Atomic and molecular gas in disk galaxies

Tony Wong, L. Blitz, A. Kawamura, H. Iritani, Y. Fukui

Research output: Contribution to journalConference articlepeer-review


Current knowledge of the radial distributions of atomic and molecular gas in disk galaxies is briefly reviewed. Almost all of our knowledge is based on observations of the Hi and CO lines at 21 cm and 2.6 mm wavelength, and some of the caveats associated with these methods are discussed. In nearby spiral galaxies the molecular gas fraction is observed to decrease with radius, which can be understood in terms of a decline in hydrostatic disk pressure. Within the LMC, the CO-Hi correlation shows considerable scatter on scales of ∼50 pc, although a binning analysis shows a strong non-linear dependence of CO on Hi intensity. The implications for molecular cloud formation and star formation recipes are briefly discussed.

Original languageEnglish (US)
Pages (from-to)206-211
Number of pages6
JournalAstrophysics and Space Science Proceedings
Issue number202419
StatePublished - 2008
Externally publishedYes
EventSymposium on Mapping the Galaxy and Nearby Galaxies, 2006 - Ishigaki island, Japan
Duration: Jun 26 2006Jun 30 2006

ASJC Scopus subject areas

  • Physics and Astronomy(all)
  • Computer Science Applications
  • Spectroscopy
  • Space and Planetary Science
  • Nuclear and High Energy Physics


Dive into the research topics of 'Atomic and molecular gas in disk galaxies'. Together they form a unique fingerprint.

Cite this