simulating the dark universe and cosmic structure formation · 2006-05-22 · simulating the dark...
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Outline
Simulating the Dark Universe and CosmicStructure Formation
Andreas Marek
Max-Planck Institut for Astrophysics
Advisor-seminar 2006
Outline
Outline
1 A short overview of Structure Formation
2 Dark Matter properties
3 SimulationsThe need for simulationsSimulation techniquesInitial conditions
4 The Millennium RunThe simulations setupA sub-sample of results
5 Outlook: Galaxy Formation
Outline
Outline
1 A short overview of Structure Formation
2 Dark Matter properties
3 SimulationsThe need for simulationsSimulation techniquesInitial conditions
4 The Millennium RunThe simulations setupA sub-sample of results
5 Outlook: Galaxy Formation
Outline
Outline
1 A short overview of Structure Formation
2 Dark Matter properties
3 SimulationsThe need for simulationsSimulation techniquesInitial conditions
4 The Millennium RunThe simulations setupA sub-sample of results
5 Outlook: Galaxy Formation
Outline
Outline
1 A short overview of Structure Formation
2 Dark Matter properties
3 SimulationsThe need for simulationsSimulation techniquesInitial conditions
4 The Millennium RunThe simulations setupA sub-sample of results
5 Outlook: Galaxy Formation
Outline
Outline
1 A short overview of Structure Formation
2 Dark Matter properties
3 SimulationsThe need for simulationsSimulation techniquesInitial conditions
4 The Millennium RunThe simulations setupA sub-sample of results
5 Outlook: Galaxy Formation
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
What means “Structure Formation”?
From an almost uniform CMB (the earliest time we canobserve) ...
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
What means “Structure Formation”?
we see at later times clusters and galxies. This is calledStructure Formation.
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The Standard Model of Structure Formation
the growth of structure originates from seed densityfluctuations
The fluctuations in the CMB are not big enough to explainStructure Formation
density fluctuations grow approximately ∝ scale factor a
Compare: (baryonic) CMB fluctuations of 10−5 at a = 10−3
with current densities of order unity
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The Standard Model of Structure Formation
the growth of structure originates from seed densityfluctuations
The fluctuations in the CMB are not big enough to explainStructure Formation
density fluctuations grow approximately ∝ scale factor a
Compare: (baryonic) CMB fluctuations of 10−5 at a = 10−3
with current densities of order unity
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The Standard Model of Structure Formation
the growth of structure originates from seed densityfluctuations
The fluctuations in the CMB are not big enough to explainStructure Formation
density fluctuations grow approximately ∝ scale factor a
Compare: (baryonic) CMB fluctuations of 10−5 at a = 10−3
with current densities of order unity
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The Standard Model of Structure Formation
the growth of structure originates from seed (DM) densityfluctuations δ
these fluctuations were present before the decoupling ofthe photon-baryon fluid (CMB)
DM strengthens the density contrast and after decouplingbaryonic matter follows the gravitational wells
in the linear regime (δ << 1) this can be calculatedanalytically
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The Standard Model of Structure Formation
the growth of structure originates from seed (DM) densityfluctuations δ
these fluctuations were present before the decoupling ofthe photon-baryon fluid (CMB)
DM strengthens the density contrast and after decouplingbaryonic matter follows the gravitational wells
in the linear regime (δ << 1) this can be calculatedanalytically
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The Standard Model of Structure Formation
the growth of structure originates from seed (DM) densityfluctuations δ
these fluctuations were present before the decoupling ofthe photon-baryon fluid (CMB)
DM strengthens the density contrast and after decouplingbaryonic matter follows the gravitational wells
in the linear regime (δ << 1) this can be calculatedanalytically
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The Standard Model of Structure Formation
the growth of structure originates from seed (DM) densityfluctuations δ
these fluctuations were present before the decoupling ofthe photon-baryon fluid (CMB)
DM strengthens the density contrast and after decouplingbaryonic matter follows the gravitational wells
in the linear regime (δ << 1) this can be calculatedanalytically
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Collisionless dynamics reviewed
DM physics is important!
