{
  "id": "2206.08505",
  "version": "v1",
  "published": "2022-06-17T01:51:22.000Z",
  "updated": "2022-06-17T01:51:22.000Z",
  "title": "ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- XI. From inflow to infall in hub-filament systems",
  "authors": [
    "Jian-Wen Zhou",
    "Tie Liu",
    "Neal J. Evans II",
    "Guido Garay",
    "Paul F. Goldsmith",
    "Gilberto C. Gomez",
    "Enrique Vazquez-Semadeni",
    "Hong-Li Liu",
    "Amelia M. Stutz",
    "Ke Wang",
    "Mika Juvela",
    "Jinhua He",
    "Di Li",
    "Leonardo Bronfman",
    "Xunchuan Liu",
    "Feng-Wei Xu",
    "Anandmayee Tej",
    "L. K. Dewangan",
    "Shanghuo Li",
    "Siju Zhang",
    "Chao Zhang",
    "Zhiyuan Ren",
    "Kenichi Tatematsu",
    "Pak Shing Li",
    "Chang Won Lee",
    "Tapas Baug",
    "Sheng-Li Qin",
    "Yuefang Wu",
    "Yaping Peng",
    "Yong Zhang",
    "Rong Liu",
    "Qiu-Yi Luo",
    "Jixing Ge",
    "Anindya Saha",
    "Eswaraiah Chakali",
    "Qizhou zhang",
    "Kee-Tae Kim",
    "Isabelle Ristorcelli",
    "Zhi-Qiang Shen",
    "Jin-Zeng Li"
  ],
  "comment": "16 pages",
  "categories": [
    "astro-ph.GA",
    "astro-ph.SR"
  ],
  "abstract": "We investigate the presence of hub-filament systems in a large sample of 146 active proto-clusters, using H$^{13}$CO$^{+}$ J=1-0 molecular line data obtained from the ATOMS survey. We find that filaments are ubiquitous in proto-clusters, and hub-filament systems are very common from dense core scales ($\\sim$0.1 pc) to clump/cloud scales ($\\sim$1-10 pc). The proportion of proto-clusters containing hub-filament systems decreases with increasing dust temperature ($T_d$) and luminosity-to-mass ratios ($L/M$) of clumps, indicating that stellar feedback from H{\\sc ii} regions gradually destroys the hub-filament systems as proto-clusters evolve. Clear velocity gradients are seen along the longest filaments with a mean velocity gradient of 8.71 km s$^{-1}$pc$^{-1}$ and a median velocity gradient of 5.54 km s$^{-1}$pc$^{-1}$. We find that velocity gradients are small for filament lengths larger than $\\sim$1~pc, probably hinting at the existence of inertial inflows, although we cannot determine whether the latter are driven by large-scale turbulence or large-scale gravitational contraction. In contrast, velocity gradients below $\\sim$1~pc dramatically increase as filament lengths decrease, indicating that the gravity of the hubs or cores starts to dominate gas infall at small scales. We suggest that self-similar hub-filament systems and filamentary accretion at all scales may play a key role in high-mass star formation.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2022-06-17T01:51:22.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "alma three-millimeter observations",
      "massive star-forming regions",
      "velocity gradient",
      "containing hub-filament systems decreases",
      "filament lengths"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 16,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}