Search: id:"swepub:oai:research.chalmers.se:1731c1c2-0cb7-4aa4-b2a4-53ffdeae8956" >
VELOCITY-RESOLVED [...
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Goicoechea, J.R.
(author)
VELOCITY-RESOLVED [C II] EMISSION AND [C II]/FIR MAPPING ALONG ORION WITH HERSCHEL
- Article/chapterEnglish2015
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2015
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electronicrdacarrier
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LIBRIS-ID:oai:research.chalmers.se:1731c1c2-0cb7-4aa4-b2a4-53ffdeae8956
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https://research.chalmers.se/publication/225568URI
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https://doi.org/10.1088/0004-637X/812/1/75DOI
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Language:English
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Summary in:English
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Subject category:art swepub-publicationtype
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Subject category:ref swepub-contenttype
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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)
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Etxaluze, M.
(author)
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Goldsmith, P.F.
(author)
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Ossenkopf, V.
(author)
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Gerin, M.
(author)
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Bergin, E.A.
(author)
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Black, John H,1949Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)jblack
(author)
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Cernicharo, J.
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Cuadrado, S.
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Encrenaz, P.
(author)
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Falgarone, E.
(author)
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Fuente, A.
(author)
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Hacar, A.
(author)
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Lis, D.
(author)
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Marcelino, N.
(author)
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Melnick, G.J.
(author)
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Müller, H.S.P.
(author)
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Persson, Carina,1964Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)carina64
(author)
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Pety, J.
(author)
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Röllig, M.
(author)
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Schilke, P.
(author)
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Simon, R.
(author)
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Snell, R.L.
(author)
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Stutzki, J.
(author)
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Chalmers tekniska högskola
(creator_code:org_t)
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In:Astrophysical Journal812:1, s. 75-1538-43570004-637X
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Goicoechea, J.R.
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Teyssier, D.
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Etxaluze, M.
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Goldsmith, P.F.
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Ossenkopf, V.
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Gerin, M.
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Bergin, E.A.
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Black, John H, 1 ...
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Cernicharo, J.
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Cuadrado, S.
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Encrenaz, P.
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Falgarone, E.
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Fuente, A.
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Hacar, A.
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Lis, D.
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Marcelino, N.
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Melnick, G.J.
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Müller, H.S.P.
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Persson, Carina, ...
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Pety, J.
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Röllig, M.
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Schilke, P.
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Simon, R.
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Snell, R.L.
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Stutzki, J.
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- NATURAL SCIENCES
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NATURAL SCIENCES
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Chalmers University of Technology