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PRODID:-//Heidelberg University//HePhySTO//EN2026-10-22 00:08:33
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DTEND:20261022T101500Z
UID:70d106d187c0146b6f29b0904a672f48@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:Jellyfish galaxies provide a striking view of the interaction b
 etween galaxies and their surrounding\n\nenvironment. As galaxies move thro
 ugh the intracluster medium\, ram-pressure stripping can remove their\n\nin
 terstellar gas and produce extended\, asymmetric tails. These structures of
 fer a unique opportunity to study how environmental processes shape the evo
 lution of galaxies\, yet the physical connection between the properties of 
 the host galaxy and those of its stripped material remains poorly understoo
 d.\n\nIn this work\, we present a new framework to identify and characteriz
 e ram-pressure-stripped gas in galaxies\n\nfrom the IllustrisTNG50 cosmolog
 ical simulation. We identify Jellyfish galaxies using the MARK–log param-\n
 \neter space\, which provides a physically motivated characterization of ga
 laxies dominated by ram pressure. We then extend the phase-space approach o
 f Min et al. (2019) by incorporating the local gas density\, allowing the s
 tripped material to be identified on a particle-by-particle basis and its p
 hysical properties to be quantified. This approach enables us to move beyon
 d a simple Jellyfish/non-Jellyfish classification and investigate the\n\nph
 ysical properties of the tails themselves. In particular\, we explore the c
 orrelations between the properties of the host galaxies\, their interaction
  with the intracluster medium\, and the resulting tail properties\, includi
 ng their extent and gas content. By connecting the conditions experienced b
 y a galaxy with the structure produced by ram-pressure stripping\, this fra
 mework provides a new way to investigate the physical mechanisms governing 
 the formation and evolution of Jellyfish tails.\n\nImported from https://ww
 w.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=13006
SUMMARY:ARI Institute Colloquium: Isaac Gonzalez-Carbajal - A density-expan
 ded phase-space for gas in Illustrious-TNG: revealing Jellyfish structures
DTSTART:20261022T091500Z
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DTEND:20261029T111500Z
UID:5787e1f619c48ba45efd2490a98514f3@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:The Vera C. Rubin Observatory has reached an important mileston
 e by starting regular operations as the Legacy Survey of Space and Time (LS
 ST). However\, turning the alert stream into scientific discoveries still r
 equires methods beyond pure machine learning\, and the stream of alerts rel
 ayed via broker teams still\n\nneeds to be vetted by observers who are less
  robotic and more human. In this context\, we report on the first year of o
 perations of one important aspect of our in-kind contribution: our LSST TVS
 SC Galactic Science Observing Priority Manager. We provide insights into th
 e reasoning behind combining multiple classifier probabilities\, catalogue 
 queries\, and time series photometry. We summarize how we have used the fir
 st identified targets for immediate follow-up observations with the Las Cum
 bres Observatory global network of telescopes\, and we discuss which functi
 onalities will be developed in future. From a scientific perspective\, we w
 ill discuss the relevance of microlensing observations in the bulge fields 
 of the Nancy Grace Roman Space Telescope and beyond.\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=13007
SUMMARY:ARI Institute Colloquium: Markus Hundertmark - Operational Status o
 f the Vera C. Rubin Observatory’s Legacy Survey and ARI in-kind contributio
 n
DTSTART:20261029T101500Z
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DTEND:20261105T111500Z
UID:452e16fceca287fed2fca8a8a022fa56@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:Little Red Dots (LRDs) are compact sources at z > 5 discovered 
 with JWST\, characterized by\n\nbroad Balmer emission lines\, narrow absorp
 tion features\, and strong Balmer breaks. These signatures point to dense\,
  optically thick hydrogen gas surrounding rapidly growing black holes\, but
  their interpretation depends critically on how Balmer photons propagate th
