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  • Goicoechea, J.R. (author)

VELOCITY-RESOLVED [C II] EMISSION AND [C II]/FIR MAPPING ALONG ORION WITH HERSCHEL

  • Article/chapterEnglish2015

Publisher, publication year, extent ...

  • 2015
  • electronicrdacarrier

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  • LIBRIS-ID:oai:research.chalmers.se:1731c1c2-0cb7-4aa4-b2a4-53ffdeae8956
  • https://research.chalmers.se/publication/225568URI
  • https://doi.org/10.1088/0004-637X/812/1/75DOI

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  • Language:English
  • Summary in:English

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  • Subject category:art swepub-publicationtype
  • Subject category:ref swepub-contenttype

Notes

  • We present the first ~7.′5 × 11.′5 velocity-resolved (~0.2 km/s) map of the [C II] 158 μm line toward the Orion molecular cloud1 (OMC1) taken with the Herschel/HIFI instrument. In combination with far-IR (FIR) photometric images and velocity-resolved maps of the H41α hydrogen recombination and CO J = 2–1 lines, this data set provides an unprecedented view of the intricate small-scale kinematics of the ionized/photodissociation region (PDR)/molecular gas interfaces and of the radiative feedback from massive stars. The main contribution to the [C II] luminosity (~85%) is from the extended, FUV-illuminated face of the cloud (G0 > 500, nH > 5 × 10^3 cm^−3) and from dense PDRs (G0>~10^4, nH>~10^5 cm^−3) at the interface between OMC 1 and the H II region surrounding the Trapezium cluster. Around ~15% of the [C II] emission arises from a different gas component without a CO counterpart. The [C II] excitation, PDR gas turbulence, line opacity (from [13C II]), and role of the geometry of the illuminating stars with respect to the cloud are investigated. We construct maps of the L[CII]/LFIR and LFIR/MGas ratios and show that L[CII]/LFIR decreases from the extended cloud component (~10^−2–10^−3) to the more opaque star-forming cores (~10^-3-10−4). The lowest values are reminiscent of the “[C II] deficit” seen in local ultraluminous IR galaxies hosting vigorous star formation. Spatial correlation analysis shows that the decreasing L[C II]/LFIR ratio correlates better with the column density of dust through the molecular cloud than with LFIR/MGas. We conclude that the [C II]-emitting column relative to the total dust column along each line of sight is responsible for the observed L[C II]/LFIR variations through the cloud.

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  • Teyssier, D. (author)
  • Etxaluze, M. (author)
  • Goldsmith, P.F. (author)
  • Ossenkopf, V. (author)
  • Gerin, M. (author)
  • Bergin, E.A. (author)
  • Black, John H,1949Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)jblack (author)
  • Cernicharo, J. (author)
  • Cuadrado, S. (author)
  • Encrenaz, P. (author)
  • Falgarone, E. (author)
  • Fuente, A. (author)
  • Hacar, A. (author)
  • Lis, D. (author)
  • Marcelino, N. (author)
  • Melnick, G.J. (author)
  • Müller, H.S.P. (author)
  • Persson, Carina,1964Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)carina64 (author)
  • Pety, J. (author)
  • Röllig, M. (author)
  • Schilke, P. (author)
  • Simon, R. (author)
  • Snell, R.L. (author)
  • Stutzki, J. (author)
  • Chalmers tekniska högskola (creator_code:org_t)

Related titles

  • In:Astrophysical Journal812:1, s. 75-1538-43570004-637X

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