2012-13 "Minnesota" Project (work in progress)
                     Vazza - Jones - Gheller - Bruggen - Ryu - et al..


Resimulation of galaxy clusters with Nested Initial conditions & fixed refinement.

W
e will study the onset and evolution of shocks and turbulent motions with a uniform high resolution and high
time sampling for a statistical set of moderate (10^14 Msol) galaxy clusters in the LCDM Universe.


 

We used the public version of ENZO.2.1 (Collins et al. 2010) plus a few developments to treat:
- reionization
- forced mesh refinement


All runs were generated and analysed at the ITASCA Linux cluster at the Supercomputing Centre of Minnesota.


- First, a set of low resolution simulations were produced, sampling a total cosmological volume
of 
(64 Mpc)^3
for each object.

- The most massive clusters (M>10^14 Msol) were resimulated with 2 sets of
nested initial conditions of increasing spatial/DM mass resolution.
The DM mass resolution in the cluster region is mdm=1.2e7 M_sol

- Within the innermost (1/10)^3 of the box, we force the code to refine by x4, achieving
a uniform spatial resolution of 20 kpc (14 kpc/h) everywhere, since the beginning of the run.
Each object is therefore followed since the beginning to the end with 320^3 cells,
covering a comoving region equivalent to 2-3Rvir^3 at z=0.                                  

- Physics: non-radiative plus reionization for 4<z<7.2.

- Saved Outputs: about 100 snapshots for each cluster, with a refined time sampling for z<1 (about 1 snaphost every 100 Myr).

- The "clean" data are presently stored under  /project/jonestw/vazzaf/new_space/


A preliminary draft introducing some of the data and methods of this project can be found here.
List of Clusters:
(classificaton is still tentative!)
MM=post major-merger, RR=relaxing, ME=merging

cluster ID
Mv
Number
of snapshot
Rv
status

[1e14Mo]

[Mpc]

IT1
6.65
0-104
2.30
MM
IT3
3.86
0-90
1.90
ME
IT6
4.01
0-109
1.94
-
IT7
1.02
0-115
1.24
-
IT10
8.95
0-169
2.54
RE
IT15B
2.87
only 1 (z=0)
1.74
-
IT62
21.71
0-125
3.40
-
IT15A
15.90
50-127
3.06

IT15A-outer
"
1-125
"
 outer parts
IT16B 3.90
0-124
1.92

IT30 6.28
0-84
2.26

IT30B
2.34
0-85
1.64



MAPS OF ALL CLUSTERS (z=0)
Gas density middle cut


Gas temperature middle cut



MOVIES OF EVOLVING CLUSTERS
IT 1 - MERGING
IT 3 - MAJOR MERGER
 IT 10 - RELAXED



New! Evolution of shock Mach number -> shock.mpg

New! Evolution of turbulent velocity -> turb.mpg







SHOCKS (under construction)

Left: cut (20kpc) showing the distribution of Mach number (log(M) is shown) reconstructed with the Velocity-Jump method.
Right: projected map of thermal energy flux across shock waves, for the full 320^3 box.
TURBULENCE (under construction)

cluster E1

Time-evolution of E(k), from z=30 to z=0
The two straight lines show k^-5/3 and k^-2

Time-evolution of E(k), from z=30 to z=0
The spectra all compensated by k^5/3

Comparison of 3D power spectra obtained for the same cluster resimulated with standard AMR
or employing our forced mesh refinement.




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