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A photometric redshift of z = 6.39 ± 0.12 for GRB 050904

Author

Listed:
  • J. B. Haislip

    (University of North Carolina at Chapel Hill)

  • M. C. Nysewander

    (University of North Carolina at Chapel Hill)

  • D. E. Reichart

    (University of North Carolina at Chapel Hill)

  • A. Levan

    (University of Hertfordshire)

  • N. Tanvir

    (University of Hertfordshire)

  • S. B. Cenko

    (California Institute of Technology)

  • D. B. Fox

    (Pennsylvania State University)

  • P. A. Price

    (University of Hawaii)

  • A. J. Castro-Tirado

    (Instituto de Astrofisica de Andalucia)

  • J. Gorosabel

    (Instituto de Astrofisica de Andalucia)

  • C. R. Evans

    (University of North Carolina at Chapel Hill)

  • E. Figueredo

    (Universidade de Sao Paulo
    Southern Observatory for Astrophysical Research)

  • C. L. MacLeod

    (University of North Carolina at Chapel Hill)

  • J. R. Kirschbrown

    (University of North Carolina at Chapel Hill)

  • M. Jelinek

    (Instituto de Astrofisica de Andalucia)

  • S. Guziy

    (Instituto de Astrofisica de Andalucia)

  • A. de Ugarte Postigo

    (Instituto de Astrofisica de Andalucia)

  • E. S. Cypriano

    (Southern Observatory for Astrophysical Research
    Laboratorio Nacional de Astrofisica)

  • A. LaCluyze

    (University of North Carolina at Chapel Hill)

  • J. Graham

    (University of California)

  • R. Priddey

    (University of Hertfordshire)

  • R. Chapman

    (University of Hertfordshire)

  • J. Rhoads

    (Space Telescope Science Institute)

  • A. S. Fruchter

    (Space Telescope Science Institute)

  • D. Q. Lamb

    (University of Chicago)

  • C. Kouveliotou

    (National Space Science Technology Center)

  • R. A. M. J. Wijers

    (University of Amsterdam and Center for High-Energy Astrophysics)

  • M. B. Bayliss

    (University of North Carolina at Chapel Hill
    University of Chicago)

  • B. P. Schmidt

    (Mount Stromlo and Siding Spring Observatories)

  • A. M. Soderberg

    (California Institute of Technology)

  • S. R. Kulkarni

    (California Institute of Technology)

  • F. A. Harrison

    (California Institute of Technology)

  • D. S. Moon

    (California Institute of Technology)

  • A. Gal-Yam

    (California Institute of Technology)

  • M. M. Kasliwal

    (California Institute of Technology)

  • R. Hudec

    (Academy of Sciences of the Czech Republic)

  • S. Vitek

    (Czech Technical University)

  • P. Kubanek

    (Integral Science Data Center)

  • J. A. Crain

    (University of North Carolina at Chapel Hill)

  • A. C. Foster

    (University of North Carolina at Chapel Hill)

  • J. C. Clemens

    (University of North Carolina at Chapel Hill)

  • J. W. Bartelme

    (University of North Carolina at Chapel Hill)

  • R. Canterna

    (University of Wyoming)

  • D. H. Hartmann

    (Clemson University)

  • A. A. Henden

    (American Association of Variable Star Observers)

  • S. Klose

    (Thueringer Landessternwarte Tautenburg)

  • H.-S. Park

    (Lawrence Livermore National Laboratory)

  • G. G. Williams

    (University of Arizona)

  • E. Rol

    (University of Leicester)

  • P. O'Brien

    (University of Leicester)

  • D. Bersier

    (Liverpool John Moores University)

  • F. Prada

    (Instituto de Astrofisica de Andalucia)

  • S. Pizarro

    (Southern Observatory for Astrophysical Research)

  • D. Maturana

    (Southern Observatory for Astrophysical Research)

  • P. Ugarte

    (Southern Observatory for Astrophysical Research)

  • A. Alvarez

    (Southern Observatory for Astrophysical Research)

  • A. J. M. Fernandez

    (Instituto de Astrofisica de Andalucia)

  • M. J. Jarvis

    (University of Oxford)

  • M. Moles

    (Instituto de Astrofisica de Andalucia)

  • E. Alfaro

    (Instituto de Astrofisica de Andalucia)

  • K. M. Ivarsen

    (University of North Carolina at Chapel Hill)

  • N. D. Kumar

    (University of North Carolina at Chapel Hill)

  • C. E. Mack

    (University of North Carolina at Chapel Hill)

  • C. M. Zdarowicz

    (University of North Carolina at Chapel Hill)

  • N. Gehrels

    (NASA/Goddard Space Flight Center)

  • S. Barthelmy

    (NASA/Goddard Space Flight Center)

  • D. N. Burrows

    (Pennsylvania State University)

Abstract

Long ago and far away The γ-ray burst GRB 050904, detected by the Swift satellite on 4 September last year, is one of the most distant objects ever observed. Its redshift of z = 6.3 equates to an explosion taking place 12.8 billion years ago, when the Universe was a mere 890 million years old. Three groups this week present detailed observations of the γ-ray, X-ray, near-infrared and optical spectra of the afterglow of GRB 050904. The results begin to paint a picture of the conditions prevailing when the parent body exploded and suggest that the γ-ray bursts that we see in the future can be used by cosmologists to probe the early Universe for evidence of star and galaxy formation, nucleosynthesis and reionization.

Suggested Citation

  • J. B. Haislip & M. C. Nysewander & D. E. Reichart & A. Levan & N. Tanvir & S. B. Cenko & D. B. Fox & P. A. Price & A. J. Castro-Tirado & J. Gorosabel & C. R. Evans & E. Figueredo & C. L. MacLeod & J. , 2006. "A photometric redshift of z = 6.39 ± 0.12 for GRB 050904," Nature, Nature, vol. 440(7081), pages 181-183, March.
    • Handle: RePEc:nat:nature:v:440:y:2006:i:7081:d:10.1038_nature04552
    DOI: 10.1038/nature04552
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