Cologne-Bonn Symposium

Poster

Slide

Abstract

Report

Memo

Day 1

• Jacqueline Hodge:
  • distant galaxies have larger gas fractions
  • ALMA flux density strongly correaltes with NIRCam
  • high-z dust strucutre bloadly similar to nearby galaxies
  • high-z galaxies bloadly fit to the KS relation, suggetsing they form stars in the same way of nearby galaxies
• Sylvia Adscheid
  • resolving the infrared backgrounds at the high-z galaxies
  • most of CIB emitted at redshift z ~ 2-4
  • maximum expected stsllar mass for a given gas-to-star conversion efficiency ->because of likely at an increased cosmic star formation efficiency, galaxy evolution models with local SFE cannot explain high-z massive galaxies
• Devismita Panda
  • surveying the complex organic moleculars
  • in SygX-N53, large numbers of fragements are detected
  • in SygX-N30, fragements are line rich and column density consistent with a hot core
• Dominik A. Riechers
  • typical z ~ 6 galaxies too faint for ISM studies, but possible at high M_star end
  • ALMA CII and dust imaging reveals partial einstein ring (G09-83898)
  • there is flat/rising rotation curve -> hints at presence of dark matter, but not much room for DM considering the consistents of mass
  • high z ~ 6 at SFR > 400 M_sun / yr
  • absorbtion of H2O+ -> diffuse atomic outflows
• Francesco Chiti Tegli
  • systematic study of superbubbles using71 nearby main-sequence disk galaxies
  • 651 bubbles with R > 150 pc
  • superbubbles might be more prevalent in galaxies where current star formation rates is higher
  • stellar clusters and associations are inhanced in superbubbles’ cavities and shells
  • superbubbles expand with 5 km/s up to 35 km/s and have dynamical ages below 60 Myr -> they are sitll expanding
• Amelie Saintonge
  • star formation efficiency varies systemaltically across the galaxy
  • about KILOGAS results
  • even after isolating the normal star-forming/gas-rich regions, significant differences remain with global galaxy properties: molecular gas formation and star formation is very sensitive to local enviroment
• Prachi Prajapati
  • determining α_CO factor for high-z
  • median ~ 5.1 but huge range ~ 2-11 from TUNER LVG modeling
  • adopting realistic cold gas sizes may reconcile M_dyn and M_gas, making the need for ~ 0.8 only cositional
• Ralf Klessen
  • direct collapse scenario probably will not work, but collisional pathways are promising
  • if the accretion rate ~ 10^-2 M_sun/yr is keeping, it is easy to make ~ 10^6 M_sun
• Constantina M. Fotopoulou
  • doing gas-rich dwarf marger simulations, ~ 100 GMCs are made by the marger
  • doing stratified galactic disc simulations (SILCC), 10 - 40 GMCs are made
  • in both simulations, most clouds are α_vir > 1, but follow the linewidth-size relation -> bound by external pressure
• Daniel Seifried
  • doing stratified galactic disc simulations (SILCC, same as above)
  • structure of molecular clouds are different: 2D rendering -> clump/filament, 3D rendering -> filaments only, 3D printing -> sheets
  • switch of magnetic field orientation from parallel to perpendicular following the density of gas increasing, it is same both 2D and 3D
• Yuto Komichi
  • doing MHD simulations of conversing flows
  • molecular abundances are determined not only by local physical consitions, but also by quasi-steady-state chemistry
  • CH column density’s linear correlation is reproduced from calculations -> confirmed as a good H2 tracer
• Wajdee Chayeb
  • simualtions of disk show formations of spiral shocks, streaming motions, local instabilities, branches, and spurs
  • the response of gas to spiral stellar potenstial can be non-linear causing non-thermal motions in the gaseous disk
  • the stellar bar and spiral arms are a potential driver of the observed dispersion in HI
• Theodoros Topkaras
  • ζH: ionization rate per H -> H3+ chemistry and varies by enviroment
  • 3D grids will enable detailed parameter space exploration to fit observational data and determine both the ζH and the attenuation coefficient
• Leonard Kaiser
  • magnetic field is coherent on scales of 50 pc
  • coherence is anti-correlated with the star formation rate as a driver of turbulence
• Tejas Oak
  • This study evaluates an enhanced “spectral line deconfusion” method to remove contaminating CO emissions from CII Line Intensity Mapping (LIM) data, which is crucial for observing galaxies during the Epoch of Reionization using the FYST telescope
  • By incorporating ancillary galaxy data, the method robustly recovers the target signal and reduces errors even under high noise conditions
  • The results indicate that this technique is highly effective and, when optimally combined with other methods like targeted masking, will enable the successful detection of CII in upcoming surveys
• Heo He
  • HI velocity dispersion is strongly correlated with HI surface density, suggesting HI disk is in pressure equilibrium with scale height of ~ 1pc
  • HI velocity dispersion has moderate correlation with SFR surface density for inner region

