Lecture 3+1: Cosmic Microwave Background
|
|
- Marshall Floyd
- 5 years ago
- Views:
Transcription
1 Lecture 3+1: Cosmic Microwave Background Structure Formation and the Dark Sector Wayne Hu Trieste, June 2002
2 Large Angle Anisotropies Actual Temperature Data Really Isotropic!
3 Large Angle Anisotropies dipole anisotropy 1 part in 1000
4 Large Angle Anisotropies 10º 90º anisotropy 1 part in
5 Understanding Maps COBE's fuzzy vision
6 Understanding Maps COBE's fuzzy vision
7 Understanding Maps COBE's imperfect reception
8 Understanding Maps Our best guess for the original map
9 Small Angle Anisotropies? <1º anisotropy seeing inside the horizon
10 New DASI Data µK 100µK
11 MAP Satellite has Launched!
12 What MAP Should See Simulated Data
13 Original Power Spectra of Maps 64º Band Filtered
14 Ringing in the New Cosmology
15 Power Spectrum Today 100 IAB Sask T (µk) FIRS COBE Viper BAM QMAP SP Ten ARGO IAC BOOM Pyth TOCO BOOM RING CAT MAX MSAM DASI BOOM WD VSA Maxima OVRO CBI ATCA SuZIE BIMA W. Hu 5/ l
16 Projected MAP Errors 10 1 θ (degrees) T (µk) W. Hu Feb l (multipole)
17 A Brief Thermal History CMB photons hotter at high redhift z At z~1000, T~3000K: photons ionize hydrogen
18 Very Brief History CMB g 3 min 3x10 5 yrs 5x10 9 yrs e p n He Nucleo- Synthesis Last Scattering Galaxy Formation
19 A Brief Thermal History Rapid scattering couples photons and baryons Plasma behaves as perfect fluid
20 From Lecture 2: Photon-Baryon System Photons and baryons described as a single system. Conservation law for the photon-baryon system [ ] d dη + 3ȧ δρ γb + 3ȧ a a δp γb = (ρ γb + p γb )(kv γb + 3 Φ), [ ] d dη + 4ȧ [(ρ γb + p γb )v γb /k] = δp γb + (ρ + p)ψ, a or with Θ = δρ γ /ρ γ and R = 3ρ b /ρ γ Θ = k 3 v γb Φ v γb = Ṙ 1 + R v γb + 1 kθ + kψ 1 + R Forced oscillator equation see Zaldarriaga s (now my) talk(s) Anisotropic stresses and entropy generation through non-adiabatic stress Silk damps fluctuations Silk 1968
21 Basics Take a simple photon dominated system, neglecting gravity Continuity Equation: Θ = 1 3 kv γ where Θ = δρ γ /4ρ γ is the temperature fluctuation in the Newtonian gauge expresses number conservation n γ T 3 Euler Equation: v γ = kθ expresses momentum conservation q = F where the force is provided by pressure gradients δp γ = δρ γ /3 = 4Θ/3.
22 Oscillator: Take One Combine these to form the simple harmonic oscillator equation Θ + c 2 sk 2 Θ = 0 where the adiabatic sound speed is defined through c 2 s ṗγ ρ γ here c 2 s = 1/3 since we are photon-dominated Given an initial temperature perturbation and no velocity perturbation, solution is Θ(η) = Θ(0) cos(ks) where the sound horizon is defined as s c s dη
23 A Brief Thermal History Redshift-ionization Photon-baryon fluid with pressure
24 Harmonic Extrema All modes are frozen in at recombination (denoted with a subscript ) yielding temperature perturbations of different amplitude for different modes Θ(η ) = Θ(0) cos(ks ) Modes caught in the extrema of their oscillation will have enhanced fluctuations k n s = nπ yielding a fundamental scale or frequency, related to the inverse sound horizon k A = π/s and a harmonic relationship to the other extrema as 1 : 2 : 3...
25 Peak Location The fundmental physical scale is translated into a fundamental angular scale by simple projection according to the angular diameter distance D θ A = λ A /D l A = k A D In a flat universe, the distance is simply D = d η 0 η η 0, the horizon distance, and k A = π/s = 3π/η so θ A η η 0 In a matter-dominated universe η a 1/2 so θ A 1/30 2 or l A 200
26 Peak Locations: Dark Energy? 80 l 1 ~200 DT (mk) Boom98 CBI Maxima-1 DASI l (multipole)
27 Curvature In a curved universe, the apparent or angular diameter distance is no longer the conformal distance D = R sin(d/r) d α D d=rθ λ Objects in a closed universe are further than they appear! gravitational lensing of the background...
28 Curvature in the Power Spectrum Features scale with angular diameter distance Angular location of the first peak
29 Restoring Gravity Take a simple photon dominated system with gravity Continuity Equation: Θ = 1 3 kv γ Φ includes a redshift effect from the distortion of the spatial metric Recall that in the absence of stress fluctuations Φ =constant and Φ = 0. Euler Equation: v γ = k(θ + Ψ) includes graviational infall generating momentum.
