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 )
5. The gas distribution in galaxy cluster outer regions (Eckert, D.; Vazza, F.; Ettori, S.; Molendi, S.; Nagai, D.; Lau, E. T.; Roncarelli, M.; Rossetti, M.; Snowden, S. L.; Gastaldello, F., 2012A&A...541A..57E A&A.)
6. Why are central radio relics so rare? (Vazza, F., Bruggen M.,Van Weeren R., Bonafede A., Dolag K., Brunetti G., 2012MNRAS.421.1868V , MNRAS)
7. Turbulence in the ICM from mergers, cool-core sloshing and jets: results from a new multi-scale filtering approach. (Vazza F., E. Roediger, Bruggen M. , 2012A&A...544A.103V A&A)
8. Discovery of radio halos and double-relics in distant MACS galaxy clusters: clues to the efficiency of particle acceleration (Bonafede, A.; Brueggen, M; van Weeren, R.; Vazza, F.; Giovannini, G.; Ebeling, H.; Edge, A. C.; Hoeft, M.; Klein, U, 2012MNRAS.426...40B,, MNRAS)
9. Properties of gas clumps and gas clumping factor in the intra cluster medium (Vazza, F.;Eckert D.; Simionescu A.; Brueggen M.; Ettori S. 2013MNRAS.429..799V, MNRAS)
10. The X-ray/SZ view of the virial region. I. Thermodynamic properties, ( Eckert, D.; Molendi, S.; Vazza, F.;Ettori, S.; Paltani, S. 2013A&A...551A..22E, A&A)
11.The X-ray/SZ view of the virial region. II. Gas mass fraction (Eckert, D.; Ettori, S.; Molendi, S.; Vazza, F.; Paltani, S., 2013A&A...551A..23E A&A)
12. Gas clumping in galaxy clusters (Eckert, D.; Ettori, S.; Molendi, S.; Vazza, F.; Roncarelli, M.; Gastaldello, F.; Rossetti, M.) 2015MNRAS.447.2198E
13. A new double radio relic in PSZ1 G096.89+24.17 and a radio relic mass-luminosity relation ( de Gasperin, F.; van Weeren, R. J.; Brüggen, M.; Vazza, F.; Bonafede, A.; Intema, H. T., 2014MNRAS.444.3130D, MNRAS)
14. Turbulence in the Intracluster Medium ( Brüggen, M.; Vazza, F., 2015ASSL..407..599B, Chapter of the Book " Magnetic Fields in Diffuse Media", Astrophysics and Space Science Library)
15. Unravelling the origin of large-scale magnetic fields in galaxy clusters and beyond through Faraday Rotation Measures with the SKA (Bonafede, A., Vazza, F., et al. 2015, 2015arXiv150100321B to be published in the AASKA SKA White Book 2015).
- 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!! |
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| M500 vs T500 |
S500
vs
T500 |
Yx vs M500 |
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| Gas
density |
Gas
Temperature |
Gas
Entropy |
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| mean
Mach
number
profile |
shock
energy
flux |
Cosmic Rays Injection |
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