inflation and the cosmic microwave background lecture (chapter 9)

Markus Possel¨ + Bjorn¨ Malte Schafer¨

Haus der Astronomie and Centre for Fakultat¨ fur¨ Physik und Astronomie, Universitat¨ Heidelberg

August 1, 2013 repetition inflation random processes CMB secondary summary outline

1 repetition 2 inflation ideas behind inflation mechanics of inflation 3 random processes Gaussian random processes 4 CMB recombination angular spectrum parameter sensitivity 5 secondary anisotropies 6 summary

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary repetition

Friedmann-Lemaˆıtre explain the expansion dynamics • H(a) of the fluids influence Hubble-expansion according to their eos parameter • w > 1/3: expansion slows down • − w < 1/3: expansion accelerates • − dark energy and the can cause accelerated • expansion q < 0, for sufficiently negative eos w > 1/3 − Hubble expansion is an , temperature drops while • expanding, T(a) depends on adiabatic index κ relic (highly redshifted) from early epochs of the universe • nucleosynthesis: neutrino background T = 1.95K • ν formation of hydrogen atoms: microwave background T = 2.75K • CMB

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary expansion history of the universe

expansion history of the universe

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary -scale

at a = 0, z = the diverges, and H(a) becomes infinite • ∞ description of breaks down, effects • become important relevant scales: • quantum mechanics: de Broglie-wave length: λ = 2π~ • QM mc general relativity: Schwarzschild radius: r = 2Gm • s c2 setting λ = r defines the Planck mass • QM s r ~c m = 1019GeV/c2 (1) P G '

question how would you define the corresponding Planck length and the Planck ? what are their numerical values?

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary flatness problem

construct a universe with w = 0and curvature w = 1/3 • − Hubble function • H2(a) Ω Ω m K (2) 2 = 3 + 2 H0 a a density parameter associated with curvature • Ω (a) H2 H2 K 0 0 (3) = 3(1+w) 2 = 2 2 ΩK a H (a) a H (a) Ω increases always and was smaller in the past • K ! 1 Ωm 1 − ΩK ΩK(a) = 1 + a (4) ΩK a ' Ωm we know (from CMB observations) that curvature is very small • today, typical limits are ΩK < 0.01 even smaller in the past 5 → at recombination ΩK 10− • ' 12 at Ω 10− • K ' Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary

horizon size: light travel distance during the • Z da χ = c (5) H a2H(a) assume Ω = 1, integrate from a = a ... a = 1 • m min rec max c p p χH = 2 Ωmarec = 175 ΩmMpc/h (6) H0 comoving size of a volume around a point at recombination inside • which all points are in causal contact angular diameter distance from us to the recombination shell: • c drec 2 arec 5Mpc/h (7) ' H0 ' angular size of the at recombination: θ 2 • rec ' ◦ points in the CMB separated by more than 2 have never been in • ◦ causal contact why is the CMB so uniform if there is no → Markus Possel¨ possibility + Bjorn¨ Malte Sch ofafer¨ heat exchange? inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary inflation: phenomenology

curvature Ω to the comoving Hubble radius c/(aH(a)) • K ∝ if by some mechanism, c/(aH) could decrease, it would drive Ω • K towards 0 and solve the fine-tuning required by the flatness problem shrinking comoving Hubble radius: • d  c  a¨ = c < 0 a¨ > 0 q < 0 (8) dt aH − a˙2 → → equivalent to the notion of accelerated expansion • accelerated expansion can be generated by a dominating fluid with • sufficiently negative equation of state w = 1/3 − horizon problem: fast expansion in inflationary era makes the • universe grow from a small, causally connected region

question what’s the relation between deceleration q and equation of state w?

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary inflaton-driven expansion

analogous to , one postulates an inflaton field φ, with a • small kinetic and a large , for having a sufficiently negative equation of state for accelerated expansion pressure and of a homogeneous scalar field • φ˙2 φ˙2 p = V(φ), ρ = + V(φ) (9) 2 − 2 Friedmann equation • ! 8πG φ˙2 H2(a) = + V(φ) (10) 3 2

continuity equation • dV φ¨ + 3Hφ˙ = (11) − dφ

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary slow roll conditions

inflation can only take place if φ˙2 V(φ) •  inflation needs to keep going for a sufficiently long time: • d d d φ˙2 V(φ) φ¨ V(φ) (12) dt  dt →  dφ

in this regime, the Friedmann and continuity equations simplify: • 8πG d H2 = V(φ), 3Hφ˙ = V(φ) (13) 3 −dφ

