BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//CERN//INDICO//EN
BEGIN:VEVENT
SUMMARY:Mapping the Faint Frontier: Improved Local Group Kinematics with J
 WST + Gaia + HST Astrometry
DTSTART;VALUE=DATE-TIME:20261028T182300Z
DTEND;VALUE=DATE-TIME:20261028T182400Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3710@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Liwen Chen (University of Toronto)\nStellar proper m
 otions (PMs) are fundamental for reconstructing the Local Group dynamics\,
  understanding the Milky Way accretion history\, and constraining the natu
 re of dark matter. While Gaia is powerful for measuring PMs\, its performa
 nce is limited for faint sources (G > 20 mag). Previous studies on Gaia + 
 Hubble Space Telescope (HST) astrometry have shown that combining telescop
 es achieved more precise PM measurements than Gaia alone.\n\nMotivated by 
 GaiaHub\, a previous Gaia + HST tool\, we have developed GaiaWebb\, which 
 combines Gaia and James Webb Space Telescope (JWST) observations. GaiaWebb
  retrieves JWST images\, extracts stellar positions and magnitudes\, cross
 -matches JWST sources with Gaia stars\, aligns JWST images to the Gaia ref
 erence frame\, and then measures the improved PMs using large JWST-to-Gaia
  time baselines. We have also expanded another Gaia + HST tool\, BP3M (Bay
 esian Positions\, Parallaxes\, and Proper Motions)\, to simultaneously com
 bine JWST + Gaia + HST measurements. The enhanced BP3M differs from GaiaWe
 bb in that it uses Gaia data as priors while jointly aligning images and m
 aking measurements. We tested our new tools on the Large Magellanic Cloud 
 and Draco dwarf galaxy\, and the resulting PMs are consistent with the lit
 erature measurements. GaiaWebb and BP3M improve PM precision by factors of
  5-20 compared to Gaia DR3 alone\, with faint stars (G > 19 mag) seeing th
 e largest improvement. \n\nOur future work will include producing publicly
  available catalogues of improved PMs\, calibrating those catalogues throu
 gh comparisons with the literature\, and measuring new bulk motions of Loc
 al Group structures.\n\nhttps://nyx.physics.mcgill.ca/event/587/contributi
 ons/3710/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3710/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Bayesian and Brisk: Scalable AGN Lightcurve Simulation and Fitting
  for Supernova Cosmology and Population Studies
DTSTART;VALUE=DATE-TIME:20261028T182200Z
DTEND;VALUE=DATE-TIME:20261028T182300Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3716@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Zoe Augspach (University of Toronto)\nActive Galacti
 c Nuclei (AGNs) are dense\, bright regions at the centre of galaxies thoug
 ht to be caused by matter accreting into a supermassive black hole. Millio
 ns of AGNs have been observed\, and population-level studies are needed to
  learn about AGN physics. \n\nOn the other hand\, AGNs can be contaminants
  in cosmology. Type 1a supernovae are frequently used as “standard candl
 es” to infer cosmological parameters by estimating both their redshift a
 nd distance modulus to trace cosmic expansion. The Legacy Survey of Space 
 and Time (LSST) will observe millions of supernovae photometrically. Since
  few Type 1as will be spectroscopically confirmed\, other transients can b
 e confused for Type 1as due to low cadence and different sources of uncert
 ainty\, such as instrument noise and model uncertainty. All sources of unc
 ertainty\, including the uncertainty in the label of the source\, must be 
 propagated throughout the model in a fully Bayesian manner to acquire cred
 ible intervals for the inferred cosmological parameters. This is what the 
 package *Cosmographi* aims to do\, while remaining scalable by using JAX. 
