Go to:

-Lightcone outputs
-Images of snapshots
-Lists of Available Data
-References
-Credit

Cluster Catalog descriptions (HTML / text)
Hubble Volume Project in Michigan

Data Visualization (images & movies from Numerical Simulation projects)

VIRGO Members
VIRGO Links
Main U.K. Site
Public Announcement
of the VIRGO data
release

Introduction: The Hubble

The Hubble Volume Project is a joint effort of the Virgo Consortium and collaborators in U.S., Canada, U.K., and Germany. To study the formation of clusters of galaxies, filaments and void-structures, a significant fraction of the entire observable universe is modelled and simulated by employing one billion(=1000000000) mass particles. This is the largest such computer simulation ever done. The 512-processor Garching T3E parallel computer was used for this simulation, which produced almost a Terabyte of output data in some 70 hours.

Lightcone outputs

An important aspect associated with the Hubble Volume Simulations is that data are output along a light-cone so the clustering evolution is incorporated in output data (see the picture below).

A narrow wedge showing the evolution of the clustering:

Get this picture in various color combinations!

Red-Black
White-Emerald
An unsmoothed version of combined two wedges

Deep wedge of LCDM simulation

Credit to all the light-cone pictures: Gus Evrard and Andrzej Kudlicki , ref.1

Images of cluster populations along light-cone

Coming soon!

Images of snapshots

You can download all pictures in original size in gzipped postscript format. (Watch out, they are huge.)

Pic.1A and B:This picture shows projected matter distribution in a slab of 2000 x 2000 x 20 (Mpc/h)³ taken from the snapshot (=particle positions are fixed at an instance) of tauCDM model.

Credit: Colberg and Yoshida, ref.2,3

Pic.2A and B: Here is another representation which gives a much better impression of the clustering. There are some huge voids and superclusters!

Pic2A

Pic2B

Credit: Couchman and Yoshida, ref.2,3

Pic.3A: A thin slice through the full volume. This picture is 12 billion lightyears on a side and is 120 million lightyears thick. It is available as gif files of various sizes:

1024 x 1024, gif format 1.2MB
512 x 512, gif format 0.3MB
1024 x 1024, gzipped PS 1.3MB
512 x 512, gzipped PS 0.36MB

Credit: Joerg Colberg, ref. 4-7

Pic. 3B: A blow-up of a subregion of the above picture. This is roughly 4 billion lightyears on a side and shows a supercluster complex and several large voids which are bigger than any currently known in the real Universe. This picture is available as gif files of various sizes:

1024 x 1024, gif format 1.2MB
512 x 512, gif format 0.3MB
1024 x 1024, gzipped PS 1.0MB
512 x 512, gzipped PS 0.3MB

Credit: Joerg Colberg, ref. 4-7

List of the available data

Go to Cluster Catalogs descriptions

The following data except the cluster catalogues are very large in size and therefore it is practically impossible to download them via internet or ftp. By selecting data types and clicking "GO" you will get information on the data such as number of pieces, size, magnetic tape format and also a detailed description of the data will be shown. Please read the description carefully and send the request as instructed.

Snapshot : By FOF algorithm with linking parameter b=0.2 for tCDM and 0.164 for LCDM, ref 2.

tCDM snapshot z=0.0 (36 MB)
tCDM snapshot z=0.5

LCDM snapshot z=0.0 (42 MB)
LCDM snapshot z=0.5

Lightcone : SO algorithm with density threshold 200, ref 1.
See also DESCRIPTION(HTML/ txt)

Others: Some data available in Michigan, ref1.

Reference

1. Galaxy clusters in Hubble Volume Simulations
   A.E.Evrard, T.MacFarland, H.M.P.Couchman, J.M.Colberg, N.Yoshida, S.D.M. White, A.Jenkins, C.S.Frenk, F.R.Pearce, G. Efstathiou, J.A.Peacock, and P.A.Thomas, 2002, ApJ, 573, 7
2. The mass function of dark matter halos
   A.Jenkins, C.S.Frenk, S.D.M.White, J.M.Colberg, S.Cole, A.E.Evrard, H.M.P.Couchman, and N.Yoshida, 2001, MNRAS, 321, 372
3. Clustering of galaxy clusters in CDM universes
   J.M.Colberg, S.D.M.White, N.Yoshida, T.MacFarland, A.Jenkins, C.S.Frenk, F.R.Pearce, A.E.Evrard, H.M.P.Couchman, G.Efstathiou, J.Peacock, P.Thomas (The Virgo Consortium), 2000, MNRAS, 319, 209
4. Evrard et al, 2000, in preparation
5. The mass function of dark matter halos
   A.Jenkins, C.S.Frenk,S.D.M.White, J.M.Colberg, S.Cole, A.E.Evrard and N.Yoshida, 2000, submitted to MNRAS, preprint astro-ph/0006260
6. Clustering of galaxy clusters in CDM universes
   J.M.Colberg, S.D.M.White, N.Yoshida, T.MacFarland, A.Jenkins, C.S.Frenk, F.R.Pearce, A.E.Evrard, H.Couchman, G.Efstathiou, J.Peacock, P.Thomas (The Virgo Consortium), 2000, submitted to MNRAS, preprint astro-ph/0005259
7. Galaxy Clusters in the Hubble Volume Simulations
   J.M.Colberg, S.D.M.White, T.J.MacFarland, A.Jenkins, C.S.Frenk, F.R.Pearce, A.E.Evrard, H.M.P Couchman, G.Efstathiou, J.A.Peacock, P.A.Thomas, 1998, Proceedings of The 14th IAP Colloquium: Wide Field Surveys in Cosmology, held in Paris, 1998 May 26-30, eds. S.Colombi, Y.Mellier

Credit

Here is an example of proper credit for these Hubble data:

The simulations in this paper were carried out by the Virgo Supercomputing Consortium using computer s based at the Computing Centre of the Max-Planck Society in Garching and at the Edinburgh parallel Computing Centre. The data are publicly available at
http://www.mpa-garching.mpg.de/galform/virgo/hubble

Comments to: Virgo Administrator virgo@mpa-garching.mpg.de