{
  "id": "2007.10275",
  "version": "v1",
  "published": "2020-07-20T16:56:29.000Z",
  "updated": "2020-07-20T16:56:29.000Z",
  "title": "FAUST I. The hot corino at the heart of the prototypical Class I protostar L1551 IRS5",
  "authors": [
    "E. Bianchi",
    "C. J. Chandler",
    "C. Ceccarelli",
    "C. Codella",
    "N. Sakai",
    "A. López-Sepulcre",
    "L. T. Maud",
    "G. Moellenbrock",
    "B. Svoboda",
    "Y. Watanabe",
    "T. Sakai",
    "F. Ménard",
    "Y. Aikawa",
    "F. Alves",
    "N. Balucani",
    "M. Bouvier",
    "P. Caselli",
    "E. Caux",
    "S. Charnley",
    "S. Choudhury",
    "M. De Simone",
    "F. Dulieu",
    "A. Durán",
    "L. Evans",
    "C. Favre",
    "D. Fedele",
    "S. Feng",
    "F. Fontani",
    "L. Francis",
    "T. Hama",
    "T. Hanawa",
    "E. Herbst",
    "T. Hirota",
    "M. Imai",
    "A. Isella",
    "I. Jiménez-Serra",
    "D. Johnstone",
    "C. Kahane",
    "B. Lefloch",
    "L. Loinard",
    "M. J. Maureira",
    "S. Mercimek",
    "A. Miotello",
    "S. Mori",
    "R. Nakatani",
    "H. Nomura",
    "Y. Oba",
    "S. Ohashi",
    "Y. Okoda",
    "J. Ospina-Zamudio",
    "Y. Oya",
    "J. Pineda",
    "L. Podio",
    "A. Rimola",
    "D. Segura Cox",
    "Y. Shirley",
    "V. Taquet",
    "L. Testi",
    "C. Vastel",
    "S. Viti",
    "N. Watanabe",
    "A. Witzel",
    "C. Xue",
    "Y. Zhang",
    "B. Zhao",
    "S. Yamamoto"
  ],
  "comment": "6 pages, 2 figures",
  "categories": [
    "astro-ph.SR",
    "astro-ph.GA"
  ],
  "abstract": "The study of hot corinos in Solar-like protostars has been so far mostly limited to the Class 0 phase, hampering our understanding of their origin and evolution. In addition, recent evidence suggests that planet formation starts already during Class I phase, which, therefore, represents a crucial step in the future planetary system chemical composition. Hence, the study of hot corinos in Class I protostars has become of paramount importance. Here we report the discovery of a hot corino towards the prototypical Class I protostar L1551 IRS5, obtained within the ALMA Large Program FAUST. We detected several lines from methanol and its isopotologues ($^{13}$CH$_{\\rm 3}$OH and CH$_{\\rm 2}$DOH), methyl formate and ethanol. Lines are bright toward the north component of the IRS5 binary system, and a possible second hot corino may be associated with the south component. The methanol lines non-LTE analysis constrains the gas temperature ($\\sim$100 K), density ($\\geq$1.5$\\times$10$^{8}$ cm$^{-3}$), and emitting size ($\\sim$10 au in radius). All CH$_{\\rm 3}$OH and $^{13}$CH$_{\\rm 3}$OH lines are optically thick, preventing a reliable measure of the deuteration. The methyl formate and ethanol relative abundances are compatible with those measured in Class 0 hot corinos. Thus, based on the present work, little chemical evolution from Class 0 to I hot corinos occurs.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2020-07-20T16:56:29.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "hot corino",
      "protostar l1551 irs5",
      "prototypical class",
      "methanol lines non-lte analysis constrains",
      "alma large program faust"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 6,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}