 \n\nThis work will present the forward model and fitting modules for AGNs 
 within the *Cosmographi* framework. The user will be able to produce simul
 ated lightcurves orders of magnitude faster compared to pre-existing metho
 ds. Moreover\, it allows for fully Bayesian lightcurve fitting\, and infer
 ence of cosmological parameters from a population with different types of 
 transients. \n\nIn conclusion\, we present advances towards a fully Bayesi
 an estimation of cosmological parameters from millions of supernovae\, and
  population-level studies of AGNs.\n\nhttps://nyx.physics.mcgill.ca/event/
 587/contributions/3716/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3716/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Bulge-driven quenching in KILOGAS: separating classical bulges\, p
 seudobulges and disks with SPADE
DTSTART;VALUE=DATE-TIME:20261028T182100Z
DTEND;VALUE=DATE-TIME:20261028T182200Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3698@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Angelo George (ASIAA)\nBulges are implicated in quen
 ching\, but which bulges\, and how they quench galaxies (gas-driven or eff
 iciency-driven)\, remain open questions. We present SPADE (Spectro-Photome
 tric Analytic Decomposition Engine)\, a new method that fits imaging\, int
 egral-field stellar kinematics and stellar-population spectra of a galaxy 
 simultaneously under one likelihood to separate a bulge from a disk\, and 
 uses the joint evidence to distinguish classical bulges from pseudobulges.
  We apply SPADE to 450 galaxies from KILOGAS\, an ALMA CO(2-1) survey at k
 iloparsec resolution of MaNGA and SAMI galaxies\, assigning every star-for
 ming\, green-valley and quiescent galaxy a bulge type and every spaxel a b
 ulge or disk membership. Combining this with the resolved star-forming mai
 n sequence\, molecular gas main sequence and Kennicutt-Schmidt relation\, 
 we measure how far classical bulge\, pseudobulge and disk regions deviate 
 from these resolved scaling relations as a function of radius. We then dec
 ompose the specific star-formation-rate deficit into a gas-fraction term a
 nd a star-formation-efficiency term. Classical bulges in green-valley gala
 xies fall well below their own disks in star formation\, and most of that 
 deficit is a loss of efficiency rather than of gas\, driven by a growing f
 raction of regions that have stopped forming stars. Pseudobulges show no s
 uch suppression\, and the gas deficit that does exist is concentrated in r
 egions where CO is undetected. These results favour quenching that begins 
 inside classical bulges as a failure to convert gas into stars\, with gas 
 loss following rather than leading.\n\nhttps://nyx.physics.mcgill.ca/event
 /587/contributions/3698/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3698/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Initial Investigations of the Outskirts of XLSSC 122
DTSTART;VALUE=DATE-TIME:20261028T182000Z
DTEND;VALUE=DATE-TIME:20261028T182100Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3677@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Eleanore Todd (University of Victoria)\nWe investiga
 te the redshift 1.98 galaxy cluster XLSSC 122 using the Hubble Space Teles
 cope (HST) from the core of the cluster out to 3 Mpc\, a scale equivalent 
 to 10 times the R500 = 295 kpc radius. We present an expanded photometric 
 and spectroscopic catalogue of the cluster\, bringing the total number of 
 spectroscopically classified member galaxies to 74\, with 35 new member ga
 laxies added in the outer regions of the cluster. We compute the radial ga
 laxy number density profile in the cluster\, and observe no clear evidence
  of infalling groups or cosmic filaments. We observe a clear bimodal colou
 r relation in member galaxies\, with red fraction increasing towards the c
 luster centre. This rapid increase of red fraction upon infall is indicati
 ve of a fast quenching mechanism\, such as ram pressure stripping\, as gal
 axies enter the cluster centre. We fit a luminosity function to the cluste
 r members\, finding a similar low mass slope but fainter scale magnitude t
 han z = 1 clusters of similar temperature\, implying a similar galaxy evol
 ution rate to clusters at lower redshift. These findings indicate that XLS
 SC 122 is experiencing an evolutionary process not typically observed in h
 igh redshift clusters\, and is more similar to z = 0 clusters.\n\nhttps://
 nyx.physics.mcgill.ca/event/587/contributions/3677/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3677/
END:VEVENT
BEGIN:VEVENT
SUMMARY:SMA observations of the archetypal CSS radio source 3C 303.1