30 Oscillator: Take Two Combine these to form the simple harmonic oscillator equation Θ + c 2 sk 2 Θ = k2 3 Ψ Φ In a CDM dominated expansion Φ = Ψ = 0. Also for photon domination c 2 s = 1/3 so the oscillator equation becomes Θ + Ψ + c 2 sk 2 (Θ + Ψ) = 0 Solution is just an offset version of the original [Θ + Ψ](η) = [Θ + Ψ](0) cos(ks) Θ + Ψ is also the observed temperature fluctuation since photons lose energy climbing out of gravitational potentials at recombination
31 Gravitational Ringing Potential wells = inflationary seeds of structure Fluid falls into wells, pressure resists: acoustic oscillations
32 Sachs-Wolfe Effect and the Magic 1/3 From comoving gauge, where the CMB temperature perturbation is initially negligible, to Newtonian gauge involves a temporal shift δt t = Ψ Temporal shift implies that during matter domination δa a = 2 δt 3 t CMB temperature is cooling as T a so Θ δt T = δa a = 2 3 Ψ Observed or effective temperature Θ + Ψ = 1 3 Ψ
33 Causality and the CMB The harmonic series of peaks of comparable amplitude, now observed, depend on the existence of an initial spatial curvature fluctuation that is nearly scale-invariant. The Bardeen curvature ζ, from Lecture 2 is constant above the horizon ζ = 0 so that if ζ(0) = 0, ζ(η) = 0. A more severe form of the horizon problem: the mechanism which ensures the homogeneity of the universe must also imprint fluctuation to the spatial curvature that are scale invariant and correlated above the apparent horizon. Inflation to the rescue... Given the observations, restrictions on the yellwould-be alternates to inflation are severe, e.g. cosmological defects cannot be the main source of structure
34 Baryon Loading Baryons add extra mass to the photon-baryon fluid Controlling parameter is the momentum density ratio: R p b + ρ b p γ + ρ γ 30Ω b h 2 of order unity at recombination ( a 10 3 ) Θ = k 3 v γb Φ v γb = Ṙ 1 + R v γb + 1 kθ + kψ 1 + R Baryons add to the inertial and gravitational mass but not to the radiation pressure
35 Oscillator: Take Three Combine these to form the not-quite-so simple harmonic oscillator equation c 2 s d dη (c 2 s Θ) + c 2 sk 2 Θ = k2 3 Ψ c2 s d dη (c 2 s Φ) where c 2 s ṗ γb / ρ γb c 2 s = R In a CDM dominated expansion Φ = Ψ = 0 and the adiabatic approximation Ṙ/R ω = kc s [Θ + (1 + R)Ψ](η) = [Θ + (1 + R)Ψ](0) cos(ks)
36 Matter-to-radiation ratio Radiation Driving ρ m ρ r 24Ω m h 2 ( a 10 3 of order unity at recombination in a low Ω m universe Radiation is not stress free and so impedes the growth of structure k 2 Φ = 4πGa 2 ρ 4Θ oscillates around a constant value, ρ a 4 so the Netwonian curvature decays. Decay is timed precisely to drive the oscillator 5 the amplitude of the Sachs-Wolfe effect! N.B. analytic solutions to E.O.M. exist but derivation too lengthy to present here see Hu & Sugiyama (1996) )
37 Damping Tight coupling equations assume a perfect fluid: no viscosity, no heat conduction Fluid imperfections are related to the mean free path of the photons in the baryons λ C = τ 1 where τ = n e σ T a is the conformal opacity to Thompson scattering Dissipation is related to the diffusion length: random walk approximation λ D = Nλ C = η/λ C λ C = ηλ C the geometric mean between the horizon and mean free path λ D /η few %, so expect the peaks 3 to be affected by dissipation
38 Equations of Motion Continuity Θ = k 3 v γ Φ, δb = kv b 3 Φ where the photon equation remains unchanged and the baryons follow number conservation with ρ b = m b n b Euler v γ = k(θ + Ψ) k 6 π γ τ(v γ v b ) v b = ȧ a v b + kψ + τ(v γ v b )/R where the photons gain an anisotropic stress term π γ from radiation viscosity and a momentum exchange term with the baryons and are compensated by the opposite term in the baryon Euler equation
39 Oscillator: Final Take Both viscosity and heat conduction through v γ v b are generated by gradients in the velocity field and add terms proportional to Θ to the oscillator equation c 2 s d dη (c 2 s Θ) + k2 c 2 s τ [A v + A h ] Θ + c 2 sk 2 Θ = k2 3 Ψ d c2 s dη (c 2 s where a leading order expansion in k/ τ in kinetic theory gives A v = 16 15, A h = R2 1 + R solution leads to a damping factor to the amplitude of order Φ) or k D exp( k 2 η/ τ) τ/η as expected from the random walk description
Lecture 3+1: Cosmic Microwave Background
Lecture 3+1: Cosmic Microwave Background Structure Formation and the Dark Sector Wayne Hu Trieste, June 2002 Tie-ins to Morning Talk Predicting the CMB: Nucleosynthesis Light element abundance depends
More informationAstro 448 Lecture Notes Set 1 Wayne Hu
Astro 448 Lecture Notes Set 1 Wayne Hu Recombination Equilibrium number density distribution of a non-relativistic species n i = g i ( mi T 2π ) 3/2 e m i/t Apply to the e + p H system: Saha Equation n
More informationLecture II. Wayne Hu Tenerife, November Sound Waves. Baryon CAT. Loading. Initial. Conditions. Dissipation. Maxima Radiation BOOM WD COBE
Lecture II 100 IAB Sask T (µk) 80