Vorträge, Seminare, Ereignisse

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Exoplanetary systems exhibit an extraordinary diversity in their physical properties and architectures, yet the origins of this diversity remain uncertain. Key open questions include when and how planets form, and how they evolve and interact with their birth environment, the protoplanetary disks. By leveraging multi-wavelength observations, we can probe different regions of these disks and the processes that shape planet formation and disk evolution. In this talk, I will highlight results from the exoALMA Large Program, a sub-millimeter planet-hunting campaign, that exploits molecular line observations to reveal a rich variety of kinematic perturbations.

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The discovery of billion-solar-mass black holes within the first Gigayear of cosmic history presents an intriguing puzzle: how did supermassive black holes (SMBHs) grow so rapidly in such a short amount of cosmic time? In this talk, I will introduce new approaches to probing the early growth of SMBHs. First, I will present the first measurement of the clustering strength of luminous quasars and their surrounding galaxies at z>6 using recent observations from the James Webb Space Telescope. These measurements allow us to infer the properties of the quasars’ host dark matter halos and their duty cycles, offering new insight into the environments that foster SMBH growth. I will then highlight new results from deep spectroscopic observations of background galaxies behind a luminous high-redshift quasar, which allow us to tomographically map the quasar’s ionized bubble, constraining the obscured fraction of quasars, their emission geometry, and the timescales of SMBH growth. To arrange a visit with the speaker during the visit, please contact their host: Nadine Neumayer

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Cold molecular gas is a key component in galaxy evolution, as it forms stars, bears feedbacks, and feeds supermassive blackholes. Interferometric observations of the Atacama Large Millimeter/submillimeter Array (ALMA) have remarkably advanced this field in the past decade. For spiral galaxies, a larger sample with higher physical resolution than before is systematically surveyed. I will discuss the molecular gas morphology and kinematics in three megamaser (Seyfert-II) galaxies at resolutions of around 100 pc. We found prevalent irregularities, potentially related to active galactic nucleus feedback and supermassive black-hole feeding. For early-type galaxies, it is now feasible to spatially resolve giant molecular clouds (GMCs). I will talk about GMCs at 15-pc resolution of the lenticular galaxy, NGC1387. Their dynamical states (Larson relations, virial parameters, etc.) are surprisingly similar to those in spiral galaxies. For our own Milky Way centre, a new ALMA large programme has mapped the central molecular zone (CMZ) at unprecedented spatial (sub-pc) and spectral (0.2 km/s) resolutions. Here, we found evidence of galactic shear effects and magnetic fields driving gas structure morphologies. I will conclude by summarising the physical drivers of molecular gas properties at different scales and in different environments.

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The carbon footprint of astronomical research has received increasing attention in recent years. A significant portion of this impact arises from how scientific activities are conducted, including travel to conferences, the use of energy-intensive supercomputers, and the construction and operation of increasingly complex telescopes that require substantial resources.
Can astronomy become more sustainable? Is it possible to design research practices, infrastructures, and institutional frameworks that reduce environmental impact while still enabling transformative scientific discoveries?
In this talk, I will give an overview of the carbon footprint linked to astronomical research. I will examine different types of environmental impacts, share examples, and suggest solutions that individuals, research institutes, and organizations can use to help make the field more sustainable.

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Galaxy clusters, representing the peaks in the cosmic density field, serve as an independent and powerful tool for investigating the evolution of cosmic structures. The strategic identification of these clusters through multi-wavelength surveys is essential for advancing our understanding of gravitational theory, general relativity, and cosmological models. Launched in 2019 aboard the Spectrum-RG mission, eROSITA marked a major milestone in astronomy by enabling the construction of the largest pure sample of galaxy clusters and groups detected through their hot intra-cluster medium in the X-ray band. In this talk, I will present results from my group’s work on deriving cosmological constraints from the evolution of the cluster mass function, combining eROSITA data with optical surveys such as DESI Legacy, DES, HSC, and KIDS. These parameters are constrained at a percentage level through the evolution of the cluster mass function, representing a significant leap forward. Beyond cosmology, a central focus of my research is on AGN feedback and its role in shaping galaxy and structure formation. Leveraging the statistical power of the eROSITA sample, we have detected warm baryons within cosmic filaments and cluster outskirts, offering a first glimpse of baryons in the faint, diffuse cosmic web. To arrange a visit with the speaker during the visit, please contact their host: Matteo Maturi

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The lives of galaxies are governed by the accretion of gas, its consumption via star formation, its removal or heating through feedback, and environmental effects. In recent years, the James Webb Space Telescope (JWST) has unveiled an unexpectedly high density of massive quiescent galaxies at high redshift , challenging standard models of early galaxy growth. Cosmological simulations predict that these quenched systems preferentially live in dense regions, where they experience accelerated growth and more feedback from Active Galactic Nuclei (AGN). Observationally, clustered environments indeed exhibit enhanced AGN activity, and AGN feedback is increasingly viewed as the primary driver of quenching in massive galaxies. In this talk, I will present JWST/NIRISS slitless spectroscopic observations of a merging protocluster at z=3 that simultaneously hosts two quiescent galaxies and a luminous, starbursting quasar at its centre. I will discuss the kinematics, substructure, and halo properties of the system, as well as examine its evolutionary stage and AGN incidence. The central quasar is an example of the rare and intense “extremely red quasar” phase: a luminous and dusty population thought to constitute an early break-out stage, with ionised outflows reaching thousands of km/s - the most extreme warm winds known to date. Spatially resolved observations with JWST/NIRSpec offer a detailed view on gas dynamics, mass loading, and localised physical conditions, bridging the extended environment down to the nucleus. At low redshifts, I will focus instead on a population of AGN with low-velocity ionised outflows and suppressed star formation, which may represent a later phase of feedback. New spatially resolved molecular gas measurements with NOEMA enable a detailed kinematic comparison of cold and warm gas phases, and reveal how the outflows reshape the cold gas reservoir while regulating star formation efficiency. Together, these results showcase distinct examples of how AGN feedback can manifest across different cosmic times and environments.

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