5th Annual Niels Bohr Institute MSc. Student Symposium

Friday 27 Mar 2026, 12:30 → 19:00 Europe/Copenhagen

Margrethe Bohr Salen (001-0-EF.000) (Niels Bohr Bygningen 1)

August Kiersgaard, Ellen Maria Skafte Schriver, Jens Milan Nielsen, Jørgen Beck Hansen (NBI), Stine Stenfatt West, Storm Gjerpe (student), Thomas Heimburg (Niels Bohr Institute, Head of studies MSc)

"For the students by the students"

Welcome to the 5^th annual student symposium in Physics at the Niels Bohr Institute. This is an initiative to celebrate and show all the great work done by all of the master students at NBI across the many fields. 

Important dates 

ABSTRACT SUBMISSION  DEADLINE: Monday the 16^th of March.

REGISTRATION DEADLINE: Tuesday the 24^th of March @ 23:59.

12:30 → 13:00 Get your posters ready: Poster setup

13:00 → 14:20 Presentations

13:05 Dominant large-scale drivers of winter precipitation variability in Europe and the North Atlantic

This study investigates the main large-scale drivers of precipitation variability. Using monthly reanalysis data spanning 46 years (1979–2025), it examines the causal pathways driving precipitation over Europe and the North Atlantic during the winter season. To this end, causal inference methods are applied, with the aim of revealing temporal and spatial structures that differ from those identified through correlation-based approaches. The causality algorithm, based on conditional independence, is implemented using both first- and higher-order techniques to assess nonlinearities in the teleconnections between atmospheric variables. The North Atlantic Oscillation (NAO), a statistical artifact summarizing the leading mode of sea level pressure variability in the North Atlantic, accounts for a significant share of precipitation variability, so it is used as a benchmark. The overarching goal is to reduce uncertainty in precipitation prediction by relying solely on physical variables, both by increasing the explained variance in regions where the NAO already shows skill, and by providing additional insight in regions where it does not. Preliminary results show a modest improvement in prediction skill over the NAO baseline, while offering a clearer physical interpretation of the mechanisms involved. The linear vs. nonlinear analysis suggests that teleconnections in this region are predominantly linear, with higher-order nonlinearities either absent or below the detection threshold of the method.

13:20 Self-Assembly of Intermediate Filaments via Phase Separation: A Cahn-Hilliard-based Model of Active Matter

The physical properties of a cell, such as stiffness and elasticity, are primarily governed by its cytoskeleton which is mainly made of three filament types. One these is intermediate filaments, which have recently gained interest because of their remarkable mechanical properties, exceptional stiffness at large deformations and elasticity on the other hand. They form a dynamic network that can break and reassemble. While historically their assembly was attributed to polymerization kinetics as is the case for actin and microtubules, recent evidence suggests liquid-liquid phase separation plays a central role.
This project investigates how phase separation dynamics give rise to network-like structures through numerical simulations of a 2D Cahn-Hilliard based active phase field model. The proposed model creates elongated structures from droplets that are reminiscent of those in passive Cahn-Hilliard dynamics. Over time these structures connect to a network of fixed filament width with breaking and reconnecting mechanisms.
This minimal yet physically grounded model suggests that phase separation with activity is sufficient to recapitulate key morphological features of intermediate filament self-assembly.

13:35 Assessing the issue of the water isotope signal loss in the Beyond EPICA Oldest Ice Core

A new deep ice-core record from the East Antarctic Plateau reaching at least 1.2 million years is now available through the Beyond EPICA Oldest Ice Core project (BEOIC). This record spans the Mid-Pleistocene Transition (MPT), when glacial-cycle pacing shifted from ~40,000 years to ~100,000 years, and therefore offers key constraints when combined water-isotope and greenhouse-gas measurements are interpreted together.

Recovering an accurate water-isotope signal from the deepest and oldest ice is challenging because diffusion in solid ice attenuates high-frequency variability. High-precision, high-resolution measurements combined with physically based estimates of isotope diffusion can be used to quantify signal attenuation and assess the feasibility of signal deconvolution.

This thesis presents a combined modelling and data study that quantifies diffusion-driven attenuation of the water isotope signal along the BEOIC using updated age–depth information and borehole temperature constraints. The resulting transfer functions are applied to high-resolution isotope sections from multiple depths to evaluate the recoverable bandwidth and to test spectral/Wiener restoration approaches, including the impact of measurement noise and sampling resolution on the reconstruction.

