A lensing model proto-grid

This directory contains simulated weak lensing maps made from ray tracing through N-body simulations of structure formation, as described in detail in White & Vale (2004; Astroparticle Physics 22(2004)19, astro-ph/0312133).

17 Sep 2004
Data for ~1000 sq. deg. of one cosmological model and 4 source redshift distributions is now available. Contact me for access.
25 May 2004
Better FITS headers added.
20 May 2004
New maps for model 1, with corresponding group catalogues, have been added to the archive. They are in the tar file "grp.001.01.tar".
19 May 2004
The file format for the galaxy catalogs has been changed. The catalogues are now in self-explaining FITS files.

Basic data

The basic data consists of a series of maps for 8 models. All of the files are in fits format and contain arrays of (reduced) shear components or convergences covering a 3x3 degree field of view. The file naming convention is as follows: [base].[model].[map].[src].fits where To simplify downloads and file management, maps have been grouped into tar files.

Auxilliary data

A few sample galaxy catalogues, containing angular and redshift position, convergence and shear for a "realistic" source distribution, are available as the gal.* files. There are 7 entries per galaxy and roughly 1 million galaxies per 3x3 degree field as explained in the FITS headers. These galaxies are meant for testing shot-noise and like projects, they don't model galaxy clustering very well.

For people interested in finding clusters, 3D cluster catalogues for 16 fields for model 1 have been produced. They are available in the grp.* files. The files group2map.??.dat contain the cluster information for each field. Each cluster has 1 row and the columns are x and y pixel position for the most bound particle in the group, M_{200} in Msun/h, comoving distance in Mpc/h, line-of-sight velocity as a distance offset (also in Mpc/h), redshift and FoF group mass.
Beware of array indexing conventions between C/Fortran/IDL etc. You may need to transpose the maps to get correspondance with the files.

Model OmegaM w h n sig8 tau chi^2
1&20.296-1.00.701.000.93 0.15977
3&40.357-0.80.641.000.88 0.15975
5&60.296-1.00.700.950.85 0.10979
7&80.357-0.80.640.950.81 0.10976

Parameters for the models run.
For each cosmological model two independent sets of initial conditions are generated. All models are spatially flat, so Omega_de=1-OmegaM. For all models the matter density is OmegaM.h^2=0.145 and the baryon density OmegaBh^2=0.023. Our results are very insensitive to this latter choice. All models have power-law spectra (no running) with index n and the dark energy has a constant equation of state w. The normalization, sigma_8, is from a fit to the WMAP TT power spectrum data and the chi^2 is for this fit with 893 degrees of freedom.

Index of Data

NameSize (MB)Last modified
born.001.10.tar 642003/11/29
born.002.10.tar 642003/11/29
born.003.10.tar 642003/11/29
born.004.10.tar 642003/11/29
born.005.10.tar 642003/11/29
born.006.10.tar 642003/11/29
born.007.10.tar 642003/11/29
born.008.10.tar 642003/11/29
checksum_24Aug06.dat 02006/08/24
gal.001.01.tar 4232004/05/26
gal.001.21.01.fits 262004/05/26
gal.001.22.01.fits 272004/05/26
gal.001.23.01.fits 262004/05/26
gal.001.24.01.fits 262004/05/26
grp.001.01.tar 1952004/05/25
s.001.01.tar 1922003/12/04
s.001.02.tar 1922003/12/04
s.001.45.tar 1922003/12/04
s.002.01.tar 1922003/12/04
s.002.02.tar 1922003/12/04
s.002.45.tar 1922003/12/04
s.003.01.tar 1922003/12/04
s.003.02.tar 1922003/12/04
s.003.41.tar 1922003/12/04
s.004.01.tar 1922003/12/04
s.004.02.tar 1922003/12/04
s.004.41.tar 1922003/12/04
s.005.01.tar 1922003/12/04
s.005.02.tar 1922003/12/04
s.005.45.tar 1922003/12/04
s.006.01.tar 1922003/12/04
s.006.02.tar 1922003/12/04
s.006.45.tar 1922003/12/04
s.007.01.tar 1922003/12/04
s.007.02.tar 1922003/12/04
s.007.41.tar 1922003/12/04
s.008.01.tar 1922003/12/04
s.008.02.tar 1922003/12/04
s.008.41.tar 1922003/12/04

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Last modified Thu Sep 7 07:35:44 2006