DTSTART;VALUE=DATE-TIME:20261028T181900Z
DTEND;VALUE=DATE-TIME:20261028T182000Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3670@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Rushikesh Bhutkar (University of Manitoba)\nAGN (act
 ive galactic nuclei) feedback plays a crucial role in shaping galaxy evolu
 tion. Numerical simulations show that the kinetic energy transfer efficien
 cy from radio jets to interstellar medium (ISM) is relatively high\, sugge
 sting a significant role of radio jets in the feedback. We investigate AGN
  feedback on cold gas in the compact steep-spectrum (CSS) radio source 3C 
 303.1. CSS sources are largely young radio galaxies evolving through dense
  environments of their host galaxies. This early evolutionary phase likely
  represents a critical stage in which the radio source has maximum impact 
 on host galaxy evolution. 3C 303.1 is the only CSS source so far showing a
 lignment in optical\, X-ray and UV with the radio structure\, making it an
  interesting source to investigate jet-feedback. We present continuum and 
 spectral line observations of the J=3-2 transition of carbon monoxide ($^{
 12}$CO) of 3C 303.1\, obtained with the Submillimeter Array. We detect con
 tinuum emission at 221.1 and 271.2~GHz. We do not detect the $^{12}$CO(J=3
 -2) line and derive an upper limit on the molecular gas mass of $\\sim 2.3
  \\times 10^{9}\\ \\mathrm{M_\\odot}$. The gas-to-dust mass (G/D) ratio is
  found to be at the lower end of typical Galactic values\, and the star-fo
 rmation rate (SFR) derived is moderate but declining likely due to a recen
 t  quenching event. Therefore\, $^{12}$CO(J=3-2) non-detection\, relativel
 y low G/D ratio\, and the moderate but declining SFR point to the shock-he
 ating and/or removal of CO gas by AGN\, consistent with the AGN feedback s
 ignatures observed in 3C 303.1.\n\nhttps://nyx.physics.mcgill.ca/event/587
 /contributions/3670/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3670/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Probing the Physical State of Warm Gas in NGC 4696: Infrared Diagn
 ostics for the JWST Era
DTSTART;VALUE=DATE-TIME:20261028T181800Z
DTEND;VALUE=DATE-TIME:20261028T181900Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3687@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Olivia Pereira (Université de Montréal)\nHow do su
 permassive black holes (SMBHs) regulate the growth of the most massive gal
 axies? The cycle of gas cooling and AGN feedback is central to this questi
 on\, yet the physical state of the "warm" multiphase gas often remains elu
 sive. In this talk\, I present JWST/NIRSpec IFU observations of the inner 
 640 pc of NGC 4696\, the prototypical BCG of the Centaurus cluster. These 
 data reveal dozens of atomic and molecular emission lines\, including a ri
 ch set of H₂ rovibrational transitions that trace spatial variations in 
 excitation mechanisms at unprecedented resolution. Using Cloudy simulation
 s\, I develop new infrared diagnostics\, analogous to optical BPT diagrams
 \, optimized for JWST observations.\nThese results provide new insights in
 to the physical state and excitation of warm gas in massive galaxies and d
 emonstrate the broader potential of JWST spectroscopy for probing feedback
 \, cooling\, and star–black hole coupling across different environments.
  This work highlights Canada’s significant role in JWST science and its 
 contribution to advancing infrared galaxy evolution research\, fostering p
 ride in our scientific community.\n\nhttps://nyx.physics.mcgill.ca/event/5
 87/contributions/3687/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3687/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Constraining the Effects of Feedback on Diffuse Gas with Hydrodyna
 mic Simulations
DTSTART;VALUE=DATE-TIME:20261028T181500Z
DTEND;VALUE=DATE-TIME:20261028T181600Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3674@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Skylar Grayson ()\nFeedback from stars and Active Ga
 lactic Nuclei (AGN) plays an important role in galaxy formation\, impactin
 g star formation and gas conditions across a range of physical and tempora
 l scales. Hydrodynamic cosmological simulations rely on feedback to match 
 observations of global properties of galaxies\, but they vary dramatically
  in their treatment of the underlying physical mechanisms. One promising m
 eans of better constraining AGN feedback models is through the circumgalac
 tic medium (CGM). In this talk\, I will begin by exploring how the AGN fee
 dback prescriptions in a range of cosmological simulations shape the CGM. 
