박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), j. r. gott (princeton, usa), j....
TRANSCRIPT
![Page 1: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/1.jpg)
박창범 ( 고등과학원 )
& 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada)
한국계산과학공학회 창립학술대회 2009. 9. 12
Cosmological N-Body Simulation of Cosmic Structure Formation
![Page 2: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/2.jpg)
Simulation of Cosmic Structure Formation
1. Purpose of cosmological simulations
2. Structure
3. Requirements
4. Recent achievement
![Page 3: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/3.jpg)
History of the Universe
![Page 4: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/4.jpg)
우주 조망도
관측 가능한 시공간
대폭발 특이면빛 분리면
암흑시대
재이온화시기
현재
high-z시대
![Page 5: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/5.jpg)
Comparison between simulated universes with the real universe
Cosmological model
Initial linear density fluctuation
Non-linear gravitational evolutionGalaxy biasing
Redshift space distortionPast light cone effectsSurvey characteristics
Simulated sample of 'galaxies'
The real universe
Observed sample of galaxies
Statistical test of adopted models
Calibration of systematic effects
Prediction of new phenomena
![Page 6: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/6.jpg)
Simulation of Cosmic Structure Formation
1. Purpose
2. Structure of cosmological simulations
3. Requirements
4. Recent achievements
![Page 7: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/7.jpg)
Execution of Cosmological Simulations
0-1. Simulation code
N-body gravity code: PM, P3M, Tree, PM-Tree codes
Hydro code: 1. particle - SPH
2. mesh (AMR) - ENZO, FLASH
0-2. Dynamic ranges
Mass range: simulation particle, collapsed object, total # of particles
Spatial range: simulation box size, force resolution
![Page 8: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/8.jpg)
Structure of Cosmological Simulations
1. Initial conditions
Cosmological model: power spectrum, high-order correlations
Generation of initial conditions on a simulation mesh
2. Evolution & Intermediate analyses
Snapshot, past-light cone, collapsed object data at predetermined epochs
3. Post analyses
Merger tree construction
Assignment of physical values to collapsed objects
Comparison with observations
![Page 9: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/9.jpg)
Growth of Structures from initial Density Fluctuations
13.7b
11.8b
7.7b tb=0
![Page 10: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/10.jpg)
Simulation of Cosmic Structure Formation
1. Purpose
2. Structure
3. Requirements of cosmological simulations
4. Recent achievements
![Page 11: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/11.jpg)
Dream Reality 1 Realty 2 Reality 3
cosmic structures to simulate
stars ~ horizon stars ~ galaxy* subgalactic objects ~ large-scale structure
galaxy ~ cosmological scale
Spatial scales to resolve
0.1pc~104Mpc
1017~1028 cm
0.1pc~100kpc
1017~1023cm
few kpc ~ few 100Mpc
1022~1027cm
few 10kpc~3000Mpc
1023~1028cm
Spatial dynamic range : initial conditions / force resolution**
1011 106 / 105 105 / 104 105 / 104
Dynamic range in mass (# of simulation particles)
1033 1015 1012 1012
(memory~40TB)
* Galaxy, a city of stars, is the building block of the universe
** Force resolution 10 times higher than the mean particle separation assumed
Requirements for cosmological simulations
![Page 12: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/12.jpg)
Simulation of Cosmic Structure Formation
1. Purpose
2. Structure
3. Requirements
4. Recent achievements
![Page 13: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/13.jpg)
Date particles scales machine
2004. 8 20483 0.05~1024 Mpc
0.275~5632 Mpc
IBM SP3 at KISTI, 128 CPUs, 0.9 TB memory
2008. 8* 41203 0.16~6592 Mpc Sun Blade at KISTI, 1648 CPUs, 2.4TB memory
planned** 100003 0.13~14000 Mpc 40TB memory
Major simulations of the KIAS astrophysical simulation group
: LCDM model, PMTree N-body code, galaxy ~ cosmological scale
* Horizon Run
** Horizon Run-II, a trillion particle simulation
![Page 14: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/14.jpg)
( 김주한 & 박창범 2004)
Simulation of bright galaxies and large-scale structure --> SDSS Main galaxy
survey
![Page 15: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/15.jpg)
T H E H O R I Z O N R U N
Kim, Park, Gott & Dubinski (2009)
http://astro.kias.re.kr/Horizon_Run
Here
Now
Universe seen along the past light cone
Deco
uplin
g
Ep
och
Dark
A
ges
The First
Obje
cts
HI +
+
He
p +
e- + +
He
Reionization Epoch
Structure Formation & Evolution
Acceleration (Dark Energy
Dominated)
Deceleration (Matter
Dominated)
Inflatio
n
SDSS Main
![Page 16: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/16.jpg)
( 김주한 , 박창범 , Gott & Dubinski 2009)
Simulation of very bright galaxies and large-scale structure; the 1st simulation out to the horizon --> SDSS-III Luminous Red Galaxy survey
![Page 17: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/17.jpg)
Evolution of the
number of simulatio
n particles
Horizon Run
Millennium Run
Horizon Run-II
![Page 18: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/18.jpg)
Millennium Run
Horizon Run
Horizon Run-II
Evolution of the spatial
dynamic range
box size
resolution scale
![Page 19: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/19.jpg)
Comparison between simulated universes with the real universe
Cosmological model
Initial linear density fluctuation
Non-linear gravitational evolutionGalaxy biasing
Redshift space distortionPast light cone effectsSurvey characteristics
Simulated sample of 'galaxies'
The real universe
Observed sample of galaxies
Statistical test of adopted models
Calibration of systematic effects
Prediction of new phenomena
![Page 20: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/20.jpg)
KSG-VAGC DR7 sample
A tour of the real universe : SDSS galaxies
![Page 21: 박창범 ( 고등과학원 ) & 김주한 ( 경희대학교 ), J. R. Gott (Princeton, USA), J. Dubinski (CITA, Canada) 한국계산과학공학회 창립학술대회 2009. 9. 12 Cosmological](https://reader033.vdocuments.pub/reader033/viewer/2022051516/56649d925503460f94a78465/html5/thumbnails/21.jpg)
Final SDSS DR7 Main Galaxy Sample (2008)
[Choi et al. 2009]
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The Sloan Great Wall (Gott et al. 2005)
The CfA Great Wall (Geller and Huchra 1989)
The Cosmic Runner (Park et al. 2005)
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SDSS2006
CfA1986
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Voids (blue - 7% low), filaments/clusters (red - 7% high) => Sponge !! (Gott et al. 2008)
SDSS2006
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A mock survey of massive halos out to z=0.6 simulating the SDSS-III Luminosity Red Galaxy Survey
that will finish in 2014.
[the Horizon Run (Kim et al. 2009)]
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Summary
1. The cosmological N-body gravity simulation is limited by memory, and hydrodynamics simulation is limited by both memory and speed.
2. In the near future a trillion particle N-body gravity simulation will be made for the first time.
3. The low-resolution cosmological simulation is now reaching the horizon scale.
4. The high-R cosmological simulations are increasing the box size, and the low-R simulations are increasing the force resolution toward smaller scales.
5. Cosmological simulations are indispensable for understanding the observed universe, guiding new surveys, and predicting new scientific findings.
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