Day 2

• Kei Tanaka
  • accretion disks are robust against radiative feedback (e.g., G45.47+0.05)
  • NaCl and AlO trace the disk (salty disk, e.g., orion source i)
  • basic massive-star formation processes persist at low Z, but chemistry and CO-traced feedback depend on environment
• Kazutaka Kimura
  • using 3d rhd simulation, resarch how protostars and circustellar disk evolve
  • no accretion shock forms at the proto stellar surface and the protostar connect smoothly to a thick disk
  • entropy generated in the disk is effectively carried into the protostar
• Daisei Abe
  • invesitgate the physical mecahnism and evlolution process of HFS
  • in the simulation, massive stars are born in concave region of HFS
  • the merged strucutre cannot be mainteained w/o self-gravity
  • acctually type O scenario may occur in the multi-scale
• Paul Clark
  • high-UV and high cosmic ray ionisation rate in star-bursts may lead to shift towards more high-mass star formation
  • increasing isrf and crir, decreasing amounts but increasing the density of structure
  • in the high UV / CRs cloud, fewer, bigger cores that fragment into more sinks are formed
• Anais Pauchet
  • 3D MHD AMR simulation
  • episodic accretion event onto the central star
  • discs act as a mass reservoir -> reduced and delayed SFE
• Fukui Yasuo
  • observation of RMC 136
  • falling HI cloud of 10^6 Mo, kpc-scale int the LMC, triggering R136 formation
  • the infalling cloud formed a half-cone-shaped boundary layer, magnetically guided filaments focused gas towared the apex, where the densest clump evloved into R136
• Jonathan Mackey
  • explores bow-shock nebulae around massive stars as excellent laboratories for studying shock physics and turbulent mixing
  • By combining a large targeted radio survey (using the VLA) with high-resolution 3D MHD simulations, the study highlights both the potential of these nebulae to reveal interstellar gas dynamics and the significant challenges they pose, such as the need for complex, non-equilibrium ionization modeling
  • The research also notes that winds from red supergiants can help constrain the properties of young massive clusters like Westerlund 1
• Masato Kobayashi
  • almost all SF regions is on the surface of the local bubble
  • by SILCC-Zoom simulations investigate multiple supernovae
  • turbulent motion is enhanced in diffuse volume with Hα but lasts < 0.3 Myr
• Ekaterina Makarenko
  • run FALSH simulations, focus on the thermal X-ray
  • self-consistent radiative cooling allows us to do on-the-fly synthetic thermal X-rays of SNRs
  • the morphology of RCW 103 is defined by SNR interaction with the nearby molecular cloud, ambient magnetic field and turbulence
  • realistic ISM envrioment
• Rob Garrod
  • focuses on astrochemical models of coupled gas and grain chemistry in star-forming regions, specifically regarding the production of complex organic molecules (COMs)
  • COM formation begins much earlier than traditionally thought—even before a protostar forms
  • incorporating “non-diffusive” chemistry and carefully treating desorption processes are critical for building comprehensive models that accurately align with recent JWST and ALMA observations
• Akash Gupta
  • introduces a comprehensive chemical model for High-Mass Star-Forming Regions (HMSFRs) that post-processes Magnetohydrodynamic (MHD) simulations
  • HMSFR chemistry is rarely in equilibrium, making traditional static models insufficient
  • By tracking tracer particles to follow the temporal evolution of density, temperature, and mass transport, the study demonstrates that the initial conditions of molecular clouds heavily influence the final chemical composition, effectively retaining the “chemical memory” of the gas
• Melisse Bonfand
  • introduces a new modeling framework that couples two-dimensional hydrodynamic simulations with gas-grain chemistry to understand the chemical diversity of hot cores in high-mass star-forming regions
