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Atomic and Molecular Gas in Disk Galaxies

  • Tony Wong
  • Leo Blitz
  • A. Kawamura
  • H. Iritani
  • Y. Fukui
Conference paper
Part of the Astrophysics and Space Science Proceedings book series (ASSSP)

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.

Keywords

Star Formation Molecular Cloud Column Density Spiral Galaxy Disk Galaxy 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer Science+Business Media, LLC 2008

Authors and Affiliations

  • Tony Wong
    • 1
  • Leo Blitz
    • 2
  • A. Kawamura
    • 3
  • H. Iritani
    • 3
  • Y. Fukui
    • 3
  1. 1.CSIRO Australia Telescope National FacilityAustralia
  2. 2.UC Berkeley Astronomy DeptBerkeleyUSA
  3. 3.Department of AstrophysicsNagoya UniversityChikusa-kuJapan

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