 I will assess the observability of these differences by generating mock th
 ermal Sunyaev-Zel’dovich and X-ray observations and comparing them again
 st stacked CGM observations. In the second half of this talk\, I will shar
 e my work using high resolution X-ray spectroscopy from the XRISM telescop
 e to test AGN feedback models at larger mass scales\, exploring the dynami
 cs of the intracluster medium. I will also talk about how XRISM has impact
 ed our understanding of stellar feedback processes\, using observations of
  the starburst galaxy M82 to test longstanding models of supernovae-driven
  winds.\n\nhttps://nyx.physics.mcgill.ca/event/587/contributions/3674/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3674/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Inferring Spatial Distributions of Dark Matter in Dwarf Galaxies w
 ith ML
DTSTART;VALUE=DATE-TIME:20261028T180500Z
DTEND;VALUE=DATE-TIME:20261028T181500Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3656@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Chun On (Andy) Yu (University of Toronto)\nThe spati
 al distribution of dark matter can help us understand the formation and ev
 olution of the structures in our universe. However\, dark matter is invisi
 ble\, so we need to infer its distribution from the motions of visible sta
 rs. Previous techniques struggle to handle incomplete and biased datasets\
 , such as missing velocity information\, and have difficulty incorporating
  measurement uncertainties. To mitigate these limitations\, we develop Neu
 ral Likelihood Estimator (NLE)\, a machine learning framework which models
  the probability of seeing a given set of visible stars given a set of dar
 k matter parameters. By applying Bayes’ theorem\, we can recover the dar
 k matter distribution of the galaxy from visible stars. Our model not only
  performs well on synthetic galaxies\, but it has proven to outperform tra
 ditional methods and modern techniques at recovering the distributions of 
 dark matter from real observational data of the dwarf galaxy Draco. The me
 thod is also highly effective at handling uncertainty and incomplete and b
 iased data.\n\nhttps://nyx.physics.mcgill.ca/event/587/contributions/3656/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3656/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Finding the boundary: Using galaxy membership to inform galaxy clu
 ster extent through machine learning
DTSTART;VALUE=DATE-TIME:20261028T175500Z
DTEND;VALUE=DATE-TIME:20261028T180500Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3665@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Christine Hao (University of Toronto)\nThe spatial e
 xtent of the environment's impact on galaxies marks a transitional region 
 between cluster and field galaxies. We present a data‐driven method to i
 dentify this region in galaxy clusters with masses $M_{200\\rm \,mean}>10^
 {13} {\\rm M}_{\\odot}$ at $z = 0$. Using resolved galaxy samples from the
  largest simulation volume of IllustrisTNG (TNG300-1)\, we examine how gal
 axy properties vary as a function of distance to the closest cluster. We t
 rain neural networks to classify galaxies into cluster and field galaxies 
 based on their intrinsic properties. Using this classifier\, we present th
 e first quantitative and probabilistic map of the transition region. It is
  represented as a broad and intrinsically scattered region near cluster ou
 tskirts\, rather than a sharp physical boundary. This is the physical dete
 ction of a mixed population. In order to determine transition regions of d
 ifferent physical processes by training property-specific models\, we cate
 gorise galaxy properties based on their underlying physics\, i.e. gas\, st
 ellar\, and dynamical. Changes to the dynamical properties dominate the in
 nermost regions of the clusters of all masses. Stellar properties and gas 
 properties\, on the other hand\, exhibit transitions at similar locations 
 for low mass clusters\, yet gas properties have transitions in the outermo
 st regions for high mass clusters. These results have implications for clu
 ster environmental studies in both simulations and observations\, particul
 arly in refining the definition of cluster boundaries while considering en
 vironmental preprocessing and how galaxies evolve under the effect of the 
 cluster environment.\n\nhttps://nyx.physics.mcgill.ca/event/587/contributi
 ons/3665/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3665/
END:VEVENT
BEGIN:VEVENT
SUMMARY:VLA 3 GHz Radio Continuum Mapping of Nearby PHANGS Galaxies: Traci