  • By utilizing an automated pipeline to generate synthetic observations, researchers can directly compare their models with actual survey data across various physical and chemical conditions
  • aims to constrain factors such as the source’s evolutionary stage, disk inclination, and chemical differentiation, ultimately serving as a tool to help prepare future observational proposals
• Youxin Wang
  • investigates how the lower metallicity and reduced dust-to-gas ratios found in the outer Galaxy impact the formation of complex organic molecules (COMs)
  • By using NOEMA to observe three newly discovered hot cores, found that sensitivity to these conditions varies by molecule; for instance, carbon chains are negatively affected, while CO-related COM abundances are enhanced
  • Ultimately, despite some discrepancies with astrochemical models, the findings confirm that metallicity significantly influences COM formation
• Caroline Gieser
  • IRAS 18089 is a high-mass protostellar object evolving into a hot core
  • investigates the link between ice and gas-phase chemistry in the high-mass hot core IRAS 18089 by combining JWST spectroscopic observations of ice with ALMA (sub)millimeter data for gas-phase molecules
  • while some molecules, such as CH3OH, demonstrate direct inheritance from ice, additional gas-phase reaction routes are likely necessary to explain the abundances of many other species
• Tatiana Rodriguez
  • addresses the challenges of measuring the luminosity of deeply embedded high-mass protostars
  • While Spectral Energy Distribution (SED) fitting is considered ideal, it suffers from observational limitations such as visual extinction and poor angular resolution
  • utilizes molecular line fitting—measuring the rotational temperature at specific radii within a core and applying a modified Stefan-Boltzmann approach—to derive more accurate luminosity estimates using data from the ALMAGAL and TEMPO surveys
• Aurelien Piluso
  • investigates Photodissociation Regions (PDRs) by combining high-resolution spectroscopic observations of H${}_2$ ro-vibrational lines with advanced numerical techniques, including a Bayesian framework
  • successfully constrains the physical conditions of these environments and provides the first robust empirical constraints on the excitation state of newly formed H${}_2$ on dust grains
  • Ultimately, the findings demonstrate that sophisticated modeling can accurately reproduce H${}_2$ emission lines, unlocking deep insights into the complex chemistry and microphysics of PDRs
• Volker Ossenkopf-Okada
  • try PDR modeling to check the CI emission just match the known 13CO lines
  • low observed C18O incompatible with CI and 13CO or with CI and CII -> PDR is invalid
  • warns against blindly trusting standard ${\chi }^2$ fits when comparing chemical models to Photodissociation Region (PDR) observations, noting that even complex networks fail to fully reproduce modern, data-rich observations
  • Instead of merely seeking the best fit, should use data outliers to systematically “debug” these chemical networks
  • gas-phase chemistry is heavily influenced by poorly understood surface reactions, such as those involving solid oxygen, and stresses the urgent need for more laboratory data on desorption processes before drawing conclusions from fit parameters
• Yanhanle Lauryn Zhao
  • investigates Polycyclic Aromatic Hydrocarbon (PAH) emissions as tracers for transition zones in Photodissociation Regions (PDRs) and HII regions
  • By applying a Gaussian Mixture Model to Spitzer photometric data and utilizing SPHEREx spectral data, successfully identified 3.3 μm PAH features
  • certain PAH band ratios increase with the evolutionary stage of molecular clumps, suggesting that evolution primarily affects ionized PAHs rather than neutral ones, which tend to reside in more shielded layers

