{
  "id": "2108.10519",
  "version": "v1",
  "published": "2021-08-24T04:34:30.000Z",
  "updated": "2021-08-24T04:34:30.000Z",
  "title": "Kinetic temperature of massive star-forming molecular clumps measured with formaldehyde IV. The ALMA view of N113 and N159W in the LMC",
  "authors": [
    "X. D. Tang",
    "C. Henkel",
    "K. M. Menten",
    "Y. Gong",
    "C. -H. R. Chen",
    "D. L. Li",
    "M. -Y. Lee",
    "J. G. Mangum",
    "Y. P. Ao",
    "S. Mühle",
    "S. Aalto",
    "S. García-Burillo",
    "S. Martín",
    "S. Viti",
    "S. Muller",
    "F. Costagliola",
    "H. Asiri",
    "S. A. Levshakov",
    "M. Spaans",
    "J. Ott",
    "C. M. V. Impellizzeri",
    "Y. Fukui",
    "Y. X. He",
    "J. Esimbek",
    "J. J. Zhou",
    "X. W. Zheng",
    "X. Zhao",
    "J. S. Li"
  ],
  "comment": "Accepted for publication in A&A",
  "categories": [
    "astro-ph.GA",
    "astro-ph.SR"
  ],
  "abstract": "We mapped the kinetic temperature structure of two massive star-forming regions, N113 and N159W, in the Large Magellanic Cloud (LMC). We have used $\\sim$1\\hbox{$\\,.\\!\\!^{\\prime\\prime}$}6\\,($\\sim$0.4\\,pc) resolution measurements of the para-H$_2$CO\\,$J_{\\rm K_ aK_c}$\\,=\\,3$_{03}$--2$_{02}$, 3$_{22}$--2$_{21}$, and 3$_{21}$--2$_{20}$ transitions near 218.5\\,GHz to constrain RADEX non-LTE models of the physical conditions. The gas kinetic temperatures derived from the para-H$_2$CO line ratios 3$_{22}$--2$_{21}$/3$_{03}$--2$_{02}$ and 3$_{21}$--2$_{20}$/3$_{03}$--2$_{02}$ range from 28 to 105\\,K in N113 and 29 to 68\\,K in N159W. Distributions of the dense gas traced by para-H$_2$CO agree with those of the 1.3\\,mm dust and \\emph{Spitzer}\\,8.0\\,$\\mu$m emission, but do not significantly correlate with the H$\\alpha$ emission. The high kinetic temperatures ($T_{\\rm kin}$\\,$\\gtrsim$\\,50\\,K) of the dense gas traced by para-H$_2$CO appear to be correlated with the embedded infrared sources inside the clouds and/or YSOs in the N113 and N159W regions. The lower temperatures ($T_{\\rm kin}$\\,$<$\\,50\\,K) are measured at the outskirts of the H$_2$CO-bearing distributions of both N113 and N159W. It seems that the kinetic temperatures of the dense gas traced by para-H$_2$CO are weakly affected by the external sources of the H$\\alpha$ emission. The non-thermal velocity dispersions of para-H$_2$CO are well correlated with the gas kinetic temperatures in the N113 region, implying that the higher kinetic temperature traced by para-H$_2$CO is related to turbulence on a $\\sim$0.4\\,pc scale. The dense gas heating appears to be dominated by internal star formation activity, radiation, and/or turbulence. It seems that the mechanism heating the dense gas of the star-forming regions in the LMC is consistent with that in Galactic massive star-forming regions located in the Galactic plane.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2021-08-24T04:34:30.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "massive star-forming molecular clumps",
      "dense gas",
      "alma view",
      "massive star-forming regions",
      "gas kinetic temperatures"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}