13:50 Tracing the dust and ISM properties of distant quiescent galaxies with JWST and ALMA

In studying the evolution of galaxies, we observe a clear bimodality in both their morphology and colour space, discerning two distinct populations: blue, star-forming galaxies with a younger, UV-bright stellar population, and red, early-type galaxies, whose star formation has halted---so-called quiescent galaxies. Understanding the halting of star formation (termed quenching) is therefore vital for building an overall picture of galaxy evolution.

Furthermore, recent observations using the James Webb Space Telescope have extended the discovery frontier of quenched, "red-and-dead" galaxies to much earlier in cosmic time than expected, back to when the Universe was less than 700 million years old. This breakthrough offers a timely opportunity to investigate what governs quenching at high redshift, and how it differs from quenching in the present-day universe.

This work focus on examining the dust and gas properties of high-redshift quenched galaxies, with the goal of understanding the impact of associated feedback mechanisms---such as those from active galactic nuclei (AGN)---on the interstellar medium. We utilise ALMA continuum data to examine dust retention in quiescent systems, and JWST/NIRSpec spectroscopy to characterise AGN activity through emission line diagnostics. By studying this quiescent population, we aim to shed light on the mechanisms that drive quenching in the early universe, and contribute to our understanding of how galaxies are born, live, and eventually die.

14:05 Mitochondrial membrane shape remodelling by ETC complex CIII of the inner mitochondrial membrane: A coarse-grained molecular dynamic studies.

Mitochondria serve as the epicentre of energy production of the eukaryotic cell, generating most of the adenosine triphosphate (ATP) required for cellular processes. This energy conversion is carried out by the respiratory chain complexes, including the electron transport chain (ETC) and F_0 F_1-ATP synthase, which are located within specialized invagination of the inner mitochondrial membrane (IMM), called cristae. The architecture of the cristae is dynamically regulated and closely associated with metabolic efficiency, cellular homeostasis and pathology. Understanding the molecular mechanisms that govern and modulate cristae morphology is therefore essential.

The roles of the Mitochondrial Contact Site and Cristae Organizing System (MICOS) and F_0 F_1-ATP synthase in shaping cristae architecture are well accepted, whereas the ETC complexes are most commonly regarded as stabilizing structures of the laminar regions of the cristae. However, recent studies suggest that certain ETC complexes may also induce local membrane curvature through the formation of super-complexes, a phenomenon that has not yet been well characterized. This project provides a new framework for understanding how the respiratory machinery shapes its own functional landscape and contributes to mitochondrial membrane remodelling. By employing coarse-grained molecular dynamic simulations using the Martini 3 force field to quantify membrane curvature induced by ETC complex 〖CIII〗_2 in a biomimetic lipid membrane, this project reveals a critical piece of the larger puzzle regarding mitochondrial morphogenesis.

14:20 → 14:45 Coffee break

14:45 → 16:05 Presentations

14:45 Entropy conservation in chemical oscillations and mecahnical springs

In physics, oscillations, e.g. of springs, are adiabatic processes. They conserve both energy and entropy. This can be monitored by observing the oscillating temperature. Oscillations also exist in chemistry. Such oscillations are described in the literature by reaction-diffusion networks of coupled rate equations that only contain chemical concentrations as variables. Therefore, these oscillations are treated differently to the oscillations of springs. Temperature and other variables are not considered, which also makes it impossible to judge whether such reactions contain entropy-conserving elements. However, there are indications that chemical oscillatio ns also display periodic variations in temperature. In this thesis, temperature and concentration variations in a few chemical oscillations, such as the Belousov–Zhabotinsky reaction and the Briggs–Rauscher reaction, will be studied. They will be compared to physical oscillators, such as springs and capacitors. The thesis has experimental and theoretical elements.

15:00 Unnaturalness of Starobinsky inflation within Asymptotic Safety

In the context of phenomenological modified gravity, Starobinsky inflation is considered one of the most successful inflationary models. However, from a fundamental physics perspective, it faces a significant naturalness challenge. Compatibility with cosmological observations requires a remarkably strong hierarchy: the $R^2$ term must be extremely large, while higher-order corrections must be strictly suppressed.
In my Master’s thesis, I investigate whether such a hierarchy can emerge dynamically from the renormalization group flow within a UV-complete theory of gravity. This question is addressed within the framework of Asymptotic Safety. Since operators beyond quadratic order correspond to irrelevant directions, their coefficients are fundamentally determined by the ultraviolet dynamics.
The results indicate that these higher-order contributions are generically not suppressed along ultraviolet-complete trajectories, barring extreme fine-tuning or pushing the scale of quantum gravity to trans-Planckian values. This reveals a structural tension between quantum consistency and observational viability. Consequently, as a purely gravitational phenomenon, Starobinsky inflation appears structurally unnatural.