Day 3

• Peter Schlike
  • high-mass pre-stellar cores may exist (e.g., Hi-GAL), but they do not consititute the dominant mode of high-mass star formation
  • in HFS, star formation already happening in filaments (conveyor belt)
  • from ALMAGAL observation, CMF gets flatter, and total mass core fraction and mass of largest cores grows with L/M (= time)
  • there is a large scatter of core properties that cannot be predicted from clump properties
• Hans Zinnecker
  • outlines the fundamental unsolved problems regarding the formation of massive O-stars (greater than 15-20 solar masses)
  1. Do the majority of massive stars form in dense clusters or in loose associations?
  2. Do the majority of massive stars form in tight (AU-scale) binaries or is there dynamical evolution (orbital shrinking)?
  3. Do more massive clusters (starburst clusters) have a top-heavy IMF? Observational evidence?
  4. Is there an upper mass limit, and if so what does it depend on (theory)?
  5. How do (Orion-like) Trapezium systems form?
  6. What is the fraction of runaway O-stars and/or WR stars? What is their binary nature?
  7. What is the main formation mechanism of massive stars: monolithic collapse followed by disk accretion, competitive accretion, hierarchical accretion, cloud-cloud collisions?
  8. what about the origin of massive stars in the GC nuclear star cluster?
  9. how to estimates the number of O-stars in the MW?
• Anahat Cheema
  • massive star formation is suggeted to be facilitated by mass inflow along the dust lanes
  • G358.69+0.03 have a U-shaped or arc-like structure and HII regions and clumps follow
  • PV diagram show the bridge feature and HII regions are inside it, and there is a widespread shock signature traced by SiO -> observed star formation shaped by large scale CCC between the dust lane inflow
• Birka Zimmermann
  • evaluates the reliability of core mass estimates in high-mass star-forming regions derived from ALMA continuum surveys
  • By generating synthetic ALMA observations from radiation-hydrodynamic simulations, quantifies specific biases: projection effects (overestimating by a factor of 2-3), temperature uncertainties (a factor of 2-5), and interferometric filtering (a factor of 1-2)
  • Combining these dominant uncertainties, conclude that individual ALMA-derived core masses are typically uncertain by a factor of 3 to 5, and potentially up to a factor of 10 in extreme cases
• Emma Bordier
  • presents a comprehensive overview of massive star multiplicity across diverse environments using high-angular-resolution interferometry with the VLTI
  • By comparing young Galactic clusters (like M17) with the extreme, supersolar metallicity environment of the Galactic Center (IRS13 via MATISSE) and the subsolar environments of the LMC and SMC (via GRAVITY+), aims to disentangle the effects of cluster dynamics from intrinsic disk fragmentation, ultimately investigating whether massive star multiplicity is a universal process or shaped by local conditions
• Igor Zinchenko
  • provides a comprehensive analysis of the S255IR high-mass star-forming region, focusing on the 20 $M_{\odot }$ protostar NIRS3
  • the star is forming via episodic disk accretion, evidenced by a 2015 luminosity outburst, an infalling clumpy sub-Keplerian disk, and regular jet ejections—including a recent double ejection with a ~20-degree orientation shift
  • also details the presence of a hypercompact H II region and newly detected Class I and II methanol masers that act as clear tracers for these outburst events
• Shuo Kong
  • the earliest embedded stages of massive star formation are constrained / multiple massive star formation is important
  • highlights high-resolution ALMA observations of the massive protostellar core C1-Sa within the Dragon Infrared Dark Cloud, revealing it to be one of the most distant and youngest binary-forming systems known
  • detail how the core exhibits hierarchical fragmentation, splitting into two kernels (C1-Sa1 and C1-Sa2) separated by 1400 AU with distinct evolutionary states
  • While C1-Sa2 is likely in a cold, starless state with complete chemical depletion, the more evolved C1-Sa1 actively drives two bipolar outflows and may itself host an unresolved close binary
• Lucas Labadie
