Rationale

 

Understanding the evolution of the interstellar medium (ISM) is essential for comprehending star formation and galaxy evolution. Galaxies are composed primarily of stars and the ISM, and the physical properties of the ISM—such as density, temperature, and kinematics—serve as the initial conditions for star formation, making them fundamental to understanding galactic evolution. The ISM encompasses various physical states, from hydrogen gas (atomic and molecular) to hot plasma and high-energy particles. These states span several orders of magnitude in density (10⁻⁴–10³ cm^-3), temperature (10–1 billions of Kelvins), and spatial scale (parsecs to hundreds of kiloparsecs), each governed by distinct radiative processes and interacting dynamically with one another. Therefore, it is crucial to investigate the multi-phase structure of the ISM across various wavelengths. This includes cold gas, which is the bulk of the ISM mass, diffuse hot plasma, and high-energy processes that dominate volume and energy.
A comprehensive understanding requires a multi-wavelength approach, capturing the ISM's evolution over its wide temperature and density range. However, such multi-faceted studies remain challenging due to the diverse observational techniques and limitations across wavelengths. This symposium invites observational and theoretical researchers interested in the evolution of the ISM through multi-wavelength analyses. It will also explore the prospects of employing next-generation telescopes to advance multi-wavelength studies and aim to foster new collaborations.
 
While the following topics are expected to be central themes, we strongly encourage contributions on any related subjects to foster broad and inclusive discussions.
 
1. Impact of Galaxy Interactions on the ISM and Star Formation (Large-Scale Impact)
      • How do large-scale gas flows triggered by galaxy interactions drive star formation?
      • What are the observable signatures in gases and dust?
      • How do tidal interactions and mergers heat the interstellar gas?
 
2. The Impact of Stellar Feedback on the ISM (Medium-Scale Impact)
      • How does gas heating and ionization occur due to stellar radiation?
      • How do cosmic rays contribute to ISM ionization and heating?
      • What is the impact on subsequent star formation?
 
3. Shock-Cloud Interactions and Cosmic Ray Acceleration (Small-Scale Impact)
      • How do shock-cloud interactions induce turbulence?
      • What gamma-ray signatures originate from high-energy interactions, such as particle acceleration and cosmic-ray interactions with gas?
      • How do shocks contribute to cosmic ray acceleration and impact the surrounding medium?
 
 

Important dates

Abstract submission opens: March 18  (Link to submission page)
Abstract submission deadline: May 11
Registration opens:  April 15 (Link to registration page)
Registration closes on July 25

Confirmed Invited Speakers

Topic 1 – Review (Theory): Florent Renaud (Observatoire Astronomique de Strasbourg / CNRS)
Topic 2 – Review (Theory): Eve Ostriker (Princeton University)
Topic 3 – Review (Theory): Inoue Tsuyoshi (Konan University)
Topic 3 – Review (Observation): Hidetoshi Sano (Gifu University)
 
 
We are in the process of confirming additional invited speakers. Updates will be provided as more speakers are finalized.
 

Accommodation and Host City Information

👉 Click here for accommodation details and local information

Scientific Organizing Committee (SOC)

 

Aya Bamba, The University of Tokyo
Yasuo Fukui, Nagoya University
Kathryn Kreckel, Heidelberg Unviersity
Knox Long, Space Telescope Science  Institute
Martin Pohl, Deutsches Elektronen-Synchrotron DESY
Manami Sasaki, Friedrich-Alexander University Erlangen-Nürnberg
Kengo Tachihara, Nagoya University
Kisetsu Tsuge, Gifu University (SOC/LOC chair)