cosmology & dark matter - indico.nikhef.nl · scott dodelson, modern cosmology. geometry of...
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Cosmology & Dark MatterCosmology & Dark Matter
Christoph WenigerChristoph WenigerUniversity of AmsterdamUniversity of Amsterdam
BND Graduate School 2017BND Graduate School 20171111thth Sep 2017 Sep 2017
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A brief history of the Universe
Credit: NAOJ
● 1e-43 s: Quantum gravity ● >1e-34 s: Inflation● <1e-11 s: Baryogenesis● 1e-11 s: Electroweak phase transition (particles acquire rest mass)● 1e-5 s: QCD phase transition (protons & neutrons form)● 1 s: Neutrino decoupling● 3 min: Big-bang nucleosynthesis
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Outline
Lecture 1 – Geometry, dynamics & thermal history of the Universe● Geodesic equation and FRW-metric● Einstein Equation and expansion of Universe● Thermodynamics in expanding Universe● Dark relics, neutrino decoupling, big-bang nucleosynthesis
Lecture 2 – Inflation and linear structure formation● Horizon problem● Inflation and scalar field dynamics● Linear structure formation● Formation of the cosmic microwave background
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Outline
Lecture 3 – The non-linear Universe, dark matter and MOND● Evidence for dark matter● N-body simulations of CDM● CDM problems and solutions● Status of Modified Newtonian Dynamics (MOND)
Lecture 4 – Searches for particle dark matter● Properties of dark matter & dark matter production● Dark matter candidates & Searches● Indirect searches for dark matter
● Signal characteristics● Searches with cosmic rays● Searches with photons● Signal hints and challenges
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“Natural units”
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Lecture 1
Geometry, dynamics &thermal history of the Universe
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Literature
Here and in the following I use material from the Baumann cosmology lectures
http://cosmology.amsterdam/education/cosmology/
&
Scott Dodelson, Modern Cosmology
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Geometry of space
The geometry of space is encoded in the metric, which connects observer-dependent coordinates with physical distances.
In 3-dimensional Euclidean space, with coordinates (x, y, z), the infinitesimal length dl is connected to dx, dy and dz via:
Example: The same metric in spherical coordinates, , reads
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Space-time geometry = Gravity
In general relativity, the fundamental object is the 4-dim space-time metric, which relates the observer-dependent coordinates, , to the invariant line element (corresponds to proper time)
Special relativity has the constant metric
The metric in general relativity depends on the space-time position:
Gravity = Geometry
Einstein sum convention
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Universe today: The 2dF Galaxy Redshift Survey
http://www.roe.ac.uk/~jap/2df/
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Metric of the Universe
The Universe appears to be on large scales● Isotropic = the same in all directions● Homogeneous = the same at all places● Changing with time
This means that the time-dependence of the metric can be factored out in the scale factor, a(t),
and the line-element is supposed to describe a “maximally symmetric 3-space”.
Side remark: one can use conformal time, , to simplify equations.
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Friedmann-Robertson-Walker Metric
Three maximally symmetric 3-spaces● Positive curvature
(spherical, k=1)● Zero curvature
(flat, k=0)● Negative curvature
(hyperbolic, k=-1)
FRW Metric Credit: Researchgate
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Geodesic equation
In absence of (non-gravitational) forces, particles move along geodesics. These can be defined as curves of least action, which extremize the proper time of a curves connecting two points.
Christoffel symbols (vanishing for constant metric)
Geodesic equation
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Dynamics and energy momentum Tensor
The geodesic equation is invariant under a parameter rescaling
Definition of proper time by (time measured by clock along the geodesic)via the four-velocity
The four-momentum is defined as
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Massless and massive particles
For a massless particle in a FRW Universe, one can show that
This implies that radiation redshifts as the Universe expands
For massive particles: with
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Distance ladder and expansion
Local Universe: Simple connection of redshift and Hubble parameter today(modulo peculiar motion of object relative to the Hubble flow)
Standard candles (here Type IA supernovae) can be used to constrain expansion history
Effects at high redshift● Energy loss (due to redshift)● Corrections to physical distance● Corrections to expansion history
Hubble’s Law
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Various cosmological distance measures
Comoving line-of-sight (LOS) distance towards object emitting at redshift z.
Luminosity distance
(F: energy flux)
Angular distance
(D: physical size)
(here only flat Universe!)
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Distance measures
Time passed since redshift z
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Dynamics
The dynamics of the metric, of a(t), is determined by the Einstein equations
1. Energy momentum tensor of a perfect fluid in the rest-frame
Equation of state
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Energy momentum tensor
Continuity equation
This implies, for constant w,
Contributions to the energy density at late times
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Friedmann equations
2. Einstein tensor
Implied equations of motion
Hubble parameter as function of scale parameter
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Energy densities scaling
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Fractional energy densities scaling
Matter radiation equality (MRE)
differentneutrino masses
Dark energy matter equality
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Equilibrium thermodynamics
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Overview over different epochsCo
vere
d to
day
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Equilibrium thermodynamics
For now, we focus on an isotropic Universe. The distribution function is independent of x.
