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PRODID:-//Heidelberg University//HePhySTO//EN2026-10-21 01:39:36
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DTEND:20261027T163000Z
UID:0cd929449a5cd100f7fd9305253c1346@physik.uni-heidelberg.de
DTSTAMP:20261022T233936Z
LOCATION:
DESCRIPTION:The WST project aims to design and construct an innovative 10-m
 etre class wide-field spectroscopic survey telescope (WST) in the southern 
 hemisphere. It will feature the parallel operation of two cutting-edge inst
 ruments: a high-multiplex (32\,000)\, large field-of-view (3 square degrees
 ) multi-object spectrograph (MOS) operating in both low- and high-resolutio
 n modes\, and a giant panoramic integral field spectrograph (IFS). WST’s am
 bitious top-level requirements place it well ahead of all existing and plan
 ned facilities. In its first five years of operation\, the MOS is expected 
 to observe 300 million galaxies\, 25 million stars at low resolution\, and 
 2 million stars at high resolution\, while the IFS will deliver 4 billion s
 pectra. These capabilities will enable transformative science across a wide
  range of astrophysical domains. A key strength of WST lies in the synergy 
 between its MOS and IFS instruments\, offering highly complementary spectro
 scopic survey modes. This dual approach is central to the project’s scienti
 fic ambition. WST is envisioned as the next major facility for ESO followin
 g the ELT\, and a proposal will be submitted in response to the upcoming ES
 O Call for Ideas in 2027. The project is backed by a large consortium of le
 ading institutes from European countries and Australia\, with deep expertis
 e in astronomical instrumentation and survey science. To arrange a visit wi
 th the speaker during the visit\, please contact their host: Dylan Nelson\n
 \nImported from https://www.physik.uni-heidelberg.de/hephysto/ (no warranty
  for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12897
SUMMARY:Heidelberg Joint Astronomical Colloquium: Roland Bacon -  WST - The
  Wide Field Spectroscopic Telescope
DTSTART:20261027T153000Z
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DTEND:20261103T163000Z
UID:c76c79271aedc9ca4645751721d42052@physik.uni-heidelberg.de
DTSTAMP:20261022T233936Z
LOCATION:
DESCRIPTION:The PHANGS-HST and JWST Treasury Programs have produced the mos
 t extensive inventories to date of optically visible and dust-obscured star
  clusters across nearby galaxies. A coherent picture is emerging of the ear
 liest phases of star formation\, built from complementary studies that cons
 istently point to short dust-clearing timescales (~3 Myr)\, in agreement wi
 th earlier optical studies. Together\, these results underscore the central
  role of early\, pre-supernova feedback in regulating the star formation cy
 cle. Drawing on the statistical power of tens of thousands of clusters span
 ning dozens of galaxies\, I will synthesize what PHANGS and related program
 s have revealed about cluster evolution\, feedback\, and the use of cluster
 s as “clocks” for timing key phases of star formation. Looking ahead\, I wi
 ll highlight work on the Habitable Worlds Observatory\, NASA’s next flagshi
 p astrophysics mission after Roman\, which will operate as a true “Super-Hu
 bble\,” with UV–optical capabilities to transform our understanding of star
  formation and fields across astrophysics. To arrange a visit with the spea
 ker during the visit\, please contact their host: Ralf Klessen\n\nImported 
 from https://www.physik.uni-heidelberg.de/hephysto/ (no warranty for accura
 cy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12898
SUMMARY:Heidelberg Joint Astronomical Colloquium: Janice Lee  - Decoding Ga
 laxies & Star Formation Feedback with 100\,000 Star Clusters: PHANGS-HST & 
 JWST today\, the future with HWO
DTSTART:20261103T153000Z
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DTEND:20261110T163000Z
UID:275937c8d690d0179c576e51005fd751@physik.uni-heidelberg.de
DTSTAMP:20261022T233936Z
LOCATION:
DESCRIPTION:The common envelope interaction happens between a growing or gi
 ant star of any mass and a more compact companion. The compact objects insp
 irals in the outer layers of the large star fully ejecting the envelope or 
 merging with the core. The CE interaction is at the origin of a number of s
 ingle and binary objects such as the progenitors of Type Ia supernovae\, ca
 taclysmic variables or the hypothesised Thorne-Zytkow objects. While 3D hyd
 ro simulations have come a long way in the last decade\, observations of th
 is fast phase have lagged\, until recently. Time-resolved surveys have rece
 ntly observed a number of objects that today are grouped into a single (alb
 eit somewhat diverse) class called Luminous Red Novae. These have been iden
 tified as common envelope mergers and marrying these observations with simu
 lations has become a priority to explain the observations and to (finally!)