 ng the Life Cycle of Star Formation
DTSTART;VALUE=DATE-TIME:20261028T174500Z
DTEND;VALUE=DATE-TIME:20261028T175500Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3634@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Hamid Hassani (University of Alberta)\nMassive stars
  strongly reshape their surroundings through radiation\, stellar winds\, a
 nd eventually supernova explosions\, but when these different feedback mec
 hanisms begin to dominate remains uncertain. We present VLA 3 GHz radio co
 ntinuum observations of 13 nearby PHANGS galaxies to trace the evolution o
 f star-forming regions during their first ~10 Myr. Combining these data wi
 th HST\, JWST\, VLT/MUSE\, and AstroSat observations\, we separate the rad
 io emission into thermal free–free and non-thermal synchrotron component
 s and connect their evolution to stellar age and other tracers of recent s
 tar formation. The radio observations also reveal a small population of 36
  embedded\, PAH- and dust-continuum-bright but optically faint star-formin
 g regions\, representing less than 10% of the radio sources and demonstrat
 ing the ability of radio emission to probe the earliest obscured phases of
  star formation. We find a clear evolution in radio properties with stella
 r age: from 1–3 to 6–10 Myr\, the median thermal fraction decreases fr
 om ~61% to ~33%\, while the median radio spectral index steepens from −0
 .05 to −0.51. The youngest regions already exhibit a non-thermal fractio
 n of ~28% before the expected onset of core-collapse supernovae\, suggesti
 ng that massive-star winds and associated shocks may contribute to early c
 osmic-ray acceleration. These results provide a resolved view of how radio
  emission evolves from the embedded phase through the emergence of synchro
 tron emission during the first ~10 Myr of stellar feedback.\n\nhttps://nyx
 .physics.mcgill.ca/event/587/contributions/3634/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3634/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Beyond Diagnostic Diagrams: Spectral Decomposition of Ionizing Sou
 rces in MaNGA
DTSTART;VALUE=DATE-TIME:20261028T173500Z
DTEND;VALUE=DATE-TIME:20261028T174500Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3636@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Aayushmathi Ashok (University of Victoria)\nStar for
 mation rates (SFR) and gas-phase metallicities in galaxies are usually mea
 sured from strong nebular emission lines under the assumption that young m
 assive stars are the only source ionizing the gas. In galaxies hosting an 
 active galactic nucleus (AGN)\, or containing old stellar populations\, ha
 rder radiation also produces these lines\, so the standard approach is to 
 classify each region with emission-line diagnostic diagrams and discard an
 ything not purely star-forming. In the MaNGA integral field spectroscopy s
 urvey\, more than half of the spatially resolved spectra (spaxels) passing
  our quality cuts fall outside the star-forming region. We apply a deep co
 nvolutional neural network that decomposes the full spectrum of each spaxe
 l into a star-forming and a non-star-forming component\, for roughly 740\,
 000 spaxels across 6\,500 galaxies\, and fit each decomposed component for
  both emission lines and continuum.\n\nThe decomposition can be used in tw
 o complementary ways. In star-forming regions\, it acts as a correction by
  removing any residual non-star-forming contamination. We use this techniq
 ue to reconstruct key galaxy scaling relations and find that the correctio
 ns are small. In composite and AGN-dominated regions\, it isolates any und
 erlying star formation. We confirm that H$\\alpha$-based SFR is substantia
 lly overestimated in AGN-classified spaxels\, and find that metallicity co
 rrections depend on the type of ionizing source. We demonstrate that this 
 decomposition can be used to extend classical calibrations to regions that
  are usually discarded in population-level studies\, and to further our un
 derstanding of how AGN activity connects to star formation and chemical en
 richment in galaxies.\n\nhttps://nyx.physics.mcgill.ca/event/587/contribut
 ions/3636/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3636/
END:VEVENT
BEGIN:VEVENT
SUMMARY:How Environment Shapes Quiescent Galaxy Stellar Halo Assembly: Ins
 ights from Extended Light and Color Profiles
DTSTART;VALUE=DATE-TIME:20261028T172500Z
DTEND;VALUE=DATE-TIME:20261028T173500Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3646@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Devin Williams (Saint Mary's University)\nGalaxies d