Fermions, bosons, and intensive quantities
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Relativistic and non-relativistic limits
Relativistic boson and fermion gases
Non-relativistic limit
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Effective number of relativistic DOF
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Entropy
Entropy density can be defined as
Entropy is conserved in reversible adiabatic expansion
One temperature Multiple components with different temperatures
Effective entropy degrees of freedom
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Neutrino decoupling
Neutrino freeze-out
Electron positron annihilation:
Degrees of freedom
Induced temperature difference
~71%
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Recombination and photon decoupling
Photo dissociation of Hydrogen
Decoupling
Saha equation (ionization equilibrium)
baryon-to-photon ratio
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Recombination and photon decoupling
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Dark matter relics
Boltzmann equation for particles in comoving volume
Relic density today
“WIMP miracle”
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BBN
Helium – and in traces other light elements – are produced during big-bang nucleosynthesis (BBN)● Above 0.1 MeV, only neutrons and protons exist● Primordial Helium after BBN mass fraction is ~25%● Production of Helium requires the existence of
deuterium
● Binding energy of deuterium is low
(while binding energy of Helium is 28.3 MeV!)● Deuterium formation is delayed by photo dissociation
Impact on element abundances→
Consider neutron fraction
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BBN
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BBN
Primordial abundances of elements provide information about the baryon density in the early Universe.
A general diagnostic for new-physics searches● Relativistic degrees of freedom
● Changes in neutron lifetime, masses, or gravitational or electro-weak couplings would affect abundances.
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Lecture 2
Inflation and Linear Structure Formation
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The particle horizon
Particle horizon Comoving distance a photon has propagated since the beginning of time
Photon propagation
Conformal time: Comoving distance
Comoving Hubble radius
Normal matter implies:
The size of particle horizon is dominated by late times.
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The horizon problem
In the standard picture, points p and q of the CMB were never in causal contact. In fact, the CMB is made of ~1e4 causally disconnected patches.
Yet, the CMB is remarkably uniform. This is the “horizon problem”.
Past light cones of present-day observer
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Inflation as solution to the horizon problem
Idea: There was more conformal time than naively thought!
Significant contributions in the past require
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Some characteristics of inflation
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Conditions for slow-roll inflation
1. Accelerated expansion
Number of “e-folds”2. Inflation lasts sufficiently long
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Scalar field dynamics
Real scalar field
Corresponding energy and momentum densities
Equation of motion
with
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Slow-roll inflation
Slow-roll parametersPragmatic parameters that describe slow-roll properties of inflaton field.
implies
Number of “e-folds”How many factors of e the Universe inflated
Solving horizon problem requires about 60 e-folds
for single scalar field
Ratio of comoving Hubble radii at end of inflation and today
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Exercise
As an example, perform a slow-roll analysis of arguably the simplest model of inflation: single-field inflation driven by a mass term
1) Derive the slow roll parameters
Q: How large must the scalar field value be to satisfy the slow-roll conditions?
2) Derive the relation between the inflation field value and the number of e-folds before the end of inflation.
Q: What is the required minimum start value for the inflation field to obtain N~60?
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Linear structure formation and consequences
● Linear growth of initial density and metric perturbations● Generation of the cosmic microwave background (CMB)● Generation of large scale structures (LSS)
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End of inflation and density perturbations
End of inflation and reheating● Inflation ends when kinetic energy starts
to dominate
● Inflaton field behaves like matter
● Inflaton field decays into SM particles, which thermalize (reheating)
Adiabatic density perturbations from quantum fluctuations
where
Metric perturbation power spectrumDensity and metric perturbations are connected
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Metric and density perturbations
Small perturbations to the mean metric and energy density.
Metric perturbations (“Newtonian gauge”)
Neglect anisotropic stress:
Energy-momentum tensor perturbations
Corresponds to Newton potential
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EoM for metric perturbations
EoM for metric perturbations (from
Matter era
super-horizon modes are frozen
sub-horizon mode oscillate and decay
Use Fourier transform of field
)
Radiation era
(damped oscillator)
Frequency: Amplitude decreases like:
all modes are frozen
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Metric perturbations
super-horizon mode
frozen in matter era
damped oscillation
frozen in radiation era beforemode enters horizon
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Metric perturbations today
1. Primoridal fluctuations
2. Transfer functionuntil a~1e-2
Potential today
3. Growth functionat late times
Small modes decay away before MRE
Large modes not affected
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Matter perturbations
Poisson equation
Matter density power spectrum
In matter era, the Poisson equation connects matter and metric perturbations
(from inflation)
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Matter power spectrum
Primordial fluctuationsDecay (and oscillation) before MRE
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Matter power spectrum
Tegmark+ 2004
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The cosmic microwave background
Planck satellite
Temperature fluctuations
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Radiation field perturbations
Equation of motion for the baryon-photon fluid
Until “decoupling” at z~1100, there is a strong coupling between electrons and photons, which behave like a single fluid.
Sound speedBaryon to photon ratio
before MRE● gravitational potential small
after MRE● grav. potential as external force
For sub-horizon modes
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Baryon-photon field oscillations
Evolution of gravitational potential and photon perturbations in radiation era
● Gravitational potential decays, and drives photon perturbations● Photons diffuse over finite length scales, leading to damping and the
generation of quadrupole fluctuations● What is actually observable today is
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Formation of peaks in the CMB power spectrum
The peak on the largest scales (first peak) is generated by the mode that entered the horizon so late that it could just perform ~1/4 of its oscillation.
Decoupling
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Observed temperature fluctuations
Momentum loss in expanding perturbed Universe
→ Perceived temperature fluctuations
Sachs-Wolfe term “Integrated Sachs-Wolfe”
Doppler shift&
At decoupling!
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Definition of angular power spectrum
Angular power spectrum
Legendre Polynomial
where
Angular power spectrum of the CMB:Describes the correlations of temperature fluctuations of the CMB in different sky directions
Mapping of plane wave modes onto temperature fluctuations.
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Predictions for the CMB
First peak
General predictions for the angular power spectrum of the temperature fluctuations in the cosmic microwave background
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Results from Planck satellite
Planck 2015
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Parameters from fit to Planck data
Planck 2015 results