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The Korean Astronomical Society (한국천문학회)
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QUANTIFYING DARK GAS

  • LI, DI (National Astronomical Observatories, Chinese Academy of Sciences) ;
  • XU, DUO (National Astronomical Observatories, Chinese Academy of Sciences) ;
  • HEILES, CARL (Astronomy Department, University of California) ;
  • PAN, ZHICHEN (National Astronomical Observatories, Chinese Academy of Sciences) ;
  • TANG, NINGYU (National Astronomical Observatories, Chinese Academy of Sciences)
  • Received : 2014.11.30
  • Accepted : 2015.06.30
  • Published : 2015.09.30
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Abstract

A growing body of evidence has been supporting the existence of so-called "dark molecular gas" (DMG), which is invisible in the most common tracer of molecular gas, i.e., CO rotational emission. DMG is believed to be the main gas component of the intermediate extinction region from Av~0.05-2, roughly corresponding to the self-shielding threshold of $H_2$ and $^{13}CO$. To quantify DMG relative to $H{\small{I}}$ and CO, we are pursuing three observational techniques; $H{\small{I}}$ self-absorption, OH absorption, and THz $C^+$ emission. In this paper, we focus on preliminary results from a CO and OH absorption survey of DMG candidates. Our analysis shows that the OH excitation temperature is close to that of the Galactic continuum background and that OH is a good DMG tracer co-existing with molecular hydrogen in regions without CO. Through systematic "absorption mapping" by the Square Kilometer Array (SKA) and ALMA, we will have unprecedented, comprehensive knowledge of the ISM components including DMG in terms of their temperature and density, which will impact our understanding of galaxy evolution and star formation profoundly.

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