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  • Falgarone, E.Ecole Normale Superieure (ENS) (author)

CH+(1-0) and 13CH+(1-0) absorption lines in the direction of massive star-forming regions

  • Article/chapterEnglish2010

Publisher, publication year, extent ...

  • 2010-10-01
  • EDP Sciences,2010
  • electronicrdacarrier

Numbers

  • LIBRIS-ID:oai:research.chalmers.se:41c7efd6-7e47-48ad-8f23-c42886652fe7
  • https://doi.org/10.1051/0004-6361/201015109DOI
  • https://research.chalmers.se/publication/131852URI

Supplementary language notes

  • Language:English
  • Summary in:English

Part of subdatabase

Classification

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

Notes

  • We report the detection of the ground-state rotational transition of the methylidyne cation CH+ and its isotopologue (CH+)-C-13 toward the remote massive star-forming regions W33A, W49N, and W51 with the HIFI instrument onboard the Herschel satellite. Both lines are seen only in absorption against the dust continuum emission of the star-forming regions. The CH+ absorption is saturated over almost the entire velocity ranges sampled by the lines-of-sight that include gas associated with the star-forming regions (SFR) and Galactic foreground material. The CH+ column densities are inferred from the optically thin components. A lower limit of the isotopic ratio [(CH+)-C-12]/[(CH+)-C-13]> 35.5 is derived from the absorptions of foreground material toward W49N. The column density ratio, N(CH+)/N(HCO+), is found to vary by at least a factor 10, between 4 and > 40, in the Galactic foreground material. Line-of-sight 12CH+ average abundances relative to total hydrogen are estimated. Their average value, N(CH+)/NH > 2.6 x 10(-8), is higher than that observed in the solar neighborhood and confirms the high abundances of CH+ in the Galactic interstellar medium. We compare this result to the predictions of turbulent dissipation regions (TDR) models and find that these high abundances can be reproduced for the inner Galaxy conditions. It is remarkable that the range of predicted N(CH+)/ N(HCO+) ratios, from 1 to similar to 50, is comparable to that observed.

Subject headings and genre

Added entries (persons, corporate bodies, meetings, titles ...)

  • Godard, B.Observatoire de Paris,Paris Observatory (author)
  • Cernicharo, J.CSIC - Instituto de Fisica Fundamental (IFF) (author)
  • de Luca, M.Ecole Normale Superieure (ENS) (author)
  • Gerin, M.Observatoire de Paris,Paris Observatory (author)
  • Phillips, T.G.California Institute of Technology (Caltech) (author)
  • Black, John H,1949Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)jblack (author)
  • Lis, D. (author)
  • Bell, T. A. (author)
  • Boulanger, F.Ecole Normale Superieure (ENS) (author)
  • Coutens, A.Université de Bordeaux,University of Bordeaux (author)
  • Dartois, E.Université Paris-Saclay,University Paris-Saclay (author)
  • Encrenaz, P.Observatoire de Paris,Paris Observatory (author)
  • Giesen, T.Universität Kassel,University of Kassel (author)
  • Goicoechea, J.R.CSIC - Instituto de Fisica Fundamental (IFF) (author)
  • Goldsmith, P.F. (author)
  • Gupta, H.National Science Foundation (author)
  • Gry, C.Laboratoire d'Astrophysique de Marseille (author)
  • Hennebelle, P.Ecole Normale Superieure (ENS) (author)
  • Herbst, E.University of Virginia (author)
  • Hily-Blant, P.Université Grenoble Alpes,Grenoble Alpes University (author)
  • Joblin, C. (author)
  • Kazmierczak, M.Netherlands Institute for Space Research (SRON) (author)
  • Kolos, R.Polish Academy of Sciences (author)
  • Krelowski, J.University of Rzeszów (author)
  • Martin-Pintado, J.Instituto Nacional de Tecnica Aeroespacial (author)
  • Monje, Raquel,1979(Swepub:cth)em1raque (author)
  • Mookerjea, B.Tata Institute of Fundamental Research (author)
  • Neufeld, D.A.Johns Hopkins University (author)
  • Perault, M.Ecole Normale Superieure (ENS) (author)
  • Pearson, J. C. (author)
  • Persson, Carina,1964Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)carina64 (author)
  • Plume, R.University of Calgary (author)
  • Salez, M.Centre national de la recherche scientifique (CNRS) (author)
  • Schmidt, M.Polish Academy of Sciences (author)
  • Sonnentrucker, P.Space Telescope Science Institute (STScI) (author)
  • Stutzki, J.Universität zu Köln,University of Cologne (author)
  • Teyssier, D.European Space Agency (ESA) (author)
  • Vastel, C.Universite Paul Sabatier Toulouse III,Paul Sabatier University (author)
  • Yu, S. (author)
  • Menten, K. M.Max-Planck Institut für Radioastronomie,Max-Planck Institute for Radio Astronomy (author)
  • Geballe, T. R.Gemini Observatory North (author)
  • Schlemmer, S.Universität zu Köln,University of Cologne (author)
  • Shipman, R.Netherlands Institute for Space Research (SRON) (author)
  • Tielens, A.G.G.M.Universiteit Leiden (UL),Leiden University (UL) (author)
  • Philipp, S.Max-Planck Institut für Radioastronomie,Max-Planck Institute for Radio Astronomy (author)
  • Cros, A.Universidad de Guadalajara,University of Guadalajara (author)
  • Zmuidzinas, J.California Institute of Technology (Caltech) (author)
  • Samoska, L.A. (author)
  • Klein, K.University of Arizona (author)
  • Lorenzani, A.Istituto nazionale di astrofisica (INAF) (author)
  • Szczerba, R.Polish Academy of Sciences (author)
  • Peron, I.Institut de Radioastronomie Millimétrique (IRAM) (author)
  • Cais, P.Université de Bordeaux,University of Bordeaux (author)
  • Gaufre, P.Laboratoire d'Astrophysique de Bordeaux (author)
  • Ravera, L.Institut de Recherche en Astrophysique et Planétologie (IRAP) (author)
  • Morris, P.California Institute of Technology (Caltech) (author)
  • Lord, S.California Institute of Technology (Caltech) (author)
  • Planesas, P.Observatorio Astronómico Nacional (OAN),Spanish National Observatory (OAN) (author)
  • Cros, A.Institut de Recherche en Astrophysique et Planétologie (IRAP) (author)
  • Ecole Normale Superieure (ENS)Observatoire de Paris (creator_code:org_t)

Related titles

  • In:Astronomy and Astrophysics: EDP Sciences521:10004-63611432-0746

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