15:15 Discovering the highest-energy neutrinos in GRAND

Where do ultra-high-energy cosmic rays—the most energetic particles known in the Universe—come from? For decades, the question has remained unanswered. Ultra-high-energy neutrinos, born from cosmic-ray interaction and with energies more than 10,000 times higher than particles made in human-made accelerators—are key to solving this mystery. Yet, so far, we have detected but a single ultra-high-energy neutrino—and unexpectedly at that! The Giant Radio Array for Neutrino Detection (GRAND) aims to solve this. GRAND is a proposed next-generation observatory optimized to observe ultra-high-energy neutrinos. It does so by detecting the radio signals that the neutrinos emit when they collide with the Earth’s atmosphere. In this work, we forecast the neutrino discovery potential of GRAND for a range of predicted neutrino flux models, from optimistic to pessimistic, anchored on simulations of the detector response. Using Bayesian inference, we report the prospects of discovering the different flux models and of distinguishing between them, crucial steps to finding the origin of ultra-high-energy cosmic rays. We find that GRAND, once completed, will be able to detect medium-to-high predicted neutrino fluxes within only a few years’ worth of operation. Our results establish a promising baseline for what the coming decade of ultra-high-energy observations will look like.

15:30 About local signatures of Unconventional magnetism

Traditionally, antiferromagnetism is a type of commensurate magnetic ordering, exhibiting Kramer's degenerate bands. Recently, it was discovered that symmetry could enforce a spin splitting of the bands. Such magnetic orders can be categorised into altermagnets with even parity spin splitting and odd-parity magnets, sometimes called antialtermagnets. In my thesis, I calculate the local spin-resolved density of states around an impurity, as well as its quasi-particle interference. This is an experimental signature that exhibits the same symmetries as the magnetic order, which is measured using spin-resolved scanning tunnelling microscopy.

15:45 How to play a black hole

Black hole spectroscopy is a vibrant field of research with significant potential to uncover new physics. Despite its importance and development over the last years, very little is known about how the different characteristic modes of black holes, called quasinormal modes, are excited, and how this relates to the physics of light rings. In this project we study the excitation of the quasinormal modes as function of the initial data, trying to find how this excitation depends on the different parameters of the initial conditions.

16:05 → 18:00 Poster session: Enjoy the posters!

16:05 Aspects of Defect ABJM Theory

Calculation of one-point functions in defect ABJM Theory.
To this end I investigate modified fuzzy spherical harmonics (i.e. rectangluar matrix valued fuzzy spherical harmonics) which simultaneously form a basis for rectangular matrices. I derive and calculate their normalisations. Along with this I derive the AdS propagator in 2+1 dimensions as this is needed to facilitate the calculation of the one-point function. My current work is extending my calculations to more general chiral primary operators.

16:05 AstroComb: dating sediment through spectral peaks

By assuming that the astronomical cycles is detectable in the spectral signal of a stratigraphic sediment-core, the depth can be transformed into time. Using bayesian inversion and 'combing' through possible sedimentation rates, this timeline can be calculated along with uncertainties. AstroComb is aimed at geologists and feature many adjustable parameters, with an ultimate goal of searching for the milankovitch cycles themselves.

16:05 DMS in Planetary Atmospheres: Atmospheric Chemistry and Biosignature Implications

In the search for life in the universe one of the most important tools are biosignatures. Biosignatures are molecules produced by biological processes. Such molecules are detectable in exoplanet atmospheres. On Earth, an example of biosignatures we would see in our atmosphere would be oxygen $(O_2)$, Methane $(CH_4)$ and lastly Dimethyl sulfide (DMS). DMS is a sulfur-containing gas produced by marine biology which is destroyed by multiple factors. Predominantly with reactions of hydroxyl radical $(OH)$ and photochemistry.

DMS is particularly interesting because both observational and theoretical studies have hinted of the possibility of presence of DMS in the atmosphere of the exoplanet K2-18 b. Additionally, on Earth, DMS is one of the biosignatures which has a creation pathway that is dominated by biological processes. Understanding the atmospheric behavior of DMS is therefore important for assessing its detectability as a potential biosignature in exoplanet observations.