conditions are fulfilled if • !2 ! 1 V 1 V 0  1, 00 η 1 (14) 24πG V ≡  8πG V ≡ 

 and η are called slow-roll parameters •

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary stopping inflation

flatness problem: shrinkage by 1030 exp(60) 60 e-folds • ' ' → due to the slow-roll conditions, the energy density of the inflaton • field is almost constant all other fluid densities drop by huge amounts, ρ by 1090, ρ by • m γ 10120 eventually, the slow roll conditions are not valid anymore, the • effective equation of state becomes less negative, acclerated expansion stops reheating: couple φ to other particle fields, and generate particles • from the inflaton’s kinetic energy

question the temperature at the beginning of inflation was equal to the Planck-temperature. what is its value (in Kelvin) and by how much has it dropped until today? Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary generation of fluctuations

fluctuations of the inflation field can perturb the distribution of all • other fluids mean fluctuation amplitude is related to the variance of φ • fluctuations in φ perturb the metric, and all other fluids feel a • perturbed potential relevant quantity • p H2 δΦ2 (15) h i ' V which is approximately constant during slow-roll Poisson-equation in Fourier- k2Φ(k) = δ(k) • − variance of density perturbations: • δ(k) 2 k4 δΦ 2 k3P(k) (16) | | ∝ | | ∝ defines spectrum P(k) of the initial fluctuations, P(k) kn with n 1 • ∝ ' fluctuations are Gaussian, because of the central limit theorem Markus• Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary random fields

random process probability density p(δ)dδ of event δ • → R alternatively: all moments δn = dδ δnp(δ) • h i in cosmology: • random events are values of the density field δ • outcomes for δ(~x) form a statistical ensemble at fixed ~x • ergodic random processes: • one realisation is consistent with p(δ)dδ special case: Gaussian random field • only variance relevant •

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary characteristic function φ(t)

for a continuous pdf, all moments need to be known for • reconstructing the pdf reconstruction via characteristic function φ(t) (Fourier transform) • Z Z X (itx)n X (it)n φ(t) = dxp(x) exp(itx) = dxp(x) = xn (17) n p n n ! n h i ! R with moments xn = dxxnp(x) h i Gaussian pdf is special: • all moments exist! (counter example: Cauchy pdf) • all odd moments vanish • all even moments are expressible as products of the variance • σ is enough to statistically reconstruct the pdf • pdf can be differentiated arbitrarily often (Hermite polynomials) • funky notation: φ(t) = exp(itx) • h i

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary cosmic microwave background

inflation has generated perturbations in the distribution of matter • the hot baryon plasma feels fluctuations in the distribution of (dark) • matter by gravity at the point of (re)combination: • hydrogen atoms are formed • can propagate freely • perturbations can be observed by two effects: • plasma was not at rest, but flowing towards a potential well • → Doppler-shift in temperature, depending to direction of motion plasma was residing in a potential well gravitational • → between the end of inflation and the release of the CMB, the density • field was growth homogeneously all statistical properties of the density field are conserved → testing of inflationary scenarios is possible in CMB observations •

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary formation of hydrogen: (re)combination

temperature of the fluids drops during Hubble expansion • eventually, the temperature is sufficiently low to allow the formation • of hydrogen atoms but: high photon density (remember η = 109) can easily reionise • B hydrogen Hubble-expansion does not cool photons fast enough between • recombination and reionisation neat trick: recombination takes place by a 2-photon process • question at what temperature would the hydrogen atoms form if they could recombine directly? what redshift would that be?

question why do we observe a continuum spectrum from the formation of Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background atoms? repetition inflation random processes CMB secondary anisotropies summary CMB motion dipole

the most important structure on the microwave sky is a dipole • CMB dipole is interpreted as a relative motion of the • CMB dispole has an amplitude of 10 3K, and the peculiar velocity is • − β = 371km/s c · T(θ) = T0 (1 + β cos θ) (18)

question is the Planck-spectrum of the CMB photons conserved in a Lorentz-boost?

question would it be possible to distinguish between a motion dipole and an intrinsic CMB dipole?

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary CMB dipole

source: COBE

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary subtraction of motion dipole: primary anisotropies

source: PLANCK simulation

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary CMB angular spectrum

analysis of fluctuations on a sphere: decomposition in Y • `m X X Z T(θ) = t Y (θ) t = dΩ T(θ)Y∗ (θ) (19) `m `m ↔ `m `m ` m

spherical harmonics are an orthonormal basis system • average fluctuation variance on a scale ` π/θ • ' 2 C(`) = t m (20) h| ` | i averaging ... is a hypothetical ensemble average. in reality, one • computes anh estimatei of the variance,

m=+` 1 X 2 C(`) t m (21) ' 2` + 1 | ` | m= ` −

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary standard ruler principle

trinity nuclear test, 16 milli-seconds after explosion

physical size: combine • 1 time since explosion 2 velocity of fireball distance: combine • 1 physical size 2 angular size

