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SciDAC 6-30-05 M. L. Norman
San Diego Supercomputer Center, UCSDKeck Observatory, HI
Simulating the Cosmic History of BaryonsDiscoveries Using Advanced Computing
Michael L. Norman, Physics Dept., UC San Diego
validation
SciDAC 6-30-05 M. L. Norman
Cosmic History of Baryons
linear perturbation theory nonlinear simulations
phase transitions gravitational instability
Baryogensis: GUT phase transitiont~10(-12) s speculative
Nucleosynthesis: formation of light nucleit~1-100 s precision era (BBNS)
Recombination: matter & radiation decouplet~380,000 yr precision era (CMB)
Structure Formation: 50 Myr < t < 14 Gyr synthesis erasurveys
SciDAC 6-30-05 M. L. Norman
Grand Challenges in Computational Hydrodynamic Cosmology
Formation and evolution of stellar systems on all scales and epochs
Chemical enrichment and reionization of intergalactic medium
Formation of massive black holes and nature of the quasar phenomenon
Cosmological constraints on nature of dark matter and dark energy
SciDAC 6-30-05 M. L. Norman
Outline
• Cosmology’s Standard Model
• Universe in a Box
• History of Baryons: Discoveries using Advanced Computing
• Exciting Opportunities Ahead– Cosmological limits on dark matter mass– Measuring dark energy equation of state
SciDAC 6-30-05 M. L. Norman
04.0~
3.0~ ,7.0~
3
820
b
M
ii H
G
• Concordance model– H0=72+/-7 km/s/Mpc
– expansion rate accelerating (q0<0)
– flat universe (k=0)– dominated by dark matter and
dark energy– baryons minor constituent
Cosmology’s Standard Model
Perlmutter (2003), Physics Today
SciDAC 6-30-05 M. L. NormanS. Perlmutter, Physics Today (2003)
Evidence for an Accelerating Universe
SciDAC 6-30-05 M. L. Norman
Cosmic Microwave BackgroundTemperature Fluctuations 380,000 yr ABB
T/T ~ ~ 10-4
NASA WMAP
SciDAC 6-30-05 M. L. Norman
The Universe is an IVP suitable for computation
• Globally, the universe evolves according to the Friedmann equation
33
8)(
2
22
a
kG
a
atH
Hubble parameter
mass-energydensity
spacetimecurvaturescale factor a(t)
cosmological constant
SciDAC 6-30-05 M. L. Norman
The Universe is an IVP...
• Locally*, its contents obey:– Newton’s laws of gravitational N-body
dynamics for stars and cold dark matter– Euler or MHD equations for baryonic
gas/plasma – Atomic and molecular processes important
for radiative cooling of gas and condensation to form stars and galaxies
– Radiative transfer equation for photons
(*scales << horizon scale ~ ct)
Numerical astrophysics on a cosmic scale
SciDAC 6-30-05 M. L. Norman
radiationbackground
galaxies IGM
photo-ionizationphoto-heating
absorption
feedback(energy, metals)SF-recipe
self-shieldingphoto-evaporation
infall
ionizingflux
multi-specieshydrodynamics
radiative transfer
N-body dynamics
cosmic expansion self-gravitydark matter
dynamics
baryonic universe
SciDAC 6-30-05 M. L. Norman
Cold Dark Matter• Dominant mass constituent: cdm~0.23• Only interacts gravitationally with ordinary matter
(baryons)• Candidates: WIMPs or axions• Collisionless dynamics governed by Vlasov-Poisson
equation
• Solved numerically using fast N-body methods
),,( 4
0),,(32 txfdG
fftxf xt
SciDAC 6-30-05 M. L. Norman
Gridding the Universe
• Transformation to comoving coordinates x=r/a(t)
a(t1) a(t2) a(t3)
• Triply-periodic boundary conditions
But what about initial conditions?
SciDAC 6-30-05 M. L. Norman
Matter Power Spectrum P(k)
http://www.hep.upenn.edu/~max
Concordancemodel
SciDAC 6-30-05 M. L. Norman
Gravitational Instability: Origin of Cosmic Structure
A
B
C
A
B
C
x
x
very small fluctuations
gravity amplifies fluctuations
Formation of the Cosmic Web:Sky Dome Rendering for DomeFest 2005
Michael Norman, Brian O’Shea, UCSD
Donna Cox, Robert Patterson, Stuart Levy, UIUCSteve Cutchin, Amit Chourasia, SDSC
SciDAC 6-30-05 M. L. Norman
Technical Details• Simulation (Enzo)
– Dark matter, gravity, multispecies gas dynamics, photo-ionization and, radiative cooling
– 1 billion cells, 1 billion particles– 512 cpu, NCSA TeraGrid cluster
• Data– 512x512x512 arrays of density– 2000 timesteps– 1 Terabyte of data
• Volume rendering– SDSC IBM DataStar
SciDAC 6-30-05 M. L. Norman
Cosmological Adaptive Mesh Refinement(Bryan & Norman 1997)
• Spatial dynamic range unlimited in principle
• Today:– L/ = 104 in statistical volumes– L/ =1010 single objects of interest
• Petascale:– L/ =106 in statistical volumes
SciDAC 6-30-05 M. L. Norman
Enzo Implementation Details • Multi-scale in space and time• Arbitrary # levels of refinement• Arbitrary # grids per level• Portable, MPI-parallel, C++/C/F77 hybrid• Nonlocal dynamic load balancing• Ported to IA64, SGI Altix, IBM SP, BG/L, your mother’s Linux cluster, …..