  constrain the simulations. I will present the first simulations that targe
 t directly LRN light curves also including the effects of dust nucleation\,
  essential to reproduce light and colours of these objects. To arrange a vi
 sit with the speaker during the visit\, please contact their host: Fritz Rö
 pke\n\nImported from https://www.physik.uni-heidelberg.de/hephysto/ (no war
 ranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12899
SUMMARY:Heidelberg Joint Astronomical Colloquium: Orsola De Marco - Dusty c
 ommon envelope interactions and luminous red novae
DTSTART:20261110T153000Z
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BEGIN:VEVENT
DTEND:20261117T163000Z
UID:d25cbbde53462000001960f61b06e6d9@physik.uni-heidelberg.de
DTSTAMP:20261022T233936Z
LOCATION:
DESCRIPTION:Strongly lensed supernovae (SNe) are emerging as a new probe of
  cosmology and SNe.  When a SN is strongly lensed by a foreground galaxy\, 
 multiple images of the SN will appear around the foreground galaxy at diffe
 rent times.  Current surveys including Euclid and the Rubin Observatory Leg
 acy Survey of Space and Time will capture hundreds of strongly lensed SNe\,
  expanding the existing sample by two orders of magnitude.  These events of
 fer excellent opportunities to: (1) measure the Hubble constant via lensing
  time delays\, shedding light on the Hubble tension\, and (2) obtain unprec
 edented constraints on SN progenitors through early-phase spectra.  I will 
 give an overview of the first discoveries of lensed SNe and their cosmologi
 cal implications.  To arrange a visit with the speaker during the visit\, p
 lease contact their host: Philipp Girichidis\n\nImported from https://www.p
 hysik.uni-heidelberg.de/hephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12900
SUMMARY:Heidelberg Joint Astronomical Colloquium: Sherry Suyu  - Cosmology 
 and Supernovae through Cosmic Lenses
DTSTART:20261117T153000Z
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BEGIN:VEVENT
DTEND:20261124T163000Z
UID:1799fe6b163fe5181b645054e890077e@physik.uni-heidelberg.de
DTSTAMP:20261022T233936Z
LOCATION:
DESCRIPTION: Galaxies do not grow in isolation\, but within a cosmic web of
  intergalactic gas. The evolution of the galaxies and this intergalactic me
 dium are closely connected. As the first galaxies formed\, their light heat
 ed the gas surrounding them in a process known as reionization. Measuring t
 he progress of reionization can give us an indirect view of how and when th
 e first galaxies formed\, complementary to direct observations of the galax
 ies themselves with telescopes like JWST. In this talk\, I will discuss how
  we can constrain the timing of reionization with different observational p
 robes\, such as absorption in the spectra of distant luminous objects. I wi
 ll present my work interpreting these observations with large cosmological 
 simulations of the intergalactic medium. I will discuss what is known about
  the history of reionization\, and what questions are still to be answered.
  To arrange a visit with the speaker during the visit\, please contact thei
 r host: Sarah Bosman\n\nImported from https://www.physik.uni-heidelberg.de/
 hephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12901
SUMMARY:Heidelberg Joint Astronomical Colloquium: Laura Keating  - A view o
 f the first galaxies through the intergalactic medium
DTSTART:20261124T153000Z
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BEGIN:VEVENT
DTEND:20261201T163000Z
UID:6b23dd2dc13c8e9ca30f1a325d90423b@physik.uni-heidelberg.de
DTSTAMP:20261022T233936Z
LOCATION:
DESCRIPTION:Theories of galaxy formation\, structure\, and evolution increa
 singly include the effects of cosmic  rays on gas dynamics and energy balan
 ce. This is usually done by treating the cosmic rays as a fluid that is cou
 pled to the thermal gas by magnetic fields on global scales and electromagn
 etic fluctuations on kinetic scales. I will discuss the foundations and ass
 umptions of the fluid model\, assess whether it is correct and complete\,  
 where it can be improved\, and how it can be tested. To arrange a visit wit
 h the speaker during the visit\, please contact their host: Max Gronke\n\nI
 mported from https://www.physik.uni-heidelberg.de/hephysto/ (no warranty fo
 r accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12902
SUMMARY:Heidelberg Joint Astronomical Colloquium: Ellen Zweibel   - Resetti
 ng Cosmic Ray Propagation Theory
DTSTART:20261201T153000Z
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BEGIN:VEVENT
DTEND:20261208T163000Z
UID:dbc95be9b78e0d550a476aad04796c76@physik.uni-heidelberg.de
DTSTAMP:20261022T233936Z
LOCATION:
DESCRIPTION:The James Webb Space Telescope (JWST) has expanded our cosmic h
 orizon to the first few hundred million years after the Big Bang\, and is t
 ransforming our view of early star formation\, reionization and black hole 
 growth. It has revealed an unexpected excess of bright galaxies at z > 10\,
  peculiar nitrogen-enhanced abundance patterns\, evidence of ionized region
 s already in place at z ≈ 7–14\, and a new population of compact objects: L
 ittle Red Dots\, which may be an obscured phase of early black hole growth.
