Letter | Published:

The Laniakea supercluster of galaxies

Nature volume 513, pages 7173 (04 September 2014) | Download Citation



Galaxies congregate in clusters and along filaments, and are missing from large regions referred to as voids. These structures are seen in maps derived from spectroscopic surveys1,2 that reveal networks of structure that are interconnected with no clear boundaries. Extended regions with a high concentration of galaxies are called ‘superclusters’, although this term is not precise. There is, however, another way to analyse the structure. If the distance to each galaxy from Earth is directly measured, then the peculiar velocity can be derived from the subtraction of the mean cosmic expansion, the product of distance times the Hubble constant, from observed velocity. The peculiar velocity is the line-of-sight departure from the cosmic expansion and arises from gravitational perturbations; a map of peculiar velocities can be translated into a map of the distribution of matter3. Here we report a map of structure made using a catalogue of peculiar velocities. We find locations where peculiar velocity flows diverge, as water does at watershed divides, and we trace the surface of divergent points that surrounds us. Within the volume enclosed by this surface, the motions of galaxies are inward after removal of the mean cosmic expansion and long range flows. We define a supercluster to be the volume within such a surface, and so we are defining the extent of our home supercluster, which we call Laniakea.

Access optionsAccess options

Rent or Buy article

Get time limited or full article access on ReadCube.


All prices are NET prices.


  1. 1.

    , & A slice of the universe. Astrophys. J. 302, L1–L5 (1986)

  2. 2.

    et al. A map of the universe. Astrophys. J. 624, 463–484 (2005)

  3. 3.

    et al. Cosmography of the local universe. Astron. J. 146, 69 (2013)

  4. 4.

    et al. A redshift survey of IRAS galaxies. IV — The galaxy distribution and the inferred density field. Astrophys. J. 385, 421–444 (1992)

  5. 5.

    et al. IRAS galaxies versus POTENT mass: density fields, biasing, and omega. Astrophys. J. 412, 1–21 (1993)

  6. 6.

    et al. Cosmic structure and dynamics of the local Universe. Mon. Not. R. Astron. Soc. 427, L35–L39 (2012)

  7. 7.

    et al. Three-dimensional velocity and density reconstructions of the local universe with Cosmicflows-1. Astrophys. J. 744, 43 (2012)

  8. 8.

    et al. Wiener reconstruction of the large-scale structure. Astrophys. J. 449, 446–459 (1995)

  9. 9.

    , & Wiener reconstruction of large-scale structure from peculiar velocities. Astrophys. J. 520, 413–425 (1999)

  10. 10.

    et al. Reconstructing cosmological initial conditions from galaxy peculiar velocities — II. The effect of observational errors. Mon. Not. R. Astron. Soc. 430, 902–911 (2013)

  11. 11.

    et al. The cosmic microwave background spectrum from the full COBE FIRAS data set. Astrophys. J. 473, 576–587 (1996)

  12. 12.

    The distribution of galaxies in the direction of the ‘Great Attractor’. Nature 342, 251–255 (1989)

  13. 13.

    et al. The large-scale tidal velocity field. Preprint at (2001)

  14. 14.

    et al. A kinematic classification of the cosmic web. Mon. Not. R. Astron. Soc. 425, 2049–2057 (2012)

  15. 15.

    & in Large-Scale Motions in the Universe: A Vatican Study Week (eds & ) 31–70 (Princeton Univ. Press, 1988)

  16. 16.

    et al. POTENT reconstruction from mark III velocities. Astrophys. J. 522, 1–38 (1999)

  17. 17.

    et al. Spectroscopy and photometry of elliptical galaxies — a large-scale streaming motion in the local universe. Astrophys. J. 313, L37–L42 (1987)

  18. 18.

    Evidence for a local supergalaxy. Astron. J. 58, 30–32 (1953)

  19. 19.

    et al. Cosmicflows-2: the data. Astron. J. 146, 86 (2013)

  20. 20.

    , & The mid-infrared Tully-Fisher relation: calibration of the type Ia supernova scale and H0. Astrophys. J. 758, L12 (2012)

  21. 21.

