Hydrodynamic Simulations of Galaxy Clusters
A page discussing the formation of a cluster of galaxies as seen in
different wavebands, along with a QuickTime movie, can be reached
More discussion of clusters, along with numerous links to other
sites, can be found by
This is one of a suite of a simulations of the Ostriker & Steinhardt
concordance model (a LCDM model with matter 30 per cent the critical density).
The box is 134Mpc/h (comoving) on a side with 2243 gas and
2243 dark matter particles. We have 330 full dumps of all of
the particle data, spaced equally in conformal time from z=19 to z=0.
This simulation was originally run for the purpose of studying the
SZ effect (an introduction to the project can be found in
or you can find my talk on this topic, complete with audio,
at the ITP
web site). A movie of structure formation in this model is
For the most massive clusters in the box we have produced maps of
Each map is a projection of a cube 3 virial radii across, centered on the
point of minimum potential in the 3D distribution.
The stretch in each case is logarithmic for the brighter regions, going
over to linear for the lower values to de-emphasize them compared to a
log plot. The only exception is the Kinetic SZ effect which has both
positive and negative regions and so is plotted on a linear scale.
The stretch for all quantities is different as the dynamic range in each
case is different. Each map is a link to the corresponding FITS image.
The gas and dark matter profiles for the
six most massive clusters show that the DM is more concentrated than the
gas and is well fit by an NFW profile down to the resolution of the
simulation (about 25kpc/h comoving in this simulation).
Also scatter plots showing the gas fraction and
the mass-temperature relation for this run and
a run with energy injection have been produced (the other injection runs
are still being processed).
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