{
  "id": "2310.14617",
  "version": "v1",
  "published": "2023-10-23T06:51:20.000Z",
  "updated": "2023-10-23T06:51:20.000Z",
  "title": "Early Planet Formation in Embedded Disks (eDisk) XII: Accretion streamers, protoplanetary disk, and outflow in the Class I source Oph IRS63",
  "authors": [
    "Christian Flores",
    "Nagayoshi Ohashi",
    "John J. Tobin",
    "Jes K. Jørgensen",
    "Shigehisa Takakuwa",
    "Zhi-Yun Li",
    "Zhe-Yu Daniel Lin",
    "Merel L. R. van 't Hoff",
    "Adele L. Plunkett",
    "Yoshihide Yamato",
    "Jinshi Sai",
    "Patrick M. Koch",
    "Hsi-Wei Yen",
    "Yuri Aikawa",
    "Yusuke Aso",
    "Itziar de Gregorio-Monsalvo",
    "Miyu Kido",
    "Woojin Kwon",
    "Jeong-Eun Lee",
    "Chang Won Lee",
    "Leslie W. Looney",
    "Alejandro Santamaría-Miranda",
    "Rajeeb Sharma",
    "Travis J. Thieme",
    "Jonathan P. Williams",
    "Ilseung Han",
    "Suchitra Narayanan",
    "Shih-Ping Lai"
  ],
  "comment": "26 pages and 17 figures",
  "categories": [
    "astro-ph.SR",
    "astro-ph.EP",
    "astro-ph.GA"
  ],
  "abstract": "We present ALMA observations of the Class I source Oph IRS63 in the context of the Early Planet Formation in Embedded Disks (eDisk) large program. Our ALMA observations of Oph IRS63 show a myriad of protostellar features, such as a shell-like bipolar outflow (in $^{12}$CO), an extended rotating envelope structure (in $^{13}$CO), a streamer connecting the envelope to the disk (in C$^{18}$O), and several small-scale spiral structures seen towards the edge of the dust continuum (in SO). By analyzing the velocity pattern of $^{13}$CO and C$^{18}$O, we measure a protostellar mass of $\\rm M_\\star = 0.5 \\pm 0.2 $~$\\rm M_\\odot$ and confirm the presence of a disk rotating at almost Keplerian velocity that extends up to $\\sim260$ au. These calculations also show that the gaseous disk is about four times larger than the dust disk, which could indicate dust evolution and radial drift. Furthermore, we model the C$^{18}$O streamer and SO spiral structures as features originating from an infalling rotating structure that continuously feeds the young protostellar disk. We compute an envelope-to-disk mass infall rate of $\\sim 10^{-6}$~$\\rm M_\\odot \\, yr^{-1}$ and compare it to the disk-to-star mass accretion rate of $\\sim 10^{-8}$~$\\rm M_\\odot \\, yr^{-1}$, from which we infer that the protostellar disk is in a mass build-up phase. At the current mass infall rate, we speculate that soon the disk will become too massive to be gravitationally stable.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2023-10-23T06:51:20.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "source oph irs63",
      "early planet formation",
      "embedded disks",
      "protoplanetary disk",
      "accretion streamers"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 26,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}