Hostname: page-component-54dcc4c588-r5qjk Total loading time: 0 Render date: 2025-09-19T19:11:46.399Z Has data issue: false hasContentIssue false

The Structure and Kinematics of the ISM in Simulated Star-forming Galaxies

Published online by Cambridge University Press:  09 February 2015

Junichi Baba
Affiliation:
Earth-Life Science Institute (ELSI), Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro, Tokyo152–8551 email: babajn@elsi.jp; babajn2000@gmail.com
Kana Morokuma-Matsui
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory of Japan, Minamimaki, Minamisaku, Nagano, 384-1305, Japan
Takayuki R. Saitoh
Affiliation:
Earth-Life Science Institute (ELSI), Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro, Tokyo152–8551 email: babajn@elsi.jp; babajn2000@gmail.com
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We performed 3D N-body/hydrodynamic simulations of local and high-z (z ∼ 2) star-forming galaxies (SFGs) to investigate the structure and kinematic properties of the different ISM phases (i.e., ionized, atomic, and molecular gases). We took into account, for the first time, a fully non-equilibrium radiative cooling by solving the non-equilibrium chemistries of atoms (H, He, C and O) and molecules (H2 and CO), as well as radiative heating, star formation, heating by HII region and supernova explosions.

References

Förster Schreiber, N. M., et al., 2009, ApJ, 706, 1364CrossRefGoogle Scholar
Saitoh, T. R. & Makino, J., 2010, PASJ, 62, 301Google Scholar
Tacconi, L. J., et al., 2010, Nature, 463, 781784Google Scholar