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Simulations of the formation, evolution and clustering of galaxies and quasars

Naturevolume 435, pages629–636 (2005)Cite this article

Abstract

The cold dark matter model has become the leading theoretical picture for the formation of structure in the Universe. This model, together with the theory of cosmic inflation, makes a clear prediction for the initial conditions for structure formation and predicts that structures grow hierarchically through gravitational instability. Testing this model requires that the precise measurements delivered by galaxy surveys can be compared to robust and equally precise theoretical calculations. Here we present a simulation of the growth of dark matter structure using 2,1603 particles, following them from redshiftz = 127 to the present in a cube-shaped region 2.230 billion lightyears on a side. In postprocessing, we also follow the formation and evolution of the galaxies and quasars. We show that baryon-induced features in the initial conditions of the Universe are reflected in distorted form in the low-redshift galaxy distribution, an effect that can be used to constrain the nature of dark energy with future generations of observational surveys of galaxies.

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Figure 1:The dark matter density field on various scales.
Figure 2:Differential halo number density as a function of mass and epoch.
Figure 3:Environment of a ‘first quasar candidate’ at high and low redshifts.
Figure 4:Galaxy two-point correlation function,ξ(r), at the present epoch as a function of separationr.
Figure 5:Galaxy clustering as a function of luminosity and colour.
Figure 6:Power spectra of the dark matter and galaxy distributions in the baryon oscillation region.

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Acknowledgements

The computations reported here were performed at the Rechenzentrum der Max-Planck-Gesellschaft in Garching, Germany.

Author information

Authors and Affiliations

  1. Max-Planck-Institute for Astrophysics, Karl-Schwarzschild-Strasse 1, 85740, Garching, Germany

    Volker Springel, Simon D. M. White, Liang Gao & Darren Croton

  2. Institute for Computational Cosmology, Department of Physics, University of Durham, South Road, DH1 3LE, Durham, UK

    Adrian Jenkins, Carlos S. Frenk, John Helly & Shaun Cole

  3. Department of Physics, Nagoya University, Chikusa-ku, Nagoya, 464-8602, Japan

    Naoki Yoshida

  4. Department of Physics & Astronomy, University of Victoria, Victoria, British Columbia, V8P 5C2, Canada

    Julio Navarro

  5. Department of Physics & Astronomy, McMaster University, 1280 Main Street West, Hamilton, Ontario, L8S 4M1, Canada

    Robert Thacker & Hugh Couchman

  6. Institute of Astronomy, University of Edinburgh, Blackford Hill, EH9 3HJ, Edinburgh, UK

    John A. Peacock

  7. Department of Physics & Astronomy, University of Sussex, BN1 9QH, Falmer, Brighton, UK

    Peter Thomas

  8. Department of Physics & Astronomy, University of Michigan, Ann Arbor, Michigan, 48109-1120, USA

    August Evrard

  9. Department of Physics & Astronomy, University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, Pennsylvania, 15260, USA

    Jörg Colberg

  10. Physics and Astronomy Department, University of Nottingham, Nottingham, NG7 2RD, UK

    Frazer Pearce

Authors
  1. Volker Springel
  2. Simon D. M. White
  3. Adrian Jenkins
  4. Carlos S. Frenk
  5. Naoki Yoshida
  6. Liang Gao
  7. Julio Navarro
  8. Robert Thacker
  9. Darren Croton
  10. John Helly
  11. John A. Peacock
  12. Shaun Cole
  13. Peter Thomas
  14. Hugh Couchman
  15. August Evrard
  16. Jörg Colberg
  17. Frazer Pearce

Corresponding author

Correspondence toVolker Springel.

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Competing interests

Reprints and permissions information is available atnpg.nature.com/reprintsandpermissions. The authors declare no competing financial interests.

Supplementary information

Supplementary Methods

This details the physical model used to compute the galaxy population, and gives a short summary of the simulation method. Where appropriate, further references to relevant literature for our methodology are included. (PDF 255 kb)

Supplementary Video

This computer animation visualizes the dark matter distribution of the simulated universe at the present epoch, in a slice of thickness 15 Mpc/h. A zoom over several decades in length-scale onto one of the many rich clusters of galaxies is shown, highlighting the morphology of structure of the universe on different scales as well as the large dynamic range of the millennium simulation. (To play this high-resolution movie on Windows or Apple computers, you may have to install the `divx'-codec, available for free atwww.divx.com). (AVI 11065 kb)

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Springel, V., White, S., Jenkins, A.et al. Simulations of the formation, evolution and clustering of galaxies and quasars.Nature435, 629–636 (2005). https://doi.org/10.1038/nature03597

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Editorial Summary

Evolution of the universe

Computer simulations have been used to blend the giant snapshot of cosmic history provided by modern galaxy surveys into a coherent picture displaying the underlying physical processes of galaxy formation and evolution. The growth of 20 million galaxies in a huge cosmological volume was modelled and it proved possible to identify the unusual formation sites and eventual fate of the first bright quasars. It was shown that large surveys are likely to include features in the galaxy distribution that directly reflect physics in the early Universe and may clarify the nature of the mysterious dark energy driving its current accelerated expansion. The cover shows the distribution of dark matter in a slice of thickness 60 million lightyears through the simulated universe.

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Digitizing the Universe

  • Nickolay Y. Gnedin
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