The Bulletin of The Korean Astronomical Society (천문학회보)

The Korean Astronomical Society (한국천문학회)
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Characteristic Chemical Correlations in Nearby Star-forming Molecular Clouds

  • Yun, Hyeong-Sik (School of Space Research, Kyung Hee University) ;
  • Lee, Jeong-Eun (School of Space Research, Kyung Hee University) ;
  • Evans, Neal J. II (Korea Astronomy and Space Science Institute) ;
  • Offner, Stella (Department of Astronomy University of Texas, Austin) ;
  • Heyer, Mark H. (Department of Astronomy, University of Massachusetts) ;
  • Choi, Yunhee (Korea Astronomy and Space Science Institute) ;
  • Lee, Yong-Hee (School of Space Research, Kyung Hee University) ;
  • Baek, Giseon (School of Space Research, Kyung Hee University) ;
  • Choi, Minho (Korea Astronomy and Space Science Institute) ;
  • Kang, Hyunwoo (Korea Astronomy and Space Science Institute) ;
  • Tatematsu, Ken'ichi (National Astronomical Observatory of Japan) ;
  • Lee, Seokho (National Astronomical Observatory of Japan) ;
  • Yang, Yao-Lun (RIKEN Cluster for Pioneering Research) ;
  • Gaches, Brandt (Department of Astronomy, University of Massachusetts) ;
  • Chen, How-Huan (Department of Astronomy University of Texas, Austin)
  • Published : 2020.10.13
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Abstract

Different molecular lines trace different physical environments (with various densities and temperatures) within molecular clouds (MCs). Therefore, multimolecular line observations are crucial to study the physical and chemical structures of MCs. We observed the Orion A and Ophiuchus clouds in six different molecular lines as a Taeduk Radio Astronomy Observatory Key Science Program (TRAO-KSP), "mapping Turbulent properties In star-forming MolEcular clouds down to the Sonic scale" (TIMES; PI: Jeong-Eun Lee). Here, we investigate the characteristic relations between the observed lines by performing the Principal Component Analysis (PCA). We also investigate the correlation between the line intensity distributions and the physical parameters, such as the gas column density and dust temperature. Finally, we will discuss how the correlations among different chemical tracers vary with the star formation environments.

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