HIGH RESOLUTION  SPH   SIMULATION OF 

 ΛCDM  GALAXY CLUSTERS

G. Yepes, Y. Ascasibar, S Gottloeber and V. Muller  2002


SIMULATION    PARAMETERS.

Ω Λ=0.7, ΩΜ=0.3; Ωbar=0.02/h2 , h=0.7

Simulated Box Lenght= 80 h-1 Mpc

Multi-mass refinement initial conditions: 3 levels of mass refinement

evolutuon of slice

SPH particle mass: =  4×107 h-1 Msun

Number of  SPH  particles  1.19x106

Total number of particles:  4.5×106 


Gravitational smoothing in refined area:   2 /h kpc


Properties of the simulated cluster at z=0

Virial Radius (at overdensity 340  background matter density) =  1.24 /h Mpc
Virial Mass = 2.2x1014 /h Msun






VIDEOS





Time Evolution of 3D gas and dark matter density in an 8/h Mpc box  
centred at the cluster center of mass at z=0


DARK MATTER  
(640x480 AVI Movie 7 Mbytes)
dark matter
density

GAS DENSITY  
(640x480 AVI Movie 7 Mbytes)
gas density








Combined  movie (5 Mbytes AVI  file)
gas and dark matter density

                         

DISK FORMATION IN A CLUSTER SIMULATION.


Same cluster simulation as above, but this time we have included radiative and compton cooling together with
UV phoionization from  QSO background. The UV flux  has a redshift dependence   according to  Haart and Madau  (1998)
This video shows one dark matter halo at z=3 which has developed a tiny disk of gas. The boxsize  shown is 1/h  comoving Mpc
and it is zoomed in  until the box is 30 /h kpc.  Particles are ploted according to gas density.



 ANIMATED GIF FILE: 12 Mbytes                     AVI FILE WITH DIVX compression (9Mbytes)

halo with disk              zooming the disk




CLUSTER MERGER  SIMULATION:

Merging of clusters is one the most energetic processes  in the Universe, after the Big Bang itself.
Here we show  some animations of  the formation of  the second most massive cluster in  our simulations.


GAS DENSITY  EVOLUTION (8/h Mpc comoving box)
(640x480  DIVX AVI Movie 3 Mbytes)  

Gas distribution of Clsuter 2   




DETAILED  STUDY OF A CLUSTER MERGER AT z=0.5  from two progenitors of Mass 1013 Msun
and relative velocity of 3000 Km/s.

This simulation has been used to   test the hipothesis of  formation of radio relics during cluster merging
See Hoeft, Brugger and Yepes  2003, (astro-ph/0302185)

These animations were done by Matthias Hoeft





2D SLICES  cut through the center of a cluster merger


GAS DENSITY  
DIVX  AVI Movie 350 Kbytes)

gas evolution of  cluster merger 


TEMPERATURE EVOLUTION
DIVX  AVI Movie 400  Kbytes)

temperature evolution through cluster erger

   



Another interesting application of  cluster merger simulations...


A music  Video clip  made  by  MIG productions 

(Require  Realplayer )


mig video