) at a resolution of 1 arcminute, corresponding to a physical scale of 0.12 parsecs at the standard distance to the region. These new HI emission maps reveal an expanding shell of the EON and a 4 pc-long protrusion from the cavity wall. The 21-cm-line emission closely matches the shell contours delineated by recent ionized carbon ([CII]) line emission observations, but indicates a lower mass for this expanding structure. From our HI data, we estimate a mass of approximately 100 solar masses for the front of the shell, roughly a factor of 10 lower than the mass derived from the [CII] observations. The HI-derived mass traces the shell's front hemisphere with relatively narrow velocity components, while [CII]-based estimates rely on broader velocity averages, likely incorporating gas that is not part of the same region. This difference in methodology may account for the overall mass discrepancy. Alternatively, the contrasting masses inferred from the two tracers may reflect substantial molecular hydrogen in the EON shell that is not accounted for in HI measurements. Our results demonstrate that high-resolution HI observations can elucidate crucial details of the connection between star-forming regions and their surroundings and expose uncharted dynamics in one of the best-studied stellar feedback laboratories.

   

  High-Resolution spectroscopy of globular clusters for chemistry and distance measurements

  Katja Fahrion (University of Vienna)

  Globular clusters (GCs) are old and dense star clusters observable in the halo regions of all massive galaxies. Traditionally, they have been used as tracers of galaxy formation and assembly, using both imaging and medium-resolution (R < 6000) multi-object spectroscopy to probe the distribution, kinematics, and chemical properties of GC systems. In this talk, I will present how using high resolution (R ~ 18000) spectroscopy of GCs opens new possibilities of using GCs as tracers of galaxy properties. I will show how high-resolution spectra allow to measure stellar population properties such as metallicities and chemical abundances. Additionally, I will discuss how these data allow us to measure the internal velocity dispersion of extragalactic GCs, which can be used to measure distances using the tight relationship between internal GC velocity and V-band magnitude. I will present the first results from our new survey with VLT/FLAMES to measure distances of several galaxies exploiting this relationship
• 24.04.2026 - Victoria Toptun (ESO) & Federica Mauro (University of Vienna)

  From clusters to Milky Way-type groups: Extending X-ray scaling relations with eROSITA 

  Victoria Toptun (ESO)

  Low-mass galaxy groups are the most common environments for galaxies and serve as a key bridge between cosmological structure formation and galaxy evolution. Yet, their hot gas and baryonic content remain poorly
  characterized, largely due to their low surface brightness in X-rays. In this talk, I will show how spectral stacking of eROSITA data offers a powerful way to uncover the X-ray properties of galaxy groups and clusters identified through large spectroscopic surveys such as SDSS and GAMA. Using eRASS1 data, I will present stacked X-ray spectra over a wide range of halo masses, from massive clusters down to group scales  comparable to the Local Group, and compare them with mock observations from Magneticum hydrodynamical simulations. This approach allows us to extend and validate key X-ray scaling relations into the low-mass regime, such as the mass-temperature relation and the stellar-to-halo mass relation for brightest central galaxies. With this approach, we also probe the impact of AGN feedback on baryon content and distribution, offering new constraints on the thermodynamics and internal structure of the intra-group medium. These results open new pathways to connecting observations and theory across the full mass spectrum of cosmic structures even for systems individually undetected in X-rays.

   

  Tracing mass assembly in star-forming galaxies at z ~ 0.3

  Federica Mauro (University of Vienna)

  The epoch at z ~ 0.3 is a key transitional phase in galaxy evolution, occurring after the peak of cosmic star formation but before the present-day, mostly quiescent Universe. At this stage, the balance between early, rapid bulge formation and prolonged disk growth can be directly observed, providing important constraints on the physical processes driving mass assembly and quenching.
  In this talk, I will present my work on the spatially resolved stellar populations of 34 galaxies at 0.28 < z < 0.35 from the MAGPI survey, using MUSE integral-field spectroscopy. I derived radial profiles and mass assembly through spectral synthesis modeling with FADO and Starlight. These profiles are constructed using isophotal annuli, preserving galaxy morphology and enabling a clean separation between inner and outer components. I further reconstruct star formation histories and cumulative mass assembly curves for these regions.
  Star formation histories show that galaxy cores formed the majority of their stellar mass rapidly, within the first 2–3 Gyr of cosmic time, while regions beyond one effective radius assembled more gradually and sustained star formation to later epochs.
  These results support a scenario in which early dissipative processes and mergers dominate the formation of galaxy bulges. In contrast, galaxy outskirts evolve through extended, secular star formation, establishing the inside-out growth and centrally concentrated quenching that link high-redshift systems to the quiescent galaxies in the local universe.
• 17.04.2026 - Oliver Hahn & Sylvia Ploeckinger (University of Vienna)

  Dark UNiverse Explorations (DUNE): overview of the new special research area and the Vienna projects

  Oliver Hahn & Sylvia Ploeckinger (University of Vienna)

  We will introduce the FWF special research area (“Spezialforschungsbereich”, SFB) Dark UNiverse Exploration (DUNE). DUNE includes seven subprojects (SP) led by researchers from the Universities of Innsbruck and Vienna, and from the Institute for Science and Technology Austria (ISTA). The aim of DUNE is to address key open question in cosmology and cosmological galaxy formation by combining data from the space telescopes Euclid and JWST with different types of cutting-edge cosmological simulations.
  