  These results point to a rapid build-up of galaxies and black holes at Cos
 mic Dawn that challenges theoretical models. I will review these discoverie
 s\, and present the latest progress in our understanding of these sources f
 rom ultra-deep JWST spectroscopy. \n\nTo arrange a visit with the speaker d
 uring the visit\, please contact their host: Max Gronke\n\nImported from ht
 tps://www.physik.uni-heidelberg.de/hephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12903
SUMMARY:Heidelberg Joint Astronomical Colloquium: Charlotte Mason  - New In
 sights into Cosmic Dawn from JWST
DTSTART:20261208T153000Z
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BEGIN:VEVENT
DTEND:20261215T163000Z
UID:c09d1b7bc083a64c52c21be30d513c77@physik.uni-heidelberg.de
DTSTAMP:20261022T233936Z
LOCATION:
DESCRIPTION:In recent years\, cosmic rays (CRs) have emerged as a key facto
 r shaping the interstellar medium (ISM) properties and influencing galaxy e
 volution. Yet\, despite significant advances\, modelling CR transport on ga
 lactic scales remains challenging\, largely due to the complex microphysica
 l interactions between CRs and thermal gas. As a result\, the true extent o
 f CR impact on ISM structure and evolution is still uncertain. In this talk
 \, I will present our latest efforts to model CR transport within the TIGRE
 SS MHD simulations of the multiphase ISM. I will discuss how CRs affect the
  dynamical and thermal state of the ISM in Milky Way-like galaxies\, showin
 g that while they have little effect on the star formation rate in galactic
  disks\, they significantly accelerate warm outflowing gas with mass loadin
 g factors higher than in simulations without CRs. These results hold across
  different galactic environments. Beyond these theoretical insights\, some 
 simulations include a spectral treatment of CR protons and electrons\, allo
 wing us to construct synthetic observables - such as CR spectra and non-the
 rmal emission - for direct comparison with observations. I will present our
  initial results comparing synthetic CR spectra with measurements in the so
 lar neighbourhood\, highlighting a very good agreement\, and discuss the im
 plications for CR transport. To arrange a visit with the speaker during the
  visit\, please contact their host: Philipp Girichidis \n\nImported from ht
 tps://www.physik.uni-heidelberg.de/hephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12904
SUMMARY:Heidelberg Joint Astronomical Colloquium: Lucia Armillotta  - Cosmi
 c-ray feedback in the multiphase interstellar medium
DTSTART:20261215T153000Z
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DTEND:20270112T163000Z
UID:365af0a65ebbf4b187286dc839d59c26@physik.uni-heidelberg.de
DTSTAMP:20261022T233936Z
LOCATION:
DESCRIPTION:To arrange a visit with the speaker during the visit\, please c
 ontact their host: Michela Mapelli \n\nImported from https://www.physik.uni
 -heidelberg.de/hephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12905
SUMMARY:Heidelberg Joint Astronomical Colloquium: Stefania Salvadori - The 
 nature of the first stars: data-driven constraints
DTSTART:20270112T153000Z
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BEGIN:VEVENT
DTEND:20270119T163000Z
UID:fe79c0a816305208ec0b5df5ed19a69b@physik.uni-heidelberg.de
DTSTAMP:20261022T233936Z
LOCATION:
DESCRIPTION:Shock waves are the universe's most prolific particle accelerat
 ors. The same mechanism\, diffusive shock acceleration\, is invoked to expl
 ain energetic particles in the solar wind\, cosmic rays from supernova remn
 ants\, and relativistic electrons at merger shocks in galaxy clusters. In t
 his picture\, particles gain energy by repeatedly scattering back and forth
  across the shock front\, aided by turbulent magnetic fields. Turbulence\, 
 however\, does not have to produce ordinary diffusion. If particles occasio
 nally make very long\, uninterrupted excursions\, they spread much faster t
 han a random walk allows. This behaviour\, known as a Lévy walk or superdif
 fusion\, appears in systems ranging from wild fires to particles transport 
 in the heliosphere. Radio relics are arcs of synchrotron emission that can 