Motivated by these findings we developed an atmospheric model to investigate the role of DMS. The atmospheric model combines a 1D self-consistent radiative transfer code (MARCS) with a photochemical solver (KROME) to simulate the chemical and radiative effects of DMS in planetary atmospheres. To validate our findings we will use it by mimicking Earths condition and then the conditions of K2-18 b. To further improve the atmospheric model we want to implement a simple modelling of clouds.

16:05 Does the AGN broad emission line gas see the ionizing continuum we see?

The ionizing spectral energy distribution (SED) of active galactic nuclei (AGN) is a fundamental, yet poorly constrained quantity that governs the photoionization of the Broad Line Region (BLR). X-ray observations of the changing-look AGN Mrk 590 by Lawther et al. (2025) have revealed a Comptonizing inner accretion flow, providing a new constraint on the SED. This thesis uses the Cloudy photoionization code to test whether this newly determined SED can reproduce the observed broad emission line intensities in Mrk 590.

UV and optical spectra from instruments are fitted using a custom spectral decomposition pipeline to measure emission line intensities. These measurements are compared against Cloudy photoionization model grids computed for a range of physical conditions, including varying hydrogen column densities, hydrogen ionization parameters, and gas densities. The grids are generated using version 25 of Cloudy and use the ionizing SED composed from Lawther et al. (2025) as input.

A key goal is to assess whether the X-ray-derived SED produces line intensities consistent with the observations, or whether additional constraints on the SED shape are needed. Furthermore, the photoionization modelling is applied to investigate whether Mrk 590's incident SED is consistent with that expected from a standard accretion disk, or whether this changing-look AGN possesses unusual physical properties. Current research suggests the latter, pointing toward an SED that deviates from standard disk models. This study contributes to a broader understanding of the connection between AGN ionization physics and BLR emission properties.

16:05 Electrical control of Quantum Dot emission embedded in Whispering Gallery Mode resonators

Quantum Dots (QDs) are nanoscale semiconductor structures that can emit single photons, making them attractive building blocks for quantum applications. When embedded in photonic disk resonators, their emission can be greatly enhanced through the Purcell effect. However, for QDs to be practically useful, their emission must be stable and tunable. These are two challenges this project aims to address.
By fabricating disk resonators with a p-i-n junction, where the QDs sit in the intrinsic middle layer, we can apply a voltage across the structure. This serves both the purpose of stabilizing the emission by suppressing charge noise in the QD surroundings, as well as tuning the emission wavelength using the quantum confined DC Stark effect. The electric field shifts the energy levels of the QD, making it tunable.
Part of this project was to design nanostructures that gate the QDs inside the disk resonator, fabricate them in the cleanroom and finally characterize them in the optical lab. This work moves toward a fully controllable QD embedded system - a promising component for future quantum technologies.

16:05 Finite-temperature scaling of voltage-tuned quantum phase transitions in a hybrid Josephson-junction array

We report transport measurements of a two-dimensional semiconductor-superconductor hybrid Josephson-junction array with a double-layer electrostatic gate, enabling independent in situ voltage-tuned inter-island coupling and proximity-induced superconductivity. We use this voltage to drive and study superconductor-insulator (SIT) and superconductor-metal (SMT) transitions within the same device. For each transition, we identify the critical resistivity from isotherm crossings and extract critical exponents via finite-temperature scaling. We find that the critical resistivity approaches h/4e^2 near the triple point, where the superconducting, metallic and insulating states meet in the gate-voltage space. Away from this point, enhancing the proximity-induced coupling increases the SIT critical resistivity while the scaling exponent remains roughly constant. In contrast, increasing the inter-island coupling systematically decreases both the SMT critical resistivity and the associated exponent. This decrease roughly coincides with a voltage-tuned crossover of the metallic state from weak localization to weak antilocalization. Based on this we discuss whether the critical behavior is sensitive to the magnitude and sign of quantum-interference corrections in the metallic regime.

16:05 Investigating the Dark Matter Distribution in Dwarf Galaxies using Extragalactic Stellar Streams

The current best cosmological model, the $\Lambda$ Cold Dark Matter model, successfully explains the large scale structures of the universe. However, this model fails to explain some small scale observations. One key example of this discrepancy between theory and observations is the core-cusp problem. Theoretically, we expect steep inner density profiles for dark matter halos, while observations often find flat inner density profiles.