• Technical details– 2563 base grid– >32,000 grid patches @ 8 levels of refinement– 110,000 cpu-hrs on 128 cpu Origin2000– 0.5 TB of data– Run at NCSA in 1999
Image credit: D. Cox et al.Science credit: M. Norman, G. Bryan, B. O’Shea
Galaxy Formation and Large Scale Structure
SciDAC 6-30-05 M. L. Norman
Computational Discoveriesusing Advanced Computing
First baryoniccondensations
SciDAC 6-30-05 M. L. Norman
“Bottom-Up” Galaxy Formation
• large galaxies form from mergers of smaller galaxies
• where does this begin?
•What are the first objects to form?
Lacey & Cole (1993)
SciDAC 6-30-05 M. L. Norman
First objects: a well-posed problem
• Initial conditions specified: i, P(k)
• Macroscopic dynamics understood
• Microphysics of primordial gas known
• Have 3D solution-adaptive algorithms
• Have adequate computer power
February 2003
SciDAC 6-30-05 M. L. Norman
Formation of First StarsAdaptive Mesh Refinement Simulation
Abel, Bryan & Norman (2001)
1 x 10 x 100 x 1000 x
104 x105 x106 x107 x
Cosmic scales
Solar system scales
SciDAC 6-30-05 M. L. Norman
Birth and Death of the First Star in the Universe
Movie credit: R. Kaehler & T. AbelScience credit: T. Abel, G. Bryan, M. Norman
SciDAC 6-30-05 M. L. Norman
Impact of the first stars the first stars in the universe began forming around
50 million years after the big bang
they were exceptionally massive and bright, bringing an earlier end to the cosmic “dark ages” than previously thought
when they exploded as supernovae they seeded the universe with heavy elements essential for planets and life
they kick-started the cosmogonic sequence which eventually formed galaxies, clusters and superclusters
SciDAC 6-30-05 M. L. Norman
Computational Discoveriesusing Advanced Computing
structure ofintergalacticmedium
SciDAC 6-30-05 M. L. Norman
N=10243
L=54 Mpc/h
Structure of the IGM
Baryon Overdensity, z=3
quasar
Earth
Simulated HI absorption spectrum
SciDAC 6-30-05 M. L. Norman
Computational Discoveriesusing Advanced Computing
whereaboutsof missingbaryons
SciDAC 6-30-05 M. L. Norman
Missing Baryons at z=0
• Galaxies in local universe account for only 10% of baryons we know exist due to three independent measurements, which all agree to 2– Big bang nucleosynthesis– CMB anisotropies– IGM absorption at high redshift
• Where are the baryons now?
SciDAC 6-30-05 M. L. Norman
Whereabouts of the missing baryons:
Warm-Hot intergalactic gas
Cen & Ostriker (1998)
warm-hot gas
“galaxies”
N=5123
SciDAC 6-30-05 M. L. Norman
Exciting Opportunities Ahead(require Terascale and beyond)
• Predicting properties of first galaxies
• Understanding quasar-galaxy connection
• Self-consistent simulation of the reionization era
• Cosmological limits on dark matter mass
• Measuring the dark energy equation of state
SciDAC 6-30-05 M. L. Norman
Effect of DM particle mass on first objects: critical threshold
25 keV
10 keV
O’Shea & Norman (2005)
SciDAC 6-30-05 M. L. Norman
Measuring Dark Energy EOS
• Principal goal of NASA/DOE JDEM mission
• Approach: precision measurements of expansion history of the universe using Type Ia SN standardizable candles
• Complimentary approach: redshift distribution of galaxy clusters
SciDAC 6-30-05 M. L. Norman
Lightcone Simulation(A. Evrard et al. 2003)
• Evrard et al. – Single, 10243 P3M– L/=104
– Dark matter only
• Our plan– Multiple, 5123 AMR– Optimal tiling of lightcone– L/=105
– Dark matter + gas
ct (Gyr)
0 -1 -2 -3 -4 -5
SciDAC 6-30-05 M. L. Norman
• Cosmic Simulator• A software facility for physical cosmology• A new collaboration between LLNL and UCSD• Scientific data management focus
– Simulations: LLNL Thunder, BG/L– Data management: SDSC SRB– Public archive @ UCSD
• Science driver: – LSST (Large Synoptic Survey Telescope)