 o not grow in isolation. Interactions with neighboring galaxies and materi
 al in their surrounding cosmic environments can drive stellar mass assembl
 y and morphological evolution. Galaxy stellar haloes retain signatures of 
 these externally driven processes due to the long dynamical timescales in 
 galaxy outskirts. Observations tracing stellar halo buildup therefore prov
 ide a probe of how merger-driven accretion and environmental processing sh
 ape galaxy assembly over cosmic time. In this talk\, I will present a comb
 ined investigation of stellar halo evolution in quiescent galaxies (QGs) a
 cross cluster and field environments over 0.1 ≤ z ≤ 1.0. Using deep CL
 AUDS+HSC-SSP multiband imaging\, we measure rest-frame g-band light and (U
 −g) color profiles extending to 10Rₑ for ∼90\,000 QGs with log(M★/
 M☉) ≥ 9.66. We isolate environmental effects by comparing the evolutio
 n in median light and color profiles of cluster QGs with those of stellar 
 mass- and redshift-matched field QGs\, tracing both the buildup of stellar
  halo material and the evolution of extended radial color gradients. Our r
 esults indicate that high-mass cluster QGs exhibit enhanced stellar halo g
 rowth fueled by increased accretion. This accretion likely arises from min
 or mergers occurring in cluster outskirts or pre-infall groups\, which dep
 osit bluer stellar populations (younger and/or lower metallicity stars) in
 to the outskirts of higher-mass cluster QGs. In contrast\, low-mass cluste
 r QGs show suppressed stellar halo growth and increased reddening of their
  outskirts relative to the field. These lower-mass QGs likely lose outer s
 tellar halo material through environmental stripping or accretion by high-
 mass galaxies during mergers.\n\nhttps://nyx.physics.mcgill.ca/event/587/c
 ontributions/3646/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3646/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The Influence of Bars on Gas Concentrations and Star Formation in 
 Nearby Galaxies
DTSTART;VALUE=DATE-TIME:20261028T171500Z
DTEND;VALUE=DATE-TIME:20261028T172500Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3664@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Jennifer Laing (McMaster University)\nGalactic bars 
 exist in over half of the galaxies in our local universe\, but studies of 
 the resolved gas properties in the bar have been limited to small samples 
 of star forming spiral galaxies. The ALMA program Kiloparsec Investigation
 s of Local Objects’ Gas And Star-formation (KILOGAS) is a survey of the 
 molecular gas in 450 mass-selected galaxies covering the full parameter sp
 ace of star forming\, quenching\, and quiescent galaxies. At redshifts bet
 ween 0.015 and 0.06\, all galaxies have unprecedented spatial resolution o
 f 1 kpc that are matched with optical field spectroscopy from the MaNGA an
 d SAMI surveys\, allowing for a detailed comparison of the molecular gas w
 ith resolved properties from ionized gas such as stellar mass\, star forma
 tion rates\, and metallicity. I will present results of our analysis using
  radial profiles of molecular gas surface density and star formation rate 
 surface density\, where we have found that galaxies with a strong bar have
  more centrally concentrated molecular gas and star formation. Our finding
 s are broadly consistent with results from Chown et al. (2019) who used a 
 smaller sample of star forming galaxies and found that galaxies with highe
 r molecular gas concentrations and centrally enhanced star formation tend 
 to be barred galaxies. We expect gas concentrations to be higher due to ga
 s inflows along the bar which have been found to suppress star formation e
 fficiency. I will further present results from a full classification of ba
 rred galaxies in the KILOGAS sample using both optical and position-veloci
 ty diagrams.\n\nhttps://nyx.physics.mcgill.ca/event/587/contributions/3664
 /
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3664/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Galaxies in JWST’s mirror may be more massive than they appear: 
 bottom-heavy initial mass functions at z ~ 0.7 from JWST-IMFERNO
DTSTART;VALUE=DATE-TIME:20261028T170500Z
DTEND;VALUE=DATE-TIME:20261028T171500Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3645@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Chloe Cheng (University of Toronto)\nJWST's discover
 y of extremely massive\, quiescent galaxies in the early Universe has intr
 oduced significant tension with current galaxy formation models\, imply
 ing that galaxies formed and quenched faster and earlier than expected. 