 rough this gas. In this talk\, I will present the formation of Balmer lines
  in LRDs via scattering processes using 3D Monte Carlo radiative transfer s
 imulations. I will first discuss how various scattering processes reshape h
 ydrogen-line profiles and ratios\, demonstrating that broad\n\nand asymmetr
 ic Balmer lines do not necessarily trace gas kinematics alone. I will then 
 focus on modeling\n\nthe Halpha and Hbeta profiles of LRDs observed with JW
 ST/NIRSpec and constraining the n=2 hydrogen column\n\ndensity from the Bal
 mer break. The observations reveal a fundamental puzzle: Hbeta absorption i
 s systematically deeper than Halpha\, despite the substantially larger scat
 tering cross-section of Halpha. A homogeneous medium cannot\n\nreproduce th
 is ordering or simultaneously satisfy the column-density constraints from H
 alpha\, Hbeta\, and the Balmer\n\nbreak. We show that these tensions are re
 solved by a multiphase medium consisting of dense\, optically thick\n\nclum
 ps embedded in diffuse hot gas. Our results demonstrate that Balmer spectra
  encode the unresolved\n\nphase structure of gas in LRDs.\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=13008
SUMMARY:ARI Institute Colloquium: Seok-Jun Chang - Formation of Balmer Line
 s in Little Red Dots with Radiative Transfer in Multiphase Gas
DTSTART:20261105T101500Z
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DTEND:20261112T111500Z
UID:84dcc2b6718c3ea4eb13f7e29c696f3d@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:Active galactic nuclei (AGNs) are among the most powerful engin
 es in the Universe. Understanding\n\nhow accretion\, obscuration\, and feed
 back are connected is therefore essential for developing a complete picture
  of black-hole and galaxy evolution. In particular\, observations of indivi
 dual quasars have suggested a possible connection between powerful ionised 
 outflows and unusually weak X-ray emission relative to established mid-infr
 ared–X-ray relations. Testing this connection statistically requires large\
 , homogeneous\, multiwavelength samples. In this talk\, I will introduce th
 e development of the SDSS-V Black Hole Mapper quasar catalogue and discuss 
 the analysis presented in Demke et al. (2026). The sample combines optical 
 spectroscopy from SDSS-V with X-ray information from eROSITA and mid-infrar
 ed photometry from WISE. I will then present the extension of this analysis
  carried out as part of my master’s thesis. By increasing the sample size b
 y about a factor of three and adding X-ray spectral information\, this data
 set enables a more detailed investigation of the relationships between X-ra
 y emission\, mid-infrared luminosity\, black-hole mass\, accretion rate\, a
 nd the\n\nkinematics of ionised gas traced by the [O III] emission line.\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=13009
SUMMARY:ARI Institute Colloquium: Delvin Demke - SDSS-V BHM: Evidence for a
  link between X-ray weakness and galactic-scale ionised gas outflows in qua
 sars
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DTEND:20261119T111500Z
UID:bf3f857fa69968895e25b49e75556014@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:ABSTRACT 1: AGN feedback plays an important role in the evoluti
 on of their host galaxy\, yet the lifecycle\n\nof such an AGN event is stil
 l not fully understood. First observations and new simulations suggest the 
 presence of AGN driven outflows even after the galaxy nucleus is no longer 
 active. Using resolved spectroscopic data obtained with integral field unit
 s\, these so-called fossil outflows can be studied on a larger scale. Predi
 ctions suggest that up to 60% of all observed outflows might be of fossil n
 ature. In this talk\, I will present a selection method for candidate fossi
 l outflow regions in the SDSS-IV MaNGA galaxy sample comprising about 10\,0
 00 galaxies\n\nat low redshift. The method is based on kinematic elevation 
 of the ionized gas\, traced by broad [OIII]5007 emission line widths. By co
 mparing the gas kinematics with the stellar velocity dispersion\, gas motio
 ns dominated by the gravitational potential can be distinguished from outfl
 ow-driven motions. We identified a fossil outflow candidate sample of 269 n
 on-AGN galaxies showing they are common in low redshift galaxies. I discuss
  some promising candidates in more detail as well as an analysis of the out
