Goals:
An (almost completed) project to re-simulatean unique sample of
20 galaxy clusters with masses
6e14 M_sol<M< 2e15 M_sol
with Adaptive Mesh Refinement triggered in two ways:
- refining on gas/DM overdensity (delta_rho/rho > 3);
- refining on velocity jumps associated to shocks/turbulence (delta_v/v>3)
using an implemented version of the ENZO 1.5 code (e.g. Norman et al.2007).
Simulations are run on the IBM-SP6/5376 cluster at CINECA (Casalecchio di Reno, Bologna, Italy)
Every run took about 30-40 000 cpu hours run over 512 processors, for a total time of about 800 000 cpu hours to complete the whole sample.
1. Massive and Refined: a sample of large galaxy clusters simulated at high resolution. I:Thermal gas and shock waves properties
(Vazza, F.; Brunetti, G.; Gheller, C.; Brunino, R. - 2010NewA...15..695V New Astronomy)
2.Massive and Refined: a sample of large galaxy clusters simulated at high resolution. II: The statistical properties of turbulent motions in massive galaxy clusters with high spatial resolution (Vazza, F.; Brunetti, G.; Gheller, C.; Brunino, R.; Brüggen, M. - 2010arXiv1010.5950V A&A in press)
3. The scatter in the radial profiles of X-ray luminous galaxy clusters as diagnostic of the thermodynamical state of the ICM
(F.Vazza, M.Roncarelli, S.Ettori, K.Dolag 2010arXiv1011.5783V MNRAS accepted)
4. Merger and non-merger galaxy clusters in cosmological AMR simulations (F.Vazza, proceeding of Nice conference, Nov 2010 2011arXiv1101.2205V )
- First, a set of low resolution simulations were produced, sampling a total cosmological volume of
(480Mpc/h)^3
- The most massive clusters (M>10e15M_sol) were resimulated with initial nested grids of increasing spatial/DM mass resolution. The DM mass resolution in the cluster region is mdm=6.7e8M_sol/h
- Adaptive Mesh Refinement is turned on inside cubes of side 4 R_vir (R_vir is the virial radius of each galaxy cluster at z=0), with the techniques tested in Vazza et al.(2009) allowing for a peak spatial resolution of 25kpc/h, and the fairly large dynamical range of N=(500-600)^3 for each
object.
(classificaton is still tentative!)
MM=post major-merger, RR=relaxing, ME=merging
| ID |
Mv |
Mgas |
Rv |
last-MM |
Ekin/Etot |
note |
| [1e15Mo] |
[1e15Mo] | [kpc] |
redshift |
|||
| E1 |
1.12 |
0.20 |
2.67 |
z=0.1 |
0.43 |
MM |
| E2 |
1.12 |
0.21 |
2.73 |
z>1.0 |
0.47 |
ME |
| E3A |
1.38 |
0.24 |
2.82 |
z=0.2 |
0.43 |
MM |
| E3B |
0.76 |
0.12 |
2.31 |
z>1.0 |
0.55 |
ME |
| E4 |
1.36 |
0.24 |
2.80 |
z=0.5 |
0.44 |
MM |
| E5A |
0.86 |
0.15 |
2.39 |
z>1.0 |
0.47 |
ME
|
| E5B |
0.66 |
0.12 |
2.18 |
z>1.0 |
0.75 |
ME |
| E7 |
0.65 |
0.11 |
2.19 |
z>1.0 |
0.45 |
ME |
| E11 |
1.25 |
0.22 |
2.72 |
z=0.6 |
0.40 |
MM |
| E14 |
1.00 |
0.18 |
2.60 |
z>1.0 |
0.23 |
RE |
| E15A |
1.01 |
0.19 |
2.63 |
z>1.0 |
0.85 |
ME |
| E15B |
0.80 |
0.14 |
2.36 |
z>1.0 |
0.33 |
RE |
| E16A |
1.92 |
0.35 |
3.14 |
z>1.0 |
0.37 |
RE |
| E16B |
1.90 |
0.31 |
3.14 |
z=0.2 |
0.67 |
MM |
| E18A |
1.91 |
0.35 |
3.14 |
z=0.85 |
0.37 |
MM |
| E18B |
1.37 |
0.23 |
2.80 |
z=0.5 |
0.34 |
MM |
| E18C |
0.60 |
0.10 |
2.08 |
z=0.3 |
0.55 |
MM |
| E26 |
0.74 |
0.13 |
2.27 |
z=0.1 |
0.29 |
MM |
| E21 |
0.68 |
0.12 |
2.18 |
z>1.0 |
0.40 |
RE |
| E62 |
1.00 |
0.17 |
2.50 |
z=0.9 |
0.63 |
MM |
a
merger clusters - relaxing clusters
 |
Images of Clusters: OR !!MOVIES!! |
 |
| M500 vs T500 |
S500
vs
T500 |
Yx vs M500 |
 |
 |
 |
| Gas
density |
Gas
Temperature |
Gas
Entropy |
 |
 |
 |
| mean
Mach
number
profile |
shock
energy
flux |
Cosmic Rays Injection |
 |
 |
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