Events, Seminars, Talks

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The Herschel surveys have enabled the detection of numerous dusty luminous sub-millimetre galaxies in the early universe. Follow-up observations of these sources are essential to determine their nature and the physical properties of their interstellar medium\; reliable measurements of their redshifts are therefore crucial to explore the molecular and atomic gas of these objects. We will here present the results of a Large Program (z-GAL), using NOEMA, aimed at a comprehensive 3 and 2-mm spectroscopic redshift survey of a large (~135 sources) sample of the brightest (S_{500 ?m}>\;80 mJy) galaxies selected from the Herschel H-ATLAS and HerMES surveys, which probe the peak of cosmic evolution (2<\;z<\;4). The results highlight the nature of the sources, including lenses, hyper-luminous galaxies, and proto-clusters. We will describe the main results of the survey, report on recently obtained complementary data, using NOEMA, ALMA and the VLA, addressing aspects of feedback activity in selected sources, and present a serendipitous discovery of a remarkable gravitationally amplified galaxy.

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Stellar spectroscopy is going through a revolution, changing manual labor by automated processing and artificial intelligence, and replacing human observers and single-target instruments by robots and highly multiplexed spectrographs. Yet, improvements at the fundamental physics level are happening far slower, and the most popular stellar atmosphere models employed to interpret stellar spectra are based on codes originally written in the 1970's. In this talk I will discuss recent advances and reflect on what's missing to realize actual progress in our understanding of the assembly and early evolution of the Milky Way from the study of the most primitive stars. To arrange a visit with the speaker during the visit, please contact their host: Hans Ludwig (LSW)

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Star clusters are the one of the most useful places in the universe for studies of stellar and galactic evolution. Formed when stars collapse from the same molecular cloud into a cluster, star clusters offer a unique way to study stars of a homogeneous age and chemical composition across a range of masses. In the age of the Gaia satellite, the census of star clusters in our galaxy has exploded in size - but not without also presenting a number of challenges that require new machine-learning based techniques to solve. In this talk, I will present my work so far aiming to improve many aspects of the census of galactic star clusters in the age of Gaia. After an introduction to the field, I will start by discussing our published catalogue of over 7000 clusters, which represents the largest homogeneous unduplicated catalogue of Milky Way star clusters to date. I will discuss our recently published update to the original catalogue that measures the largest ever sample of cluster masses to better define them observationally, including many surprising results like that most clusters in the galaxy appear to have the same initial mass function - but only after first correcting for selection effects. I will discuss our ongoing work on the sample’s completeness and variable star content. Finally, I will discuss future avenues for research, including upcoming data releases like Gaia DR4 and the LSST.

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I will present the latest insights into the formation pathways of early galaxies, placing them in the broader context of self-regulated galaxy growth observed both today and during cosmic noon. Beginning with new theoretical developments from the cosmological THESAN-zoom simulations, I will explore how early star formation is regulated, how galaxies evolve along the star-forming main sequence, and how their sizes increase over cosmic time. I will then connect these theoretical predictions to recent JWST observations from NIRCam and NIRSpec as part of the JADES survey – one of the most extensive observational campaigns conducted with JWST. I will highlight the diversity of galaxies at cosmic dawn (redshift z>10), where vigorous star formation and black hole growth are prevalent. Next, I will examine the role of mergers in shaping galaxy evolution and discuss the emergence of disk-like structures during the Epoch of Reionization (z=4-10). I conclude by placing observational constraints on the morphological evolution of galaxies within the framework of star formation variability, providing a comprehensive view of how early galaxies grew and evolved. To arrange a visit with the speaker during the visit, please contact their host: Richard Tuffs

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To arrange a visit with the speaker during the visit, please contact their host: Laura Kreidberg