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Collisionless dynamics reviewed
DM only interacts gravitationally: thus only a non-saturatinglong-range force is important!
Important for collisionless dynamics: Vlasov-equation
∂f∂t
+ ~v∇qf − m∇qΦ∇pf = 0 (1)
apply moments method: Jeans-Equations
no pressure and viscous terms! but: How does relaxationthen proceed ?
how are objects stabilized against gravity ?
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Collisionless dynamics reviewed: Governing equations
DM only interacts gravitationally: thus only a non-saturatinglong-range force is important!Governing Equations −→ Jeans equations:
Continuity equation:
∂ρ
∂t+ div(ρ~v) = 0 (2)
momentum equation:
∂~v∂t
+ (~v∇)~v = −∇Φ − div(ρσ2) (3)
withσ2
ij = 〈~vi~vj〉 − 〈~vi〉〈~vj 〉 (4)
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Collisionless dynamics reviewed: Governing equations
DM only interacts gravitationally: thus only a non-saturatinglong-range force is important!Governing Equations −→ Jeans equations:
Poisson equation:4Φ = 4πGρ (5)
closed system
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Collisionless dynamics reviewed: Dynamical friction
a particle moving through a cloud produces a wake
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Collisionless dynamics reviewed: Dynamical friction
behind the particle there is a density enhancement
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Collisionless dynamics reviewed: Dynamical friction
density enhancement breaks down particle velocity
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Collisionless dynamics reviewed: Dynamical friction
Ekin of particle =⇒ unordered random motion
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Collisionless dynamics reviewed: Dynamical friction
used for describing capturing of objects
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Outline
1 A short overview of Structure Formation
2 Dark Matter properties
3 SimulationsThe need for simulationsSimulation techniquesInitial conditions
4 The Millennium RunThe simulations setupA sub-sample of results
5 Outlook: Galaxy Formation
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The need for simulations / Simulation goals
Gravitational instability leads to non-linear effects that areonly track-able by direct simulations
Thus (large) simulations are needed for theoreticalpredictions of the “Standard Model of Structure Formation”
Simulations can test the consequences of different models(DM,inflation)
Simulations of can be compared to observations and arehelpful to determine experimental biases. Statisticsimportant!
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The need for simulations / Simulation goals
Structure Formation simulations allow to investigate
the time evolution of the hierarchical tree
when (at which redshift) massive clusters and quasarswere formed
galaxy formation; additional input physics (e.g. semi-analytical models) needed!
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Outline
1 A short overview of Structure Formation
2 Dark Matter properties
3 SimulationsThe need for simulationsSimulation techniquesInitial conditions
4 The Millennium RunThe simulations setupA sub-sample of results
5 Outlook: Galaxy Formation
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
N-Body Codes
DM is represented by particles of certain mass
These particles move according evolution equations
Advantage: resolution automatically increases where it isneeded
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Gravity: a heavy burden
DM only interacts via gravity. Makes physics easier! =⇒Good
Gravity is a long range force (every particle interacts withall other particles). Thus direct calculation of gravitationalforce scales with N2 =⇒ Bad (Computational costs)
Think of a clever way to circumvent the direct summation
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Gravity: a heavy burden
DM only interacts via gravity. Makes physics easier! =⇒Good
Gravity is a long range force (every particle interacts withall other particles). Thus direct calculation of gravitationalforce scales with N2 =⇒ Bad (Computational costs)
Think of a clever way to circumvent the direct summation
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Gravity: a heavy burden and a way around
Part I: the Particle Mesh (PM) Method
Compute the mass density on a Cartesian grid
Solve Poisson equation
Interpolate the gravitational field from grid to particles
This is a fast method (scales roughly O(N) with use of FFT)
BUT: it creates large errors for close particles
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Gravity: a heavy burden and a way around
Part II: the Barnes-Hut (BH) Tree Method
Divide space recursively into hierarchy of cells
If appropriate calculate gravitational force by multipoles ofthese cells; else use direct summation (almost neverneeded)
Fast algorithm (scales O(NlogN))
Force for near particles can be calculated quite accurate
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Part II: the Barnes-Hut (BH) Tree Method
Divide space recursively into hierarchy of cells
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Part II: the Barnes-Hut (BH) Tree Method
Calculate gravitational force by multipoles of the cells
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Outline
1 A short overview of Structure Formation
2 Dark Matter properties
3 SimulationsThe need for simulationsSimulation techniquesInitial conditions
4 The Millennium RunThe simulations setupA sub-sample of results
5 Outlook: Galaxy Formation
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Initial conditions: DM Powerspectrum, Theory
We need the initial DM fluctuations which act as seed forgravitational instability. These fluctuations come frominflationary models and are Gaussian random fields.