In this project, we use extragalactic stellar streams to constrain the inner and outer slope of the radial density profile as well as other dark matter halo properties. Stellar streams form when the stars in a smaller galaxy tidally strips, due to a stronger gravitational pull from a larger galaxy. This leads to structures of stars orbiting the larger host galaxy. The new extragalactic stream fitting code, X-Stream, enables the exploration of a huge parameter space regarding stream morphology and dark matter features using 2D images of extragalactic streams. We focus our studies on fitting a model to the stream and shells around the dwarf galaxy NGC 300. Dwarf galaxies contain a large fraction of dark matter compared to larger galaxies, making them excellent systems to investigate the dark matter density profile. We model NGC 300's stream and shells as one structure and use it to constrain the progenitor orbit and halo properties of NGC 300. Additionally, we implement the ability to evaluate multiple radial velocity measurements to the code, X-Stream, instead of only using the on sky 2D spatial stream morphology. We first test the method with simulated streams to check the validity, and subsequently use the method on the dwarf galaxy NGC 4449, which has multiple radial velocity measurements along its stream. This opens up for future, tighter stream model constraints of systems in which radial velocities exist.

16:05 Modeling the Great Oxidation Event (GOE) with a Kinetic Equilibrium Model– Can we observe an oxidation event on exoplanets with synthetic transit radii?

The Great Oxidation Event (GOE) occurred 2.54 billion years ago and transformed the composition of the Early Archean Earth’s atmosphere from being less than 1ppm of O2 to approximately 2% (Catling, et al. 2017). We model the processes behind the GOE by incorporating the complete photochemical network detailed in Liu et al. 2019 with additional reactions describing the process of carbon burial made possible from oxygenic photosynthesis. The main goal of this research is to see how similar processes on exoplanets might be observable through transit spectroscopy. With this work I model with a kinetic equilibrium code, and create synthetic transit depth spectra at different points in the evolution using the petitRadtrans python package. Then, harnessing the tools in petitRadtrans, synthetic transit radii can be created from the model data and compared to current observation. By taking the outputs of the model at different time steps, there is a visible difference in the transit radii produced. Our preliminary results suggested that the most observable difference in the atmospheric composition is the decline in CO2 and CH4 caused by burial of carbon as organic material and consequently the creation of OH. We then expanded our research by increasing the chemical network to include more of the processes affecting the atmospheric O2, in particular the ability to detect O2 via the proxy of O3. Improving our understanding of O2 in the atmosphere might be a crucial next step in the search for complex life outside of Earth, both due to the role of O2 as a biosignature, and because complex life might be more dependent on high energy available in aerobic metabolism (Catling, et al. 2005).

16:05 Neutrino flavor measurements at the highest energies with TAMBO

Ultra-high-energy cosmic neutrinos have energies millions of times greater than any particle produced
on Earth. Traveling across the breadth of the observable Universe, they bring us unaltered information
from the most extreme astrophysical environments. However, because these particles are scarce and
interact with matter so rarely, detecting them requires specialized techniques. TAMBO (the Tau Air-
Shower Mountain-Based Observatory) is a proposed neutrino telescope, currently in pilot phase,
designed to probe a largely unexplored energy range (10^15 to 10^17 eV). While primarily optimized to
detect tau neutrinos, TAMBO also possesses a unique sensitivity to electron anti-neutrinos within a
specific, narrow energy window. Measuring the relative abundance of these different neutrino types---
their "flavor composition"---provides a powerful test for both extreme astrophysical models and
fundamental physics. In this study, we use advanced detector simulations to evaluate the capacity of
TAMBO to identify these electron anti-neutrinos. We report, for the first time, how precisely TAMBO
could measure neutrino flavor composition at these unprecedented energies, benchmarking its
upcoming science reach.

16:05 Non-relativistic string theory and the holographic principle

In my thesis, I investigate how a non-relativistic limit (c to infinity) can be applied to the framework of string theory. I focus in on the holographic principle, which relates gravity and quantum field theory. The goal of my thesis is to see how the holographic principle carries over to non-relativistic string theory.