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The field of black hole accretion is seeing a renaissance in the past 5–10 years, thanks to the advent of time domain surveys across the electromagnetic spectrum. These surveys monitor hundreds of thousands of galaxies at unprecedented cadence, revealing the secrets black holes were keeping while we weren’t watching. In this talk, I will present recent highlights on black hole accretion and growth in two parts: (1) in “Standard Accretion” events like Active Galactic Nuclei and accreting stellar-mass black holes, where we can use Reverberation Echoes to map the inflowing gas and measure the black hole spin, (2) through the discovery and characterization of exotic transients, like Tidal Disruption Events, and a new phenomenon called Quasi-Periodic Eruptions (QPEs), which have been posited as due to the presence of an orbiting stellar mass object, or EMRI. We will discuss the current state of the field, and implications for joint detections in the next decade with future space missions like AXIS, the X-ray Probe recently selected for a NASA Phase A study, and the recently adopted LISA Gravitational Wave Observatory. To arrange a visit with the speaker during the visit, please contact their host: Julien Wolf

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Magnetic fields permeate nearly every astrophysical environment, from planets and stars to galaxies and galaxy clusters. In these cosmologically overdense regions, magnetic fields are thought to arise primarily from magnetohydrodynamic (MHD) dynamos. These mechanisms convert turbulent kinetic energy into magnetic energy through the stretching and twisting of field lines. In the first part of this talk, I will present recent advances in our understanding of MHD dynamos. In the second part, I will focus on the vast underdense regions of space, cosmic voids, where blazar observations have revealed the existence of magnetic fields. As voids lack turbulence and therefore the energy source of classical dynamos, these large-scale magnetic fields likely originate in the very early Universe shortly after the Big Bang and therefore offer a unique window into fundamental physics. I will outline key theoretical models of magnetogenesis and present new insights in the pre-recombination evolution of these primordial magnetic fields from state-of-the-art numerical simulations. To arrange a visit with the speaker during the visit, please contact their host: Philipp Girichidis

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Episodes of supermassive black hole growth are known as “active galactic nuclei” (AGN). These are crucial periods in the life cycle of all massive galaxies. One way in which AGN can influence galaxies, is by driving multi-phase outflows of gas. However, the orders-of-magnitude ranges in spatial, temporal, and temperature scales makes this a very challenging process to constrain observationally. Questions remain on the properties, potential impact, and physical drivers of these outflows. I will present our work exploring these questions by combining cosmological simulations, high-resolution simulations of individual galaxies, and multi-wavelength observations. The power of this combined approach is understanding how specific observational experiments can (or cannot) test specific aspects of different theoretical models. Indeed, I will show how some published observational evidence that is in apparent contradiction with models, can be explained away once accounting for missing/unknown information in the data, and with a clearer understanding of which measurements can be robustly compared to simulations. I will finish by presenting new observational results highlighting a connection between dust, radio emission, and AGN outflows that now requires a physical explanation. To arrange a visit with the speaker during the visit, please contact their host: Marco Alban (ARI)

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To arrange a visit with the speaker during the visit, please contact their host: Fabian Schneider

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KoCo Signature Speaker

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Giant low surface brightness galaxies (gLSBGs) have the largest discs in the Universe with the radii up to 130 kpc. The formation of such enormous discs is a stress-test for the hierarchical galaxy formation paradigm and without clarifying it we cannot paint a coherent picture of galaxy evolution. In the talk I will give the answers to the following questions. How rare are gLSBGs? What are the formation scenarios of gLSBGs? And how does it all correspond to the results of modern cosmological simulations? These answers are based on both in-depth study of 8 gLSBGs, including the results of our deep spectroscopic and photometric observations, HI data collected in the framework of our observing programs and complemented by archival datasets. Finally, we used deep optical images from HSC Subaru Strategic Program and publicly available redshift catalogs, estimated the volume density of gLSBGs in the local Universe and compared it to state-of- the-art numerical simulations.

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To arrange a visit with the speaker during the visit, please contact their host: Dominika Wylezalek

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