{
  "id": "2111.02231",
  "version": "v1",
  "published": "2021-11-03T13:53:22.000Z",
  "updated": "2021-11-03T13:53:22.000Z",
  "title": "ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- V. Hierarchical fragmentation and gas dynamics in IRDC G034.43+00.24",
  "authors": [
    "Hong-Li Liu",
    "Anandmayee Tej",
    "Tie Liu",
    "Namitha Issac",
    "Anindya Saha",
    "Paul F. Goldsmith",
    "Jun-Zhi Wang",
    "Qizhou Zhang",
    "Sheng-Li Qin",
    "Ke Wang",
    "Shanghuo Li",
    "Archana Soam",
    "Lokesh Dewangan",
    "Chang Won Lee",
    "Pak-Shing Li",
    "Xun-Chuan Liu",
    "Yong Zhang",
    "Zhiyuan Ren",
    "Mika Juvela",
    "Leonardo Bronfman",
    "Yue-Fang Wu",
    "Ken'ichi Tatematsu",
    "Xi Chen",
    "Di Li",
    "Amelia Stutz",
    "Siju Zhang",
    "L. Viktor Toth",
    "Qiu-Yi Luo",
    "Feng-Wei Xu",
    "Jinzeng Li",
    "Rong Liu",
    "Jianwen Zhou",
    "Chao Zhang",
    "Mengyao Tang",
    "Chao Zhang",
    "Tapas Baug",
    "E. Mannfors",
    "Eswaraiah Chakali",
    "Somnath Dutta"
  ],
  "comment": "14 pages with 6 figures, and in press",
  "doi": "10.1093/mnras/stab2757",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We present new 3-mm continuum and molecular lines observations from the ATOMS survey towards the massive protostellar clump, MM1, located in the filamentary infrared dark cloud (IRDC), G034.43+00.24 (G34). The lines observed are the tracers of either dense gas (e.g. HCO+/H13CO+ J = 1-0) or outflows (e.g. CS J = 2-1). The most complete picture to date of seven cores in MM1 is revealed by dust continuum emission. These cores are found to be gravitationally bound, with virial parameter, $\\alpha_{vir}<2$. At least four outflows are identified in MM1 with a total outflowing mass of $\\sim 45 M_\\odot$, and a total energy of $\\sim 1\\times 10^{47}$ erg, typical of outflows from a B0-type star. Evidence of hierarchical fragmentation, where turbulence dominates over thermal pressure, is observed at both the cloud and the clump scales. This could be linked to the scale-dependent, dynamical mass inflow/accretion on clump and core scales. We therefore suggest that the G34 cloud could be undergoing a dynamical mass inflow/accretion process linked to the multiscale fragmentation, which leads to the sequential formation of fragments of the initial cloud, clumps, and ultimately dense cores, the sites of star formation.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2021-11-03T13:53:22.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "alma three-millimeter observations",
      "massive star-forming regions",
      "hierarchical fragmentation",
      "gas dynamics",
      "mass inflow/accretion process"
    ],
    "tags": [
      "journal article"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 14,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}