16:05 Physics-based AI-driven Molecular Reconstruction of Organelle Membranes

Biological membranes, especially organelle membranes, are highly complex structures composed of diverse proteins and lipid types that are often distributed unevenly across the membrane surface. Understanding how these molecules are arranged laterally is essential for revealing how organelles interact with their environment. Although extensive experimental data exist on global membrane composition, obtaining detailed information about the lateral organization of membrane components remains challenging. Molecular dynamics (MD) simulations offer one possible route to study this organization. However, due to their high computational cost, conventional MD techniques struggle to achieve the precision and scale needed to model entire organelle membranes. Therefore, this project aims to produce a "computational microscope" that integrates machine learning (ML) to predict the lipids organization in the membrane. By training ML models on data from simulations of smaller membrane patches consisting of the structural properties of the membrane, we aim to establish rules that allow these local predictions to be combined into a coherent model of the full membrane. Such an approach could significantly enhance the efficiency of MD simulations of cell scale system by generating improved initial configurations for membrane molecules, ultimately accelerating studies of membrane structure and function.

16:05 The chemical structure and evolution of protoplanetary disks

This thesis studies the temporal and spacial evolution of both gaseous and solid materials in protoplanetary disks. A model for evolving gas and dust as well as water in forms of both ice and vapor is set up. The icy dust grains experience hydrodynamic transport, collisional growth as well as sublimation/condensation of water when the disk temperature allows it. The gas is likewise transported hydrodynamically. The intended results of the project, aims to showcase the distribution of water along both disk radii and dust grain sizes through several test cases evolving the disk for Myrs.

16:05 Toward a kinetic model for the mechanical activation of the adhesion GPCR ADGRL3 in single cells

Adhesion G protein-coupled receptors (GPCRs) are proposed to play pivotal adhesive roles in neurons. We investigate mechanotransduction as a possible operating principle for adhesion GPCRs using an optical tweezer-based strategy at two different scales. At the cellular level, we use an optically trapped bead to apply forces directly to many ADGRL3 receptors (a prototypical adhesion GPCR) on the membrane of living HEK cells, while applying forces and deformation velocities comparable to physiological traction and migration velocities, in parallel with confocal imaging of fluorescent mini G proteins (mG12) reporting on receptor signaling activation. At the single-molecule (SM) level on supported lipid bilayers (SLBs), we investigate ADGRL3 interactions with its endogenous transsynaptic ligand FLRT3, both present on opposing fluid SLBs of membrane-coated optically trapped beads. Recent SM studies on functionalized ADGRL3 GAIN domains suggest a force-dependent reversible transition between a compact and an unfolded state, as well as an irreversible transition between an unfolded and a dissociated state. The unfolded and dissociated states are believed to drive receptor signaling activation, yet there is little evidence for this in living cells. Using our SM strategy with SLB-coated beads we examine whether the force per receptor applied in our cell assay would promote the structural transitions reported by others, thereby enabling a link to signaling activity (mG12 recruitment). The data suggest receptor-ligand SM interactions, with a fourfold increase in interaction frequency relative to negative controls, as well as ADGRL3 activation under tensile forces, but not under compression forces. A draft for a force-dependant kinetic model for the mechanical activation of ADGRL3 on live cells is proposed

16:05 Tracing the dust and ISM properties of distant quiescent galaxies with JWST and ALMA

In studying the evolution of galaxies, we observe a clear bimodality in both their morphology and colour space, discerning two distinct populations: blue, star-forming galaxies with a younger, UV-bright stellar population, and red, early-type galaxies, whose star formation has halted---so-called quiescent galaxies. Understanding the halting of star formation (termed quenching) is therefore vital for building an overall picture of galaxy evolution.

Furthermore, recent observations using the James Webb Space Telescope have extended the discovery frontier of quenched, "red-and-dead" galaxies to much earlier in cosmic time than expected, back to when the Universe was less than 700 million years old. This breakthrough offers a timely opportunity to investigate what governs quenching at high redshift, and how it differs from quenching in the present-day universe.

This work focus on examining the dust and gas properties of high-redshift quenched galaxies, with the goal of understanding the impact of associated feedback mechanisms---such as those from active galactic nuclei (AGN)---on the interstellar medium. We utilise ALMA continuum data to examine dust retention in quiescent systems, and JWST/NIRSpec spectroscopy to characterise AGN activity through emission line diagnostics. By studying this quiescent population, we aim to shed light on the mechanisms that drive quenching in the early universe, and contribute to our understanding of how galaxies are born, live, and eventually die.

18:00 → 18:15 Prizes: Presentation of Prizes

Convener: Jørgen Beck Hansen (NBI)