{
  "id": "1503.05179",
  "version": "v1",
  "published": "2015-03-17T19:41:58.000Z",
  "updated": "2015-03-17T19:41:58.000Z",
  "title": "An Ammonia Spectral Map of the L1495-B218 Filaments in the Taurus Molecular Cloud : I. Physical Pproperties of Filaments and Dense cores",
  "authors": [
    "Young Min Seo",
    "Yancy L. Shirley Paul Goldsmith",
    "Derek Ward-Thompson",
    "Jason M. Kirk",
    "Markus Schmalzl",
    "Jeong-Eun Lee",
    "Rachel Friesen",
    "Glen Langston",
    "Joe Masters",
    "Robert W. Garwood"
  ],
  "comment": "ApJ Accepted",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We present deep NH$_3$ observations of the L1495-B218 filaments in the Taurus molecular cloud covering over a 3 degree angular range using the K-band focal plane array on the 100m Green Bank Telescope. The L1495-B218 filaments form an interconnected, nearby, large complex extending over 8 pc. We observed NH$_3$ (1,1) and (2,2) with a spectral resolution of 0.038 km/s and a spatial resolution of 31$\"$. Most of the ammonia peaks coincide with intensity peaks in dust continuum maps at 350 $\\mu$m and 500 $\\mu$m. We deduced physical properties by fitting a model to the observed spectra. We find gas kinetic temperatures of 8 $-$ 15 K, velocity dispersions of 0.05 $-$ 0.25 km/s, and NH$_3$ column densities of 5$\\times$10$^{12}$ $-$ 1$\\times$10$^{14}$ cm$^{-2}$. The CSAR algorithm, which is a hybrid of seeded-watershed and binary dendrogram algorithms, identifies a total of 55 NH$_3$ structures including 39 leaves and 16 branches. The masses of the NH$_3$ sources range from 0.05 M$_\\odot$ to 9.5 M$_\\odot$. The masses of NH$_3$ leaves are mostly smaller than their corresponding virial mass estimated from their internal and gravitational energies, which suggests these leaves are gravitationally unbound structures. 9 out of 39 NH$_3$ leaves are gravitationally bound and 7 out of 9 gravitationally bound NH$_3$ leaves are associated with star formation. We also found that 12 out of 30 gravitationally unbound leaves are pressure-confined. Our data suggest that a dense core may form as a pressure-confined structure, evolve to a gravitationally bound core, and undergo collapse to form a protostar.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2015-03-17T19:41:58.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "taurus molecular cloud",
      "ammonia spectral map",
      "l1495-b218 filaments",
      "dense core",
      "physical pproperties"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}