Enriched haloes at redshift z = 2 with no star formation: implications for accretion and wind scenarios†

  1. N. Bouché1,2,3,*,
  2. M. T. Murphy4,
  3. C. Péroux5,
  4. T. Contini2,3,
  5. C. L. Martin1,
  6. N. M. Forster Schreiber6,
  7. R. Genzel6,
  8. D. Lutz6,
  9. S. Gillessen6,
  10. L. Tacconi6,
  11. R. Davies6,
  12. F. Eisenhauer6

Article first published online: 26 SEP 2011

DOI: 10.1111/j.1365-2966.2011.19500.x

Issue

Monthly Notices of the Royal Astronomical Society

Monthly Notices of the Royal Astronomical Society

Volume 419, Issue 1, pages 2–13, January 2012

Additional Information

How to Cite

Bouché, N., Murphy, M. T., Péroux, C., Contini, T., Martin, C. L., Forster Schreiber, N. M., Genzel, R., Lutz, D., Gillessen, S., Tacconi, L., Davies, R. and Eisenhauer, F. (2012), Enriched haloes at redshift z = 2 with no star formation: implications for accretion and wind scenarios. Monthly Notices of the Royal Astronomical Society, 419: 2–13. doi: 10.1111/j.1365-2966.2011.19500.x

Author Information

  1. 1

    Department of Physics, University of California, Santa Barbara, CA 93106, USA

  2. 2

    CNRS, Institut de Recherche en Astrophysique et Planétologie [IRAP] de Toulouse, 14 Avenue E. Belin, F-31400 Toulouse, France

  3. 3

    Université Paul Sabatier de Toulouse, UPS-OMP, IRAP, F-31400 Toulouse, France

  4. 4

    Swinburne University of Technology, Mail H30, PO Box 218, Hawthorn, VIC 3122, Australia

  5. 5

    Observatoire d’Astrophysique de Marseille-Provence, 38 rue Frédéric Joliot-Curie, F-13388 Marseille, France

  6. 6

    Max Planck Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany

* Based on observations made with the European Southern Observatory (ESO) telescopes at Paranal Observatories under programme ID 060.A-9041, 076.A-0527, 079.A-0341, 079.A-0600, 081.A-0568.A, 081.A-0682, 082.A-0580.
E-mail: nbouche@physics.ucsb.edu
Marie Curie Fellow.

Publication History

  1. Issue published online: 13 DEC 2011
  2. Article first published online: 26 SEP 2011
  3. Accepted 2011 July 22. Received 2011 July 21; in original form 2011 January 17

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