  • discusses the complex multiplicity of the B-type object GU CMa, revealing it to be a rich dynamical quintuple system rather than just a simple binary
  • Using VLTI/GRAVITY high-angular resolution observations, constrained the highly eccentric orbit ($e\approx 0.98$) of a companion star interacting with the central eclipsing binary
  • kinematic analysis of Br$\gamma$ emissions captured the real-time disruption of the circumstellar disk during a very close periastron encounter, suggesting the central object is likely an evolved fast rotator rather than a typical Herbig star
• Rosie Chen
  • by analysis of SMC, investigate low Z is inefficient cooling, interacting ~ turbulent
  • clouds in SMC have smaller σ -> less turbulent
  • SMC clouds viralized w/o P_ext -> no hinderace on SF
  • single CO line ratio not ∝ actual SF activity
• Anna McLeod
  • discusses the challenge of moving from a qualitative to a quantitative understanding of stellar feedback across different environments and cosmic time, utilizing data from large integral field unit (IFU) surveys of nearby galaxies
  • highlights that future progress requires addressing four major “axes of uncertainty,” specifically the indirect nature of observational diagnostics, unresolved uncertainties in stellar population synthesis models, the difficulty of making direct comparisons between simulations and observations, and the critical question of whether feedback operates fundamentally differently in the extreme physical regimes of the high-redshift early Universe
• Simon Dannhauer
  • the findings of the SOFIA legacy project, FEEDBACK
  • Utilizing CII emission data, the study demonstrates that stellar feedback and molecular cloud formation are deeply interconnected and must be understood together
  • emphasize that expanding bubbles are ubiquitous across regions, and stellar feedback drives rapid cloud dispersal, proving that feedback timescales are actually very short
• Kartik Rajan Neralwar
  • explores the evolution of molecular clouds (MCs) by comparing synthetic observations generated from simulations (STARFORGE) with real observational data
  • highlight a distinct evolutionary path: MCs start as diffuse “cloudlets,” form filamentary structures due to gravity, and are eventually fragmented and dispersed into bubbles by stellar feedback
  • developed a new algorithm to track individual clumps over time and plan to use machine learning to further bridge their synthetic models with actual observations
• Aaron Bryant
  • investigates the “Paradox of Youth” at the Galactic Centre by analyzing the Circumnuclear Disk (CND) using high-resolution SOFIA/FIFI-LS emission line data
  • The resulting PDR analysis reveals that the gas density throughout the CND is far below the Roche tidal limit, implying it is not currently a stable reservoir for in-situ star formation
  • because the Galactic Centre is a highly dynamic and episodic environment, the CND’s exact role remains complex, suggesting that additional gas might still be flowing in from its surroundings
• Sudeep Neupane
  • look into the NGC 6334 filamentary complex
  • CO emission showed the coherent velocity connected strucutres, and many V-shape and bridged structure inside
  • multi-phase carbon emission reveals a clear stratified strcuture from extended CII through intermediate 12CO/CI to dense 13CO filaments
  • dense clumps/filaments found around the bubble rims -> HII regions actively shape the complex
• David Rebolledo
  • provides a comprehensive, multi-phase study of the interstellar medium (molecular, atomic, and ionized gas) in the Carina Nebula Complex using high-resolution observations from ATCA, Mopra, and ALMA
  • despite the strong feedback exerted by massive stellar clusters, the region remains molecular-dominated
  • stellar feedback and turbulence strongly influence cold gas fragmentation, leading to the formation of fewer, but more massive, cores in highly affected areas
• Esan Mouli Ghosh
  • look into W43 region
  • CII traced the arcs extending east and west, prominent cavity in east and west, WR-O stars between the cavity
  • Tension between cluster age ~ 3 Myr and bubble kinamatics age ~ 0.4 Myr -> O stars causing initial expansion and later rejuvenated by WR star