 extend over megaparsecs\, tracing shocks driven by colliding galaxy cluster
 s. They provide a natural laboratory for testing how particles are transpor
 ted on large scales. We discovered that several relics show faint radio emi
 ssion reaching up to 100 kpc ahead of the shock\, where standard theory pre
 dicts almost nothing. I will show that superdiffusive electron transport ex
 plains this precursor naturally. I will then discuss how the spectral index
  profile ahead of the shock\, measurable with LOFAR\, MeerKAT and soon the 
 SKA\, can distinguish true superdiffusion from simply faster normal diffusi
 on.  In the final part\, I will show what other curiosities recent radio ob
 servations have revealed about cosmic-ray transport in the intra-cluster an
 d intra-group medium. To arrange a visit with the speaker during the visit\
 , please contact their host: Max Gronke\n\nImported from https://www.physik
 .uni-heidelberg.de/hephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12906
SUMMARY:Heidelberg Joint Astronomical Colloquium: Marcus Brüggen  - When Pa
 rticles Don't Random-Walk: Superdiffusion and the Largest Shocks in the Uni
 verse
DTSTART:20270119T153000Z
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DTEND:20270126T163000Z
UID:c5754044b47813a13a30c8e743d47db5@physik.uni-heidelberg.de
DTSTAMP:20261022T233936Z
LOCATION:
DESCRIPTION:\n\nThe field of exoplanets has made giant leaps over the last 
 few decades: we went from detecting planets\, to detecting their atmosphere
 s\, to characterizing the properties of their atmospheres. In my colloquium
  I will show how observatories such as the James Webb Space Telescope or th
 e upcoming Extremely Large Telescope allow us to probe deeper than ever bef
 ore: we begin to understand the multi-dimensional flow structure of atmosph
 eres in detail and study effects such as cloud nucleation in the highest at
 mospheric layers. I will also discuss one of the main challenges ahead: whi
 le in the past the community was limited by the noise of their data\, we ar
 e rapidly approaching a situation where we are limited by the models that w
 e use to compare to the data. Models can be too simplistic\, leading to bia
 ses\, or too complex\, leading to long computation times and inference (aka
  fitting) algorithms that get lost in highly dimensional parameter spaces. 
 Exciting times and lots of work lie ahead of us!\n\nImported from https://w
 ww.physik.uni-heidelberg.de/hephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12907
SUMMARY:Heidelberg Joint Astronomical Colloquium: Paul Mollière  - Studying
  the atmospheres of exoplanets in multiple dimensions
DTSTART:20270126T153000Z
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DTEND:20270202T163000Z
UID:4a8d70c4d45f4306b6cea02be9feccb2@physik.uni-heidelberg.de
DTSTAMP:20261022T233936Z
LOCATION:
DESCRIPTION:Galaxy formation is an inherently multiscale problem. Processes
  acting on sub-parsec scales\, such as radiative cooling\, turbulent mixing
 \, and the survival and growth of cold gas in hot flows\, shape the gas on 
 galactic and circumgalactic scales. Current simulations cannot resolve thes
 e scales\, so key properties\, and with them many observable predictions\, 
 often fail to converge. Multiscale problems are common across physics\, and
  a standard solution is to model unresolved scales through physically motiv
 ated "subgrid" prescriptions. In this talk\, I will introduce the new ASGAR
 D (Astrophysical Gas & Radiation Dynamics) group at ARI and our efforts to 
 build such a subgrid model for multiphase gas\, using high-resolution simul
 ations of the small-scale physics to inform and calibrate it\, and connecti
 ng it to observables such as absorption lines and Lyman-alpha emission.\n\n
 Imported from https://www.physik.uni-heidelberg.de/hephysto/ (no warranty f
 or accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12908
SUMMARY:Heidelberg Joint Astronomical Colloquium: Max Gronke - Resolving th
 e Multiphase\, Multiscale Universe
DTSTART:20270202T153000Z
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