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary formation of baryon acoustic oscillations

evolution of a single perturbation (source: Eisenstein, Seo and Hu (2005))

from a pointlike perturbation, a spherical wave travels in the • photon-baryon-plasma

Markus Possel¨ propagation + Bjorn¨ Malte Sch stopsafer¨ when atoms form inflation and the cosmic microwave background • repetition inflation random processes CMB secondary anisotropies summary cosmic microwave background: standard ruler

all-sky map of the cosmic microwave background, WMAP

hot and cold patches of the CMB have a typical physical size, • related to the horizon size at the time of formation of hydrogen atoms idea: physical size and apparent angle are related, redshift of • known

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary standard ruler: measurement principle (Eisenstein) a a a on on on iz iz iz

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Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary parameter sensitivity of the CMB spectrum

source: WMAP

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary features in the CMB spectrum

predicting the spectrum C(`) is very complicated • perturbations in the CMB photons n T3, u T4, p = u/3 T4: • ∝ ∝ ∝ δn δT δu δp = 3 Θ, = 4Θ = (22) n0 T ≡ u0 p0 continuity and Euler equations: • 2 p n˙ = n0divυ = 0, υ˙ = c ∇ + δΦ (23) − u0 + p0 ∇ use u + p = 4/3u = 4p • 0 0 0 0 combine both equations • c2 1 Θ¨ ∆Θ + ∆δΦ = 0 (24) − 3 3 identify two mechanisms: • oscillations may occur, and photons experience Doppler shifts • photons feel fluctations in the potential: Sachs-Wolfe effect Markus Possel¨ +• Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary parameter sensitivity of the CMB spectrum

source: Wayne Hu Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary baryon acoustic oscillations in the galaxies

pair density ξ(r) of galaxies as a function of separation r

baryon acoustic oscillations: the (pair) density of galaxies is • enhanced at a separation of about 100Mpc/h comoving idea: angle under which this scale is viewed depends on redshift Markus• Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary secondary CMB anisotropies

CMB photons can do interactions in the cosmic large-scale • structure on their way to us two types of interaction: Compton-collisions and gravitational • consequence: secondary anisotropies • study of secondaries is very interesting: observation of the growth • of structures possible, and precision determination of cosmological parameters all effects are in general important on small angular scales below • a degree

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary thermal Sunyaev-Zel’dovich effect

44

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[Jy] 150 44.5 5 W S [deg] and 100 4 β Y S

45 50 3

2 0 latitude 45.5

1 −50 Sunyaev-Zel’dovich flux

46 0 −100 134 134.5 135 135.5 136 0 2 4 6 8 10 12 14 16 18 20 ecliptic longitude λ [deg] dimensionless frequency x = hν/(kBTCMB)

thermal SZ sky map CMB spectrum distortion

Compton-interaction of CMB photons with thermal electrons in • clusters of galaxies characteristic redistribution of photons in energy spectrum • Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary kinetic Sunyaev-Zel’dovich/Ostriker-Vishniac effect

44 4 200

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−3 −50 Sunyaev-Zel’dovich flux −4 46 −100 134 134.5 135 135.5 136 0 2 4 6 8 10 12 14 16 18 20 ecliptic longitude λ [deg] dimensionless frequency x = hν/(kBTCMB)

thermal SZ sky map CMB spectrum distortion

Compton-interaction of CMB photons with electrons in bulk flows • increase/decrease in CMB temperature according to direction of • motion

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary CMB lensing

source: A. Lewis, A. Challinor

gravitational deflection of CMB photons on potentials in the cosmic • large-scale structure CMB spots get distorted, and their fluctuation statistics is changed, • in particular the polarisation

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary integrated Sachs-Wolfe effect

source: B. Barreiro

gravitational interaction of photons with time-evolving potentials • higher-order effect on photon geodesics in general relativity •

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background repetition inflation random processes CMB secondary anisotropies summary summary

inflation: • solves flatness-problem • solves horizon-problem • generates perturbations in the density field • perturbations are Gaussian, and can be described by a correlation • function ξ(r) or a power spectrum P(k) perturbations have a scale-free spectrum P(k) kns with n 1 • ∝ s ' Meszaros-effect changes spectrum to P(k) kns 4 on small scales • ∝ − normalisation of the CDM spectrum P(k) by the parameter σ • 8 cosmic microwave background probes inflationary perturbations • dynamics of the plasma in potential fluctuations • precision determination of cosmological parameters • secondary effects influence the CMB on small scales (gravitational • lensing, Sunyaev-Zel’dovich effect, integrated Sachs-Wolfe effect)

Markus Possel¨ + Bjorn¨ Malte Schafer¨ inflation and the cosmic microwave background