Day 4

• Jarice Lee
  • gas are cleared rapidly in <5 Myr after star formation
  • compact / partially exposed / exposed sequence of Hα around the clusters follow the ages
  • from JWST data, compact 3.3 micron PAH undetected in vast majority of hubble optical clusters older than ~ 3 Myr
  • clusters maybe the clocks to time ISM processes on pc-scales
• Tim-Eric Rathjen
  • introduces the Emission Line Diagnostics (ELD) framework, a powerful tool designed to bridge the gap between high-resolution magnetohydrodynamic simulations and actual observations of H II regions in the interstellar medium
  • By generating synthetic optical emission-line maps, ELD helps identify significant biases in classical optical diagnostics caused by factors like dust attenuation and contamination from diffuse ionized gas
• Oleg Egorov
  • HII regions’ density disribution is not uniform
  • instruct the first ultra wide field IFU instrument
  • enable multiple density, temperature, abundance, kinematics diagnostics for various types of nebulae across MW
• Zein Bazzi
  • analyze PHANGS-JWST to look into the evolution of MC and bubbles
  • apply SCIMES and make the GMC catalog
  • by the destruction by stellar feedback, value of γ in dN/dM ∝ M^γ decrease
  • GMC formed fastly in the central, and later in bars
  • high Σ_SFR region create GMC faster (by feedback?)
  • age of cloud is ~ 1% of depletion time -> star formations is inefficient
• Slawa Kabanovic
  • analyzed 7.7 μm PAH emission data from 75 galaxies in the PHANGS-JWST survey. By applying an automated topological data analysis technique (persistent homology) and machine learning (Self-Organizing Maps), they identified and classified stellar-feedback-driven bubbles entirely without human input or bias.
  • The algorithm successfully detected over 100,000 voids across the 75 galaxies.
  • The bubble “walls” occupy only 20% of the galactic disc area but contribute to 42% of the 7.7 μm emission.
  • The entire population of bubbles universally splits into exactly four shape classes, showing that cavities grow from ~19 pc to ~126 pc before their surrounding enhancement fades and the void refills.
• Lina Gerlach
  • uses high-resolution JWST imaging to study massive star formation in the low-metallicity dwarf galaxies NGC 6822 and Sextans A, which serve as analogs to the early universe
  • created red source lists and performed SED fitting to identify candidate Young Stellar Objects (YSOs)
  • plan to finalize these YSO catalogues, analyze their physical properties, and implement machine learning techniques to automate the identification process for future large-scale surveys
• Thomas Salomon
  • HHe+ is the first molecule formed by radiative association, and by the collisions of them, He2H+ might have been formed in the early universe
  • He2H+ might be detectable through its longer-wavelength bending motion
  • used high-resolution leak-out spectroscopy (pairing a 4 K cryogenic ion trap with a quantum cascade laser) to measure the rovibrational lines of the symmetric linear molecule HHe${}_2^{+}$ near 1300 cm${}^{-1}$
  • recorded seven lines, which showed excellent agreement with highly precise quantum chemical calculations, proving the method’s effectiveness for these cations
• Maria Melamed
  • about the G objects
  • move as compact objects on Keplarian orbits around Sgr A* -> likely have some central mass
  • can be found in the L band, K band, and Br-γ emission -> ongoing accretion
  • high escitation temperatures -> dusty and stellar components
  • candidate YSO;s or binary merger products?
• Miguel Figueria Sebastiao
  • look into the outer galaxy
  • extract GMC by dendrogram and pick up the cluster by SCIMES
  • similar star formation activity inside the arms and inter arms
• Friedrich Wyrowski
  • the results of large-scale (sub)millimeter Milky Way surveys, such as ATLASGAL and SEDIGISM, to study star formation as a multi-scale process from clouds to cores
  • By combining unbiased, high-resolution mapping of molecular clouds and massive clumps with velocity data, these surveys provide a 3D view of the galactic structure, revealing how gas converts into dense, star-forming regions depending on the surrounding galactic environment
  • Gas flows coherently across multiple scales, proving that hierarchical “hub-filament” structures exist continuously from large clouds down to core scales
  • Analysis of the HCN-IR star formation relation revealed a steeper slope than expected, indicating that only a small fraction of HCN emission actually originates from dense, star-forming clumps
• Sarwar Khan
  • The GLOSTAR project conducted a highly sensitive, unbiased radio survey (4-8 GHz) of the Galactic plane using the VLA and Effelsberg telescopes to characterize the early phases of high-mass star formation
  • The survey successfully mapped vital tracers—including compact HII regions, 6.7 GHz methanol masers, formaldehyde, and Radio Recombination Lines (RRLs)—capturing emission across all spatial scales down to a 1.0 arcsecond resolution
  • As a major milestone, the high-resolution images from the VLA D and B configurations are now publicly available to the community
• Han-Tsung Lee
  • from ALMAGAL data extract 419 massive clumps by H2CO line fitting
  • the more L/M increasing, the more thermal energy increasing -> stellar feedback becomes more significant as clumps evolve
  • the more thermal energy increaseing, the more number of cores increasing -> outflow feedback enhances the fragmentation levels
• Jakob den Brok
  • outlines the effort to build a 100pc-scale multi-CO line galaxy sample using ALMA, IRAM, and SMA data to investigate variations in giant molecular cloud properties across local galaxies
  • analyzing multiple CO isotopologue lines and excitation ratios, rather than relying on a single optically thick ${}^{12}$CO line, enables much more robust constraints on underlying physical conditions like temperature and density
  • these molecular gas conditions change systematically in relation to galactic morphology