  Oliver Hahn leads SP3 “Ray-tracing through fast differentiable simulations”. Leveraging the full potential of surveys like Euclid requires innovative statistical and simulation techniques. This SP will extend the DISCO-DJ framework to include weak gravitational lensing and improved small-scale matter modelling. These upgrades will ready the pipeline for a multi-probe field-level analysis of Euclid and other large-scale structure data, enabling deeper insight into cosmic evolution and fundamental physics.
  
  Sylvia Ploeckinger leads SP6 “Testing galaxy formation and cosmology on small scales”. This subproject aims to establish a comprehensive framework linking the detailed properties of galaxies to the dark components of the Universe that determine the characteristics of the initial density fluctuations. The initial focus is on understanding the connection between early Universe linear density perturbations, dominated by dark matter, and the resulting observable galaxy properties at low redshift. By employing both traditional and machine learning‑based statistical methods, SP6 seeks to classify galaxy properties based on their predictability from the primordial environment. The goal of this subproject is to quantify the likelihood for each tested DM model to represent the observed EUCLID galaxies, independent from the applied galaxy formation model in the simulations.

   

   
• 20.03.2026 - Guimei Liu (University of Vienna) & Horst Foidl (University of Vienna)

  Tracing Hierarchical Star Formation with Galactic Open Clusters

  Guimei Liu (University of Vienna)

  Open clusters (OCs) are key tracers of the structure and dynamical evolution of the Galactic disc. Their spatial distribution provides important insight into the hierarchical nature of star formation and the assembly of stellar systems at early evolutionary stages.
  In this talk, I will present a systematic study of the spatial and kinematic clustering of OCs in the solar neighbourhood using high-quality Gaia-based cluster catalogues. I will describe the methodology used to quantify their clustering properties and discuss the implications for the hierarchical formation of stellar structures and the dynamical evolution of stellar complexes in the Galactic disc, and place these results in the broader context of comparisons with extragalactic star cluster systems.

   

  The DESI project is about to discover new physics

  Horst Foidl (University of Vienna)

  This talk concludes our series of papers, all of them based on the results of my PhD thesis, addressing possible explanations for dark energy and the Hubble tension. In this series of papers, we empirically found a degeneracy in the customary computation of the expansion history of cosmological models, which replace Λ with a dynamical model of dark energy (DDE), such that cosmological models with a phantom energy type dark energy component perfectly reproduce ΛCDM results. Here, we explain in detail the conditions that must be met for this degeneracy to occur. It is important to understand this degeneracy as a property of the customary computation method for the expansion history, as it can bias the Markov chain Monte Carlo (MCMC) analysis of cosmological measurement data, since the computation of individual models is the elementary building block of such a data analysis. We provide an explanation for the very similar results obtained by the major cosmological observation campaigns for DDE-based models, all of them having an increasing EoS parameter (even a phantom energy type DDE). Furthermore, we show that the presumed evidences for new physics needed in the explanation of dark energy, reported by the DESI project, are due to the bias of the MCMC analysis and an overly simplified picture of the transition from the matter-dominated to the dark energy-dominated universe.

   

   
• 13.03.2026 - Adrián Gutiérrez Adame (University of Vienna) & Simone Spedicato (University of Vienna)

  Cosmological simulations with local primordial non-Gaussianities

  Adrian Gutierrez Adame (University of Vienna)

  Measuring primordial non-Gaussianities (PNGs) in large-scale structure (LSS) of the Universe is a key goal in observational cosmology, as even a small detection could provide evidence for new physics in the early Universe. Achieving this requires validating analysis tools using high-fidelity cosmological simulations, which play a central role in covariance estimation, survey design, and theoretical modelling of clustering, lensing, and redshift-space distortions.
  In this talk, I will present a comprehensive simulation pipeline we have developed to generate realistic galaxy mock catalogues from full N-body simulations, including local-type PNGs and observational selection effects. I will discuss our validation methods and publicly available tools, as well as the practical guidelines we establish for generating accurate and computationally efficient simulations in the presence of PNG. These results provide a robust framework for current and upcoming galaxy surveys aiming to probe the regime of σ(fNL) < 1.

   

  Meet Your Data Steward: Research Data Management Essentials at FGGA

  Simone Spedicato (University of Vienna)

  In this 30‑minute primer, I’ll introduce the services I offer as the new Data Steward for the Faculty of Earth Sciences, Geography and Astronomy (FGGA) and highlight good practice in Research Data Management (RDM) across the data life cycle. Topics include drafting practical Data Management Plans for funders (e.g., FWF, FFG, Horizon Europe), organizing data and metadata, selecting storage and backup options, ensuring data security and compliance, and sharing or publishing with appropriate licenses and persistent identifiers (e.g., DOIs, ORCID). We will also address reproducibility considerations and the use of trusted repositories and collaboration platforms (e.g., PHAIDRA, GitLab). This is a general‑audience session open to everyone. Participants will gain a clearer overview of institutional and funders expectations, relevant policies, and the support available at FGGA through the Data Steward, with time reserved for questions.