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The Jubilee Simula-on
William Watson
21/06/2012
21/06/2012
The JUropa huBbLE volumE (JUBILEE) Project
1
Collabora-on: Ilian Iliev (Sussex), Gustavo Yepes (UAM), Alexander Knebe (UAM), Stefan GoJloeber (AIP), Jose Maria Diego (UniCan), E. MarNnez González (IFCA)
Simula-on run late 2011, taking ~1.5 million compu-ng hours, on Juropa at the Jülich Supercompu-ng Centre (JSC), Germany. Using 8000 cores.
6 Gpc/h box size, 60003 par-cles (216 Billion), Par-cle Mass: 7.49x1010 /h Msun, resolu-on down to the smoothing length of 50kpc/h
30 output slices stored of par-cle data (halo catalogues stored for 105 slices) – totaling ~150 TB of data
WMAP 5 cosmology (ΩM= 0.27; ΩΛ= 0.73; h = 0.7; σ8 =0.8; n=0.96; Ωbaryon= 0.044)
Code used was CubeP3M, a massively parallel, collisionless dark maJer N-‐body code
jubilee.k.uam.es/simula-ons
21/06/2012
Jubilee Science Goals
2
All-‐sky map of the Integrated Sachs-‐Wolfe effect (or ISW)
Catalogs of luminous red galaxies (or LRG), radio and IR galaxies
All sky maps of the Sunyaev-‐Zel’dovich (or SZ) effect
All sky maps of lensing effects
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6 Gpc/h
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3 Gpc/h
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1.5 Gpc/h
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500 Mpc/h
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The Jubilee Mass Func-on
10
1013 1014 1015 1016
log10[MM!
]
100 1000 10000 105
Number of Particles
!6
!5
!4
!3
!2
!1
log 1
0[M
2
!0
dN
dM]
SOAHFFOF
PSST
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SO and AHF Residuals z = 0
11
!1
!0.6
!0.2
0.2
0.6
1ST-SO Tinker-SO
!1
!0.6
!0.2
0.2
0.6
1ST-AHF Tinker-AHF
Number of Particles
log10[MM!
]
Data!
Analytic
Analytic
102 103 104 105 102 103 104 105
1013 1014 1015 1016 1013 1014 1015 1016
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FOF Residuals z = 0
12
!1!0.8!0.6!0.4!0.2
00.20.40.60.81
ST Angulo Warren!1
!0.8!0.6!0.4!0.2
00.20.40.60.81
Jenkins Crocce Courtin
Number of Particles
log10[MM!
]
Data!
Analytic
Analytic
102 103 104 105 102 103 104 105 102 103 104 105
1013 1014 1015 1016 1013 1014 1015 1016 1013 1014 1015 1016
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FOF Residuals z = 0
13
!1!0.8!0.6!0.4!0.2
00.20.40.60.81
ST Angulo Warren!1
!0.8!0.6!0.4!0.2
00.20.40.60.81
Jenkins Crocce Courtin
Number of Particles
log10[MM!
]
Data!
Analytic
Analytic
102 103 104 105 102 103 104 105 102 103 104 105
1013 1014 1015 1016 1013 1014 1015 1016 1013 1014 1015 1016
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Redshik Evolu-on
14
1013 1014 1015 1016
log10[MM!
]
100 1000 10000 105
Number of Particles
!8
!7
!6
!5
!4
!3
!2
!1
0log 1
0[M
2
!0
dN
dM]
z = 0.0z = 0.5z = 1.0z = 2.0z = 3.0z = 4.0z = 5.0z = 6.0Tinker
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Redshik Evolu-on
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!1
!0.8
!0.6
!0.4
!0.2
0
0.2
0.4
0.6
0.8
1!1
!0.8
!0.6
!0.4
!0.2
0
0.2
0.4
0.6
0.8
1TinkerST
Data!
Analytic
Analytic
log10[MM!
]
Number of Particles
102 103 104 105 102 103 104 105 102 103 104 105 102 103 104 105
1013 1014 1015 1016 1013 1014 1015 1016 1013 1014 1015 1016 1013 1014 1015 1016
z = 5.0 z = 6.0z = 3.0 z = 4.0
z = 1.0 z = 2.0z = 0.0 z = 0.5
21/06/2012
Cosmic Variance – Mass Func-on
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!0.15
!0.1
!0.05
0
0.05
0.1
!0.15
!0.1
!0.05
0
0.05
0.1
0.15
Octan
t!FullBox
FullBox
log10[MM!
]
Number of Particles
102 103 104 105 102 103 104 105 102 103 104 105 102 103 104 105
1013 1014 1015 1016 1013 1014 1015 1016 1013 1014 1015 1016 1013 1014 1015 1016
z = 5.0 z = 6.0z = 3.0 z = 4.0
z = 1.0 z = 2.0z = 0.0 z = 0.5
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Simula-ng The ISW Effect
17
EdS Universe
T (z = 0) T (z = CMB)
Φ
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Simula-ng The ISW Effect
18
ΛCDM Universe
T + ΔT (z = 0)
T (z = CMB)
Φ
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Simula-ng The ISW Effect
19
ΛCDM Universe
T + ΔT (z = 0)
T (z = CMB)
Φ
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When?
20
ϒ Λ
1100
Redshift
0
0.5
1!m
!!
!!
21/06/2012
Where?
21
Need a large volume to observe the effect as it occurs most strongly for large-‐scale perturba-on modes in the density field (100s of Mpcs)
For Jubilee we need to resolve down to the scale of Luminous Red Galaxies (LRGs) (1013 M halos) to cross correlate with the ISW signal
Need many snapshots to ensure integral is accurate (Jubilee has 30 between z = 0 and 6).
Cai et al. 2010
21/06/2012
Poten-al Calcula-on
22
We calculate the poten-al from the density:
- Smooth the density field (CIC, 60003 grid) - Calculate the poten-al from the density using Poisson’s
equa-on:
- And the Mul-ple Fourier Transform (MFT) method (Hockney and Eastwood)
From the poten-al we then calculate the Temperature:
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6 Gpc/h
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3 Gpc/h
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1.5 Gpc/h
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500 Mpc/h
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Cai et al. Maps
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Cross Correla-on With LRGs
Jubilee halos (z = 0.4)
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Next Steps
Complete remaining poten-als from par-cle data (half done – each par-cle snapshot is 5 Tb)
Produce full sky maps of density and poten-al fields (not vital – nice to have)
Convert poten-al into ISW Temperature maps
Produce full sky maps of LRGs from halo catalogues
Cross correlate to ISW signal