    Planck Collaboration. et al. Planck intermediate results. XVI. Profile likelihoods for cosmological parameters. Available at (2013)

  22. 22.

    et al. A 3% solution: determination of the Hubble constant with the Hubble Space Telescope and Wide Field Camera 3. Astrophys. J. 730, 119 (2011)

  23. 23.

    et al. Carnegie Hubble Program: a mid-infrared calibration of the Hubble constant. Astrophys. J. 758, 24 (2012)

  24. 24.

    et al. Three-dimensional velocity and density reconstructions of the local universe with Cosmicflows-1. Astrophys. J. 744, 43 (2012)

  25. 25.

    , & Wiener reconstruction of large-scale structure from peculiar velocities. Astrophys. J. 520, 413–425 (1999)

  26. 26.

    & The density and peculiar velocity fields of nearby galaxies. Phys. Rep. 261, 271–431 (1995)

  27. 27.

    et al. Wiener reconstruction of the large-scale structure. Astrophys. J. 449, 446–459 (1995)

  28. 28.

    et al. Interactive visualization of astrophysical plasma simulations with SD-vision. Astron. Soc. Pacif. Conf. Ser. 385, 327 (2008)

  29. 29.

    et al. 2MASS Extended Source Catalog: overview and algorithms. Astron. J. 119, 2498–2531 (2000)

Download references


We thank our many collaborators in the accumulation of Cosmicflows-2 distances. We thank the CLUES collaboration, and in particular S. Gottlöber and J. Sorce in connection with the analysis. T. Jarrett provided an unpublished 2MASS Extended Source Catalog redshift compendium, the only all-sky redshift catalogue extensive enough to match the region of our reconstruction. The narration in the Supplementary Video is by S. Anvar and the original music is played by N.-E. Pomarède. The name ‘Laniakea’ was suggested by N. Napoleon, Kapiolani Community College, Hawaii. Financial support was provided by US National Science Foundation award AST09-08846, several awards through the Space Telescope Science Institute for observing time with Hubble Space Telescope, an award from the Jet Propulsion Lab for observations with Spitzer Space Telescope, and NASA award NNX12AE70G for analysis of data from the Wide-field Infrared Survey Explorer. We also acknowledge support from the Israel Science Foundation (1013/12) and the Lyon Institute of Origins under grant ANR-10-LABX-66 and the CNRS under PICS-06233.

Author information


  1. Institute for Astronomy, University of Hawaii, Honolulu, Hawaii 96822, USA

    • R. Brent Tully
  2. Université Claude Bernard Lyon I, Institut de Physique Nucléaire, Université Lyon I, CNRS/IN2P3, Lyon 69622, France

    • Hélène Courtois
  3. Racah Institute of Physics, Hebrew University, Jerusalem 91904, Israel

    • Yehuda Hoffman
  4. Institut de Recherche sur les Lois Fondamentales de l’Univers, CEA/Saclay, 91191 Gif-sur-Yvette, France

    • Daniel Pomarède


  1. Search for R. Brent Tully in:

  2. Search for Hélène Courtois in:

  3. Search for Yehuda Hoffman in:

  4. Search for Daniel Pomarède in:


R.B.T. guided the project, was involved in the data acquisition, interacted closely in the development of the ideas that are presented here, and wrote most of the Letter. H.C. was involved in the observing programme, was instrumental in coordinating activities, and was involved in all facets. Y.H. took responsibility for the theoretical analysis, including the Wiener filter, the cosmic web and the Malmquist bias correction. D.P. developed and applied visualization tools useful to this research.

Competing interests

The authors declare no competing financial interests.

Corresponding author

Correspondence to R. Brent Tully.

Extended data

Supplementary information

PDF files

  1. 1.

    Supplementary Information

    This file contains the transcript for Supplementary Video 1.


  1. 1.

    Laniakea Supercluster of Galaxies

    By steps, the video illustrates the observed local distribution of galaxies, the observed departures from the expansion of the universe of the fraction of the galaxies with distance measurements, the inferred three-dimensional flow pattern of the local galaxies, and the inferred underlying distribution of matter causing these flows. Flows are differentiated between motions inward toward a local basin of attraction and flows outward toward external attractors. A boundary is located between inward and outward flows. We call the contiguous region of the inward flow pattern the Laniakea Supercluster of galaxies, our home supercluster. For a high resolution version of this video please follow this link http://irfu.cea.fr/laniakea or http://vimeo.com/pomarede/laniakea.

About this article

Publication history






Further reading


By submitting a comment you agree to abide by our Terms and Community Guidelines. If you find something abusive or that does not comply with our terms or guidelines please flag it as inappropriate.