Theory: P(k) ∝ kns T (k)2 , with T (k) being atransferfunction, and ns = 1
Do measurements give the same?
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
DM Powerspectrum, Measurements
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Initial conditions: the density fluctuations
Once one has a chosen Powerspectrum one can calculatedensity fluctuations δ which are a Gaussian random field
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Initial conditions: From the dark matterPowerspectrum to density fluctuations
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Initial conditions: Cosmological parameters
From CMB + SNIa measurements we obtain thecosmological parameters: ΩΛ, σ8, ns, h, Ωm, ΩB
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Initial conditions: Cosmological parameters
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The Millennium Run
produced by the VirgoConsortium(http://www.virgo.dur.ac.uk/new/)
performed at MPA by V. Springelwith Lean-Gadget-2(http://www.mpa-garching.mpg.de/gadget/)
on an IBM Power4 RegattaSystem (http://www.rzg.mpg.de)
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Outline
1 A short overview of Structure Formation
2 Dark Matter properties
3 SimulationsThe need for simulationsSimulation techniquesInitial conditions
4 The Millennium RunThe simulations setupA sub-sample of results
5 Outlook: Galaxy Formation
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The simulation setup
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The simulation setup
Up to now the largest Structure Formation simulation
21603 particles (≈ 1010)
L = 500 h−1 Mpc
5 h−1 kpc spatial resolution
roughly 840 GByte memory needed
350000 CPU hours on 512 CPUs
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The computer system IBM REGATTA
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Outline
1 A short overview of Structure Formation
2 Dark Matter properties
3 SimulationsThe need for simulationsSimulation techniquesInitial conditions
4 The Millennium RunThe simulations setupA sub-sample of results
5 Outlook: Galaxy Formation
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The universe in a box
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Some movies ... a) Formation of a cluster
(http://www.mpa-garching.mpg.de/galform/datavis/)
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Some movies ... b) Zooming into an cluster
(http://www.mpa-garching.mpg.de/galform/virgo/millennium/)
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Some movies ... c)Flying through the universe
(http://www.mpa-garching.mpg.de/galform/virgo/millennium/)
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The baryonic-acoustic oscillations
At the moment of decoupling the Baryon-Photon gasoscillates in the gravitational potential given by the DM andmodulates this potential
After decoupling the photon gas dilutes quickly (photondensity scales with a−4
Baryons then follow (modified) Dark matter potential
Galaxyformation is “modulated” on a 150 MPc scale(measured by SLOAN)
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The baryonic-acoustic oscillations
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
The baryonic-acoustic oscillations
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Understanding galaxy formation
One has to consider baryonic matter: radiation processesand complicated hydro make life much harder
A lot of unknown physics is involved: details of starformation, galactic winds, AGN feedback effects
Thus phenomenological models are used
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Understanding galaxy formation
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Understanding galaxy formation
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Understanding galaxy formation
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
Understanding galaxy formation
Introduction Dark Matter Properties Simulations The Millennium Run Outlook: Galaxy Formation
References
Volker Springel, The cosmological simulation codeGADGET-2,astro-ph/0505010
Volker Springel et. al., Nature, 435, 629
http://dsg.port.ac.uk/ schaeferb/teaching