 flow properties of the outflow candidates compared to currently active gala
 xies. Simple outflow age calculations suggest outflow detections\n\nup to a
 bout 8 Myr after the AGN shutdown.\n\n\n\n\n\nABSTRACT 2: One of the prime 
 mechanisms suspected of driving the decline of star formation in massive\n\
 ngalaxies is the so-called Active Galactic Nucleus (AGN) feedback\, which s
 till remains to this day as one of the least understood concepts in galaxy 
 evolution. AGN feedback acts via many different\, often combined\, modes an
 d when trying to decipher these processes it is crucial to tackle the diffe
 rent forms of feedback one by one to dissect their multi-faceted nature and
  understand which effects result from which causes. In this talk I will pre
 sent a case-study conducted as part of my Bachelor Thesis by my group on on
 e AGN host galaxy\, dubbed the Cone Source\, aimed at investigating how AGN
  feedback in the form of biconical outflows can locally affect the molecula
 r gas reservoir as well as star formation. For this purpose\, we combined a
 nd analyzed spatially resolved 12CO(1-0) observations taken by the Northern
  Extended Millimeter Array (NOEMA) with optical-IFU data from the MaNGA sur
 vey. In this data we find correlations of stellar properties with the multi
 -phase outflow strength as well as signs of a recent starburst phase within
  our galaxy\, highlighting the complex evolution and interplay between AGN 
 and their host galaxies.\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=13010
SUMMARY:ARI Institute Colloquium: 1. Theodor Brosi (ARI)\, 2. Matthias Kunt
 z (ARI) - 1. Kinematic signatures for fossil AGN outflows in the SDSS MaNGA
  sample / 2. The impact of multi-phase AGN driven outflows: A galaxy caught
  between starbust and quenching?
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DTEND:20261126T111500Z
UID:cfb9fd9c6e66d773d89ce0498f120cef@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:Quenching mechanisms have been extensively studied over the pas
 t decade\, yet identifying which\n\nprocesses shut down star formation\, th
 eir relative importance\, and on what timescales\, remains a central\n\npro
 blem in galaxy evolution. In this talk\, I will present the first systemati
 c census of quenching mechanisms using kinematic asymmetries in a large sam
 ple (> 6700 galaxies) of spatially resolved galaxies\, providing a unified 
 view of what halts star formation in the local Universe (z < 0.2). Our anal
 ysis reveals that the most effective quenching pathways leave minimal kinem
 atic imprints by the time galaxies are fully quenched\, pointing to slow-ac
 ting processes (>3 Gyr) such as starvation and maintenance feedback. To com
 pare these observations with theoretical predictions\, we use mock galaxies
  from IllustrisTNG to investigate satellite quenching pathways\, focusing o
 n the role of the circumgalactic medium (CGM). Using a merger-tree-based al
 gorithm\, we reconstruct the baryonic\, dark-matter\, structural\, and chem
 ical histories of about 7300 spatially\n\nresolved galaxies\, using time si
 nce infall as the physical axis along which quenching unfolds. For the firs
 t time\, we present the coupled evolution of the hot and cool gas reservoir
 s after infall. Satellites lose about 90% of their hot CGM within about 4 G
 yr\, with the depletion increasing with residence time and remaining largel
 y independent of stellar mass. The hot gas mass correlates strongly with SF
 R\, establishing the CGM as a long-term fuel reservoir. Despite losing litt
 le stellar mass\, satellites experience gas depletion and tidal stripping o
 f their dark matter and metal-poor stellar outskirts\, becoming more compac
 t and metal-rich than centrals at fixed mass. Our results suggest that the 
 gradual erosion of the hot CGM is a key link between infall and the slow sh
 utdown of star formation.\n\nImported from https://www.physik.uni-heidelber
 g.de/hephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=13011
SUMMARY:ARI Institute Colloquium: Natan de Isidio - The kinematic imprintin
 g of environmental quenching
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DTEND:20261203T111500Z
UID:1b21884a14c98182b0d29df0a7d696a4@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:ESO is constructing the Extremely Large Telescope (ELT)\, which