Day 5

• Giuliana Cosentino
  • massive stars drive feedback throughout their entire lives (outflow, HII region, stellar wind, supernova)
  • feedback has negative and positive effects for further star formations
  • actually ~ 60 % of the molecular cloud found in one of the SEDIGSM fields of view is associated with HII regions
  • feedback mechanism might have triggered the formation of the sun and influenced chemisitry of our planet
• Jia Wei Teh
  • introduces TRINITY, a new theoretical code that efficiently couples major stellar feedback mechanisms—such as winds, radiation, supernovae, and photoionized gas pressure—to simulate the evolution of bubbles in molecular clouds
  • these bubbles act as time-dependent records of stellar feedback
  • there is no single dominant feedback mechanism overall; instead, the most influential process depends heavily on the specific regime, changing dynamically with time, cloud structure, and the surrounding environment
• Matus Rybak
• Rin Yamada
  • it remains unclear how kpc-scale galaxy interactions phenomena drive the physical processes
  • N113 region in the LMC show the 2 primary filament structures
  • clouds hosting high-mass stars are virial or supervirial
• Brandt Gaches
  • orion bar rigion probe excited-state chemistry
  • doing the bar-model 3D simulation and resolving the fronts, the fronts largely overlap, except in voids where the radiation escapes further, making the C+ front a bit deeper
• Kisetsu Tsuge
  • R136 regions in LMC show the characteristic of CCC
  • SMC is metal poor than LMC
  • investigate the dust-to-gas ratio distribution, colliding HI flows are associated with metal-poor gas
  • the colliding HI flows and massive star formation be likely induced by metal-poor gas accreted from the SMC
• Xinyue Liang
  • applies the MULTIGRIS code to the Large Magellanic Cloud (LMC) using optical, CO, and infrared tracers to model its multiphase interstellar medium and constrain key physical parameters of H II regions
  • a global ionizing photon escape fraction ($f_{esc}$) of approximately 4%, notes that most of the molecular gas is CO-dark, and finds that the strongest correlations for $f_{esc}$ involve SII line ratios
  • ISM properties do not significantly depend on the galactocentric radius, though the massive 30 Doradus region notably drives up the local H II gas and dust surface density and ionization parameters while lowering cloud depth
• Jin Koda
  • investigated star-forming and dormant molecular gas across M83 and 12 other nearby galaxies using ALMA CO(1-0) observations and CO line ratio maps
  • molecular clouds and filaments evolve in sync with large-scale galactic structures, coagulating and fragmenting while remaining dense and molecular for long timescales comparable to galactic rotation
  • stellar feedback is highly localized, dormant gas is abundant outside of spiral arms and bars, and crucially, CO(2-1) emission is not a reliable tracer of molecular mass once galactic structures are clearly resolved
• Eleonore Rodrigues da Costa
  • uses ALMA and ATCA observations to investigate stellar feedback in the chemically rich, high-mass star-forming region AG274.0659-1.1488, located in the outer Galaxy
  • By tracing velocity structures with water masers and identifying four distinct outflows, determined that the region hosts an active hot core in an early protostellar stage
  • the exceptional properties of this core-rich source and its surrounding large-scale molecular cloud may be directly linked to an expanding H I shell and cloud-cloud collisions
• Seyma Mercimek
  • by SQUALO observation, molecular outflows are detected across all evolutionary stages (L/M), indicating that active accretion begins early and persists throughout massive star formation
  • outflow velocity show no dependense on clump mass but outflow force increases strongly with clump surface density
  • higher clump infall rates are associated with higher cumulative protostellar accretion rates
  • SQUALO clumps follow the M_acc - L_clump trend seen across independent survey
• Lennart Bohm
  • NH3 line emissions in W33 show the HFS structure and filaments have the velocity gradient
  • filaments have the secondery hubs
  • anisotropic feedback flows to different direction from the filaments and filamnents survive
• Farideh Mazoochi
  • investigates the energy balance and structural formation within a 7 pc radius of the Galactic Center (Sgr A*) by analyzing multi-wavelength data from MeerKAT, ALMA, Herschel, and JCMT
