{
  "id": "1708.09098",
  "version": "v1",
  "published": "2017-08-30T03:30:24.000Z",
  "updated": "2017-08-30T03:30:24.000Z",
  "title": "Gas kinematics and star formation in the filamentary molecular cloud G47.06+0.26",
  "authors": [
    "Jin-Long Xu",
    "Ye Xu",
    "Chuan-Peng Zhang",
    "Xiao-Lan Liu",
    "Naiping Yu",
    "Chang-Chun Ning",
    "Bing-Gang Ju"
  ],
  "comment": "10 pages, 11 figures, accepted for publication in A&A",
  "categories": [
    "astro-ph.GA",
    "astro-ph.SR"
  ],
  "abstract": "We performed a multi-wavelength study toward the filamentary cloud G47.06+0.26 to investigate the gas kinematics and star formation. We present the 12CO (J=1-0), 13CO (J=1-0) and C18O (J=1-0) observations of G47.06+0.26 obtained with the Purple Mountain Observation (PMO) 13.7 m radio telescope to investigate the detailed kinematics of the filament. The 12CO (J=1-0) and 13CO (J=1-0) emission of G47.06+0.26 appear to show a filamentary structure. The filament extends about 45 arcmin (58.1 pc) along the east-west direction. The mean width is about 6.8 pc, as traced by the 13CO (J=1-0) emission. G47.06+0.26 has a linear mass density of about 361.5 Msun/pc. The external pressure (due to neighboring bubbles and H II regions) may help preventing the filament from dispersing under the effects of turbulence. From the velocity-field map, we discern a velocity gradient perpendicular to G47.06+0.26. From the Bolocam Galactic Plane Survey (BGPS) catalog, we found nine BGPS sources in G47.06+0.26, that appear to these sources have sufficient mass to form massive stars. We obtained that the clump formation efficiency (CFE) is about 18% in the filament. Four infrared bubbles were found to be located in, and adjacent to, G47.06+0.26. Particularly, infrared bubble N98 shows a cometary structure. CO molecular gas adjacent to N98 also shows a very intense emission. H II regions associated with infrared bubbles can inject the energy to surrounding gas. We calculated the kinetic energy, ionization energy, and thermal energy of two H II regions in G47.06+0.26. From the GLIMPSE I catalog, we selected some Class I sources with an age of about 100000 yr, which are clustered along the filament. The feedback from the H II regions may cause the formation of a new generation of stars in filament G47.06+0.26.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2017-08-30T03:30:24.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "filamentary molecular cloud",
      "star formation",
      "gas kinematics",
      "bolocam galactic plane survey",
      "infrared bubble"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 10,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}