  will become the world’s largest\n\noptical and near-infrared telescope and
  a flagship facility for ground-based astronomy in the coming decades. With
  its 39-metre primary mirror and unprecedented sensitivity and spatial reso
 lution\, the ELT will open new parameter space across a wide range of astro
 physical topics\, from exoplanets and star formation to galaxy evolution an
 d cosmology. Realising this scientific potential depends critically on a ne
 w generation of highly sophisticated instruments developed by international
  consortia together with ESO. In this talk\, I will provide\n\nan overview 
 of the ELT and its instrumentation\, with particular emphasis on the two in
 struments that are\n\nmost advanced in development: MICADO\, the high-resol
 ution near-infrared imager\, and METIS\, the mid-infrared imager and spectr
 ograph. I will discuss their scientific capabilities\, technical challenges
 \, and the\n\ntransformational opportunities they will provide for future a
 stronomy.\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=13012
SUMMARY:ARI Institute Colloquium: Heidi Korhonen - Instrumentation for the 
 "world’s biggest eye on the sky"
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DTEND:20261210T111500Z
UID:30ea9035155af5a5896e6952e1781900@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:In this talk\, I will present the SOFIA Legacy Project FEEDBACK
 \, which has provided the first\n\nlarge-scale\, velocity-resolved view of 
 stellar feedback in galactic star-forming regions. This was achieved by uti
 lising the [CII] 158 micron and [OI] 63 micron lines\, which are key tracer
 s of photodissociation regions (PDRs) at\n\nthe interface between ionised a
 nd molecular gas. By probing feedback across a wide range of physical scale
 s and evolutionary stages\, FEEDBACK provides a comprehensive observational
  perspective on the formation\, evolution and eventual dispersal of molecul
 ar clouds.\n\nOne of the project’s major findings concerns cloud formation 
 and dispersal. In Cygnus X\, widespread high-\n\nvelocity [CII] emission pr
 edominantly tracing neutral gas reveals the formation of molecular clouds v
 ia converging atomic flows (Schneider et al. 2023). In the same region\, th
 e Diamond Ring exemplifies a distinct\n\nfeedback geometry: it arises as th
 e terminal phase of a stellar wind bubble expanding into a flat molecular\n
 \ncloud\, where bipolar breakout along the low-density directions above and
  below the cloud plane produces a\n\ntrue ring - not a sphere - as the obse
 rvable signature. This ring morphology is detected in [CII] and confirmed b
 y dedicated HD simulations following the evolution of a bubble in a flat mo
 lecular sheet (Dannhauer et al. 2025). Cloud dispersal is further evidenced
  across several FEEDBACK regions (RCW79\; Bonne et al. 2023\; Bonne et al. 
 submitted)\, where [CII] emission reaches velocities of up to 25 km/s\, org
 anised partly in fragmented shells and partly in flows escaping through low
 -density channels. Derived mass-loss rates of order 0.01 Msun/yr imply shor
 t cloud erosion timescales of less than 5 Myr\, providing direct observatio
 nal evidence that stellar feedback can rapidly disperse molecular clouds an
 d regulate star formation efficiency.\n\nAcross the full FEEDBACK sample ex
 panding bubbles are a common feature. While classical expanding\n\nshells a
 re observed\, the [CII] data often reveal fragmented\, incomplete or asymme
 trical bubbles\, frequently accompanied by high-velocity wings and multiple
  kinematic components. Expansion velocities exceeding 10 km/s are detected 
 in most regions\, but their dynamics often require additional energy input 
 from stellar winds beyond pure thermal pressure.\n\nOverall\, FEEDBACK has 
 provided a revised model of feedback-driven cloud evolution across scales: 
 (i) molecular clouds form and disperse efficiently on short timescales\; (i
 i) the geometry of feedback is fundamentally anisotropic and is governed by
  the turbulent\, porous structure of the interstellar medium (ISM)\; (iii) 
 [CII] can be used to trace both expanding shells and escaping gas flows\; a
 nd (iv) individual embedded systems\, such as S106 and the Diamond Ring\, d
 emonstrate that feedback can be detected from protostellar to cloud scales.