  • By separating the free-free and synchrotron components, found that the non-thermal component dominates the thermal emission at 1.3 GHz, with non-thermal and kinetic energy densities significantly exceeding the thermal energy density
  • computations of the mass-to-magnetic flux ratio classify the Circumnuclear Disk (CND) as a subcritical region, demonstrating that strong magnetic fields (estimated at 445 μG) play a vital role in protecting gas clumps from gravitational collapse
• Golshan Ejali
  • utilizes NIKA2 observations at 1.15 and 2 mm, combined with multi-wavelength data, to conduct a spatially resolved Bayesian SED modeling of the star-forming galaxy NGC 6946 at sub-kpc scales. To accurately interpret the data, the researchers carefully decomposed the millimeter continuum to remove contamination from CO, free-free, and synchrotron emission
  • dust properties are highly environment-dependent and not spatially uniform across the disk. Specifically, the galactic center and spiral arms are warmer, whereas the interarm regions are colder with a steeper effective emissivity slope
  • the NIKA2 data provided critical Rayleigh-Jeans constraints that removed inaccurate solutions permitted by Herschel data alone, ultimately uncovering a strong correlation between dust temperature and star formation rate surface density as direct evidence of stellar feedback
• Wei-An Chen
  • investigates outflow kinematics in high-mass star-forming regions by analyzing nine ALMAGAL clumps using high-resolution ALMA observations, with SiO(5-4) emission acting as the primary outflow tracer
  • identified 76 SiO outflow lobes across these sources and determined that their mass-related properties can be well explained by mass entrainment
  • the outflow force data derived from both CO and SiO suggests an ongoing process of accelerating accretion. The study also highlights a notable anticorrelation between dust polarization and SiO emission—manifesting as “polarization holes”—which indicates a potential reduction in dust grain size caused by the energetic physical processes within the outflows
• Raina Irons
  • introduces a highly adaptable novel technique that uses circular models and kernels to detect radial and circular magnetic field structures in dust polarization maps
  • By applying this method to molecular clouds from the BISTRO survey and known catalogs, located radial magnetic fields and detected known WISE bubbles such as W5 and W7
  • The application to the W5 region in NGC 6334 provided a strong confirmation of the method’s effectiveness, while the analysis also revealed that certain structures, like Cluster 6, are not associated with any currently known bubbles
• Janik Karoly
  • ALMA Band 6 observations of the massive star-forming region IRAS 16562-3959 as part of the MagMaR project to investigate the influence of magnetic fields
  • an incredibly well-ordered yet complex magnetic field across the region, successfully identifying four distinct cores that exhibit pinched, hourglass-like magnetic field structures
  • These structures serve as strong potential indicators of magnetically regulated star formation, a phenomenon rarely observed in such multiplicity within a single region, while other magnetic field lines were found to trace the walls of outflow cavities
• Huixin Zhang
  • investigates the magnetic field properties in the Sagittarius C region using multi-wavelength polarimetric observations from JCMT (850 μm) and SOFIA (214 μm)
  • the 850 μm magnetic field couples to dense gas structures and remains dynamically important, though gravity, turbulence, and magnetic support are ultimately comparable rather than one being universally dominant
  • protostar-associated gas appears more dynamically disturbed by local star formation, and the multi-wavelength polarization data demonstrate that they do not trace a single uniform dust component, pointing instead to a complex, layered dust structure along the line of sight

自分の研究について

• 大質量星形成に必要なガスがコア内で完結するのか外部から来るのかが気になってるのに、最終的な結論をクランプのアソシエーションでとってるのが違和感あるかもしれない、コアってクランプの中にあるものだろうし、スケール感の混同が起こってる？（自分の研究に限らず界隈全体の問題？）
• より議論を深めるためにはやっぱりYSOの正確な質量は欲しいね
• YSOやclumpがないleafについてはどうなの？virializeされてはいるからこれから星ができるのかも…って答えはしたけどほんとか？

その他

• ALMAGALめっちゃおもろそう、論文読みたいし自分の研究にも使えないか

Link

公式サイト

workshop observation analysis d1 project poster slide