  However\, estimates of distant galaxy masses are highly uncertain.  The
 y assume a stellar initial mass function (IMF) similar to that in the Mil
 ky Way\, despite evidence that the cores of massive\, local ellipticals (
 the likely descendants of these massive\, high-redshift galaxies) are ric
 her in low-mass stars (i.e. they have a bottom-heavy IMF).  Until now\, 
 it has been impossible to robustly measure the IMF beyond the low-redshift
  Universe in individual galaxies\, as extremely deep spectra covering both
  optical and near-infrared wavelengths are required.  The JWST-IMFERNO p
 rogram\, which combines deep\, optical spectra from the LEGA-C survey wit
 h extremely deep\, near-infrared\, JWST/NIRSpec-MSA spectra\, has unlocked
  this challenging constraint.  I will present the first robust measureme
 nts of the IMF beyond the local Universe.  Using a sample of 9 massive\,
  quiescent galaxies at z ~ 0.7\, I will demonstrate that distant galaxie
 s have bottom-heavy IMFs compared to the Milky Way\, implying higher stel
 lar masses than previously estimated.  Finally\, I will discuss how our 
 galaxies\, which are direct descendants of JWST’s “impossibly early”
  galaxies\, amplify tensions with galaxy formation models.\n\nhttps://nyx
 .physics.mcgill.ca/event/587/contributions/3645/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3645/
END:VEVENT
BEGIN:VEVENT
SUMMARY:A Systematic Census of Strongly Lensed Population III Galaxy Candi
 dates at z ~ 6–7 from JWST VENUS and MUSE
DTSTART;VALUE=DATE-TIME:20261028T165500Z
DTEND;VALUE=DATE-TIME:20261028T170500Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3654@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Gavin Farley (University of Toronto)\nThe first gene
 ration of stars\, Population III (Pop III)\, likely played a fundamental r
 ole in the formation and evolution of early galaxies. Recent JWST observat
 ions have opened a new window for systematically identifying Pop III signa
 tures at high redshift (z ≈ 3–6)\, during the universe’s first few b
 illion years\, including strong hydrogen emission and weak or absent metal
  lines such as [O III]\, and have revealed a small but growing candidate s
 ample. We conduct a systematic search for extremely metal-poor\, Pop III
 –like galaxies at z ∼ 6–7 using JWST/NIRCam imaging from the VENUS s
 urvey\, the largest lensing-cluster program to date. Combining this data w
 ith deep MUSE spectroscopy\, we search for strongly lensed Pop III candida
 tes whose light is magnified by foreground galaxy clusters. Our search yie
 lds two candidates with spectroscopic redshifts that satisfy our selection
  criteria\, including a highly magnified (μ ∼ 28)\, otherwise inaccessi
 ble\, intrinsically ultra-faint galaxy (M_UV = −15.3) at z = 5.72. This 
 source exhibits strong\, spatially extended Lyα emission\, an extreme Hα
  equivalent width (∼2920 Å)\, a prominent Balmer jump\, and no detectab
 le [O III] in current data—textbook signatures of a young\, metal-poor s
 tellar population consistent with Pop III–like systems. MUSE observation
 s reveal multiple Lyα emitters at the same redshift in the field\, sugges
 ting that the local environment may help sustain such systems even at z = 
 5.7. We present the source-plane properties of these candidates\, their en
 vironments\, and constraints on the number density of Pop III–like galax
 ies at z ∼ 6–7.\n\nhttps://nyx.physics.mcgill.ca/event/587/contributio
 ns/3654/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3654/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Measuring Simulated Circumgalactic Medium Turbulence with Emission
 -Weighted Projected Velocity Structure Functions in FOGGIE
DTSTART;VALUE=DATE-TIME:20261028T164500Z
DTEND;VALUE=DATE-TIME:20261028T165500Z
DTSTAMP;VALUE=DATE-TIME:20261021T144331Z
UID:indico-contribution-49-3652@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Helena Bouchereau ()\nThe spatially-resolved kinemat
 ics of line emission from the circumgalactic medium (CGM) of a galaxy can 
 contain information about the CGM turbulence\, which may play an important
  role in galaxy evolution. Due to the region's diffuse nature\, there have
  been limited observations of low-redshift CGM emission until recent effor
 ts that use spatially-resolved emission line kinematics to probe CGM turbu
 lence. We use velocity structure functions (VSFs) as a measure for the pro
 perties of turbulence using the high-resolution cosmological zoom-in FOGGI
 E simulations. We focus on the location of the "turnover" in the VSF slope
 \, often used as a measurement of the turbulence driving scale\, and study
  how resolution\, measurement area size\, projection effects\, and gas tem
 perature influence the inferred CGM turbulence driving scale. We find that
  projection significantly lowers the VSF normalization but we do not find 
 significant differences in the slope between 3D VSFs and emission-weighted
  projected 2D VSFs. We find that the size of the area used to measure the 
 VSF\, which can be thought of as the size of the emission nebula for a giv
 en instrument sensitivity\, correlates directly with the turnover location
  in the VSF. These dependencies should be considered when using VSFs to in
 terpret CGM turbulence from emission data\, as projection\, resolution and
  sensitivity constraints\, and the temperature of the gas probed will all 
 have a measurable effect on the VSF structure and the corresponding inferr
 ed turbulent properties.\n\nhttps://nyx.physics.mcgill.ca/event/587/contri
 butions/3652/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3652/
END:VEVENT
END:VCALENDAR