CO depletion in the Gould Belt clouds

  1. H. Christie1,*,
  2. S. Viti1,
  3. J. Yates1,
  4. J. Hatchell2,
  5. G. A. Fuller3,
  6. A. Duarte-Cabral4,5,
  7. S. Sadavoy6,
  8. J. V. Buckle7,8,
  9. S. Graves7,8,
  10. J. Roberts9,
  11. D. Nutter10,
  12. C. Davis11,
  13. G. J. White12,13,
  14. M. Hogerheijde14,
  15. D. Ward-Thompson10,
  16. H. Butner15,
  17. J. Richer7,8,
  18. J. Di Francesco16

Article first published online: 4 APR 2012

DOI: 10.1111/j.1365-2966.2012.20643.x

Issue

Monthly Notices of the Royal Astronomical Society

Monthly Notices of the Royal Astronomical Society

Volume 422, Issue 2, pages 968–980, May 2012

Additional Information

How to Cite

Christie, H., Viti, S., Yates, J., Hatchell, J., Fuller, G. A., Duarte-Cabral, A., Sadavoy, S., Buckle, J. V., Graves, S., Roberts, J., Nutter, D., Davis, C., White, G. J., Hogerheijde, M., Ward-Thompson, D., Butner, H., Richer, J. and Di Francesco, J. (2012), CO depletion in the Gould Belt clouds. Monthly Notices of the Royal Astronomical Society, 422: 968–980. doi: 10.1111/j.1365-2966.2012.20643.x

Author Information

  1. 1

    Department of Physics and Astronomy, UCL, Gower Street, London WC1E 6BT

  2. 2

    School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL

  3. 3

    Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL

  4. 4

    Univ. Bordeaux, LAB, UMR 5804, F-33270 Floriac, France

  5. 5

    CNRS, LAB, UMR 5804, F-33270 Floriac, France

  6. 6

    Department of Physics and Astronomy, University of Victoria, PO Box 355, STN CSC, Victoria, BC V8W 3P6, Canada

  7. 7

    Astrophysics Group, Cavandish Laboratory, JJ Thomson Avenue, Cambridge CB3 0HE

  8. 8

    Kavli Institute for Cosmology, c/o Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA

  9. 9

    Instituto Nacional de Technica Aeroespacial, 28830 San Fernando de Henares, Spain

  10. 10

    School of Physics and Astronomy, Cardiff University, Queen’s Buildings, The Parade, Cardiff CF24 3AA

  11. 11

    Joint Astronomy Centre, 660 North A’ohoku Place, University Park, Hilo, HI 96720, USA

  12. 12

    Department of Physics and Astronomy, The Open University, Milton Keynes MK7 6AA

  13. 13

    The Rutherford Appleton Laboratory, Space Science and Technology Division, Didcot OX11 0NL

  14. 14

    Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, the Netherlands

  15. 15

    Department of Physics and Astronomy, James Madison University, Harrisonburg, VA 22807, USA

  16. 16

    National Research Council of Canada, Herzberg Institute of Astrophysics, Department of Physics and Astronomy, University of Victoria, Victoria, BC V9E 2E7, Canada

* E-mail: hc@star.ucl.ac.uk

Publication History

  1. Issue published online: 25 APR 2012
  2. Article first published online: 4 APR 2012
  3. Accepted 2012 January 27. Received 2012 January 26; in original form 2011 November 18

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Keywords:

  • molecular data;
  • stars: abundances;
  • stars: formation;
  • ISM: abundances

ABSTRACT

We present a statistical comparison of CO depletion in a set of local molecular clouds within the Gould Belt using Sub-millimetre Common User Bolometer Array (SCUBA) and Heterodyne Array Receiver Programme (HARP) data. This is the most wide-ranging study of depletion thus far within the Gould Belt. We estimate CO column densities assuming local thermodynamic equilibrium and, for a selection of sources, using the radiative transfer code radex in order to compare the two column density estimation methods. High levels of depletion are seen in the centres of several dust cores in all the clouds. We find that in the gas surrounding protostars, levels of depletion are somewhat lower than for starless cores with the exception of a few highly depleted protostellar cores in Serpens and NGC 2024. There is a tentative correlation between core mass and core depletion, particularly in Taurus and Serpens. Taurus has, on average, the highest levels of depletion. Ophiuchus has low average levels of depletion which could perhaps be related to the anomalous dust grain size distribution observed in this cloud. High levels of depletion are often seen around the edges of regions of optical emission (Orion) or in more evolved or less dynamic regions such as the bowl of L1495 in Taurus and the north-western region of Serpens.

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