 \n\nAlongside other observations presented in this talk it highlights the p
 ower of FIR observations.\n\nBuilding on these results\, the next step will
  be taken by the GEco survey on the CCAT/FYST telescope\, with\n\nexpected 
 first light autumn this year. GEco will extend the FEEDBACK studies by mapp
 ing the [CII] and\n\nmid-J CO lines across entire molecular cloud complexes
  and the broader Galactic ecosystem on a large scale.\n\nTogether with FEED
 BACK\, GEco will also probe the carbon cycle in the galactic interstellar m
 edium.\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=13013
SUMMARY:ARI Institute Colloquium: Simon Dannhauer - Climbing the Ladder: St
 ellar Feedback from SOFIA to CCAT/FYST
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DTEND:20261217T111500Z
UID:88dc043e737dfad88d09b2e907929473@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:Gaia Data Release 4\, to be published on 2 December 2026 at 12:
 00 CET\, is the first release based\n\non Gaia’s complete nominal mission\,
  covering roughly 5.5 years of observations\, almost doubling the 34-month 
 observation baseline underlying Gaia DR3. Because proper-motion precision i
 mproves with the observation time span to the power of 3/2 - much faster th
 an the square-root scaling of parallax precision - this extended baseline y
 ields a disproportionate leap in astrometric accuracy for anything involvin
 g stellar motion: binary\n\nand multiple-star orbits\, cluster dynamics\, a
 nd subtle accelerations caused by unseen companions.\n\nThe full release co
 mprises astrometric\, photometric\, and spectroscopic catalogues for close 
 to two billion\n\nsources\, together with substantially expanded non-single
 -star solutions\, variability\, and astrophysical parameters. This talk pre
 views the scientific scope of the release through the topics addressed by t
 he DR4 Performance Verification Papers\, spanning the full breadth of Gaia 
 science: dormant black holes in binary systems\; exoplanets revealed throug
 h subtle astrometric and spectroscopic signatures\; the structure and dynam
 ics of open\n\nand globular star clusters\; asteroids\, asteroid families\,
  and comets in the Solar System\; the orbits and dynamics of the nearest st
 ars to the Sun\; the coolest and least massive stars at the bottom of the m
 ain sequence\; classical pulsating stars tracing the spiral structure of th
 e Milky Way\; time delays in gravitationally lensed\n\nquasars\; and the fi
 rst three-dimensional cartography of a galaxy beyond the Milky Way\, the La
 rge Magellanic\n\nCloud. Together\, these studies illustrate how Gaia DR4 w
 ill transform our view of the Milky Way and its\n\nneighbourhood\, from the
  Solar System to the structure of the Local Group and beyond.\n\nAs the det
 ailed scientific results remain under embargo until the release date\, this
  talk will present the concrete findings in full after 2 December 2026\, 12
 :00 CET.\n\nImported from https://www.physik.uni-heidelberg.de/hephysto/ (n
 o warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=13014
SUMMARY:ARI Institute Colloquium: Stefan Jordan - Gaia DR4 – The First Comp
 lete Gaia Star Catalogue
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UID:0fff2bb0b9ad1691ae9d11d1994fa417@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:Very massive stars (VMS) are born with masses above 100 Msun an
 d represent the most extreme\, albeit rare\, class of stellar objects. They
  shine with luminosities exceeding a million times that of the Sun and\n\nd
 rive powerful line-driven winds that inject momentum and chemically process
 ed material into the interstellar medium. VMS are invoked to explain distin
 ctive spectral features in unresolved stellar populations\, yet the stars t
 hemselves remain poorly understood. At the highest masses\, the scarcity of
  observational constraints limits our ability to test models of VMS evoluti
 on\, while at high metallicity\, uncertainties in mass loss remain a major 
 challenge. In this talk\, I will motivate the detailed investigation of O/W
 Nh stars as key laboratories\n\nfor probing VMS evolution. In the Milky Way
 \, only nine such stars are currently known\, and none has\n\npreviously be
 en quantitatively characterized using detailed stellar atmosphere modeling.
  For the first time\, we have computed models reproducing the observed opti
 cal spectrum of WR 31-1\, the most luminous Galactic O/WNh star. I will pre
 sent the results of this pilot study and discuss how they motivate future t
 argeted observational campaigns.\n\nImported from https://www.physik.uni-he
 idelberg.de/hephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=13015
SUMMARY:ARI Institute Colloquium: Joris Josiek - WR 31-1 and the search for
  Very Massive Stars in the Milky Way
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UID:369f71eb6fb5fcb5ffcd4a5fbb91e05f@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:The evolution of galaxy clusters is strongly shaped by the phys
 ics of the intracluster medium (ICM)\, where processes such as turbulence\,
  mixing\, and galaxy-ICM interactions drive much of the cluster’s dynamical
  state. One key ingredient is viscosity\, which can suppress small-scale ga
 s motions and modify\n\ndensity fluctuations and magnetic fields. Yet\, bot
 h the strength and nature of viscosity in the ICM remain\n\nuncertain. In t
 his talk\, I will present results from high-resolution cosmological simulat
 ions that explicitly include viscosity\, with a particular focus on the Com
 a cluster. Recent XRISM observations of Coma have revealed unexpectedly low
  small-scale gas motions\, challenging our current understanding of ICM dyn
 amics. I will explore whether viscosity can help explain these observations
 \, comparing inviscid simulations with models including both isotropic and 
 anisotropic viscosity. I will show how these different treatments affect cl
 uster morphology\, turbulence\, and ICM fluctuations\, and discuss how simu
 lations and observations together can constrain the microphysics of the ICM
 .\n\nImported from https://www.physik.uni-heidelberg.de/hephysto/ (no warra
 nty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=13016
SUMMARY:ARI Institute Colloquium: Tirso Marin Gilabert - Viscous or Turbule
 nt? The XRISM Puzzle of Coma
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DTEND:20270128T111500Z
UID:783e3b2f04d04aa63413f4fb80b2a9e4@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:The Dark Energy Spectroscopic Instrument (DESI) Data Release 1\
 , published in March 2025\, provides a lot of spectra of the ionized inters
 tellar medium in HII-regions within supposed dwarf galaxies.\n\nUsing the s
 trong line calibration method\, we derive their gas-phase oxygen abundance 
 (12+log(O/H))\, as a\n\nmetallicity indicator. Comparing these metallicitie
 s with stellar-mass estimates (CIGALE\, FASTSPECFIT)\,\n\nprovided by the D
 ESI VACs\, we find that a "significant percentage" of the dwarf galaxies de
 viate significantly from the mass-metallicity relation. We find that this i
 s due to deblending issues of extended galaxies in Legacy Survey (LS) data 
 releases - including DR9\, on which DESI DR1 photometry is based - leading 
 to faulty luminosities across all color bands in DESI DR1. This subsequentl
 y disturbs mass estimates. Using segmentation maps applied to model images\
 , which we reconstruct from LS DR9 Tractor catalog data\, we estimate the l
 uminosities in different bands for over 3 million galaxies at z < 0.2. We f
 ind that for a "significant percentage" of the galaxies our derived magnitu
 des are more than 1 mag brighter than DESI DR1 results.\n\nWith this correc
 ted photometry\, genuine outliers from the mass-metallicity relation can no
 w be observed.\n\nImported from https://www.physik.uni-heidelberg.de/hephys
 to/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=13017
SUMMARY:ARI Institute Colloquium: Victor Wichelhaus - Dwarf galaxies in DES
 I DR1: Deviation from the mass-metallicity relation or faulty photometry?
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DTEND:20270204T111500Z
UID:1c197e7058b41fa294a056c2649249fe@physik.uni-heidelberg.de
DTSTAMP:20261023T220833Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:Studying the impact of Active Galactic Nuclei (AGN) on the inte
 rstellar medium at high redshift\n\nis crucial for understanding how galaxi
 es evolve. In this talk\, I will first present results from 4C +03.24\, a p
 owerful radio galaxy at z ~ 3.5\, using integral-field spectroscopy obtaine
 d with JWST/NIRSpec. The joint analysis of our observations with archival V
 LT/MUSE and HST data reveals extended continuum emission (~14 kpc)\, possib
 ly arising from recent star formation and associated with nearby companions
 . The presence of a gap in the [CII] emission within the bipolar region dom
 inated by AGN photo-ionization may provide direct evidence of negative AGN 
 feedback. We further find that the outflow power associated with the kinema
 tically\n\ndisturbed ionized gas peaks ~ 2 kpc from the nucleus\, with a lo
 w kinetic coupling efficiency of ~0.0063%. In the second part\, I will disc
 uss new results on AGN across different epochs (1 < z < 6)\, obtained from 
 archival JWST data.\n\nImported from https://www.physik.uni-heidelberg.de/h
 ephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=13018
SUMMARY:ARI Institute Colloquium: Bruno Dall’Agnol de Oliveira - Exploring 
 AGN Feedback at different epochs with JWST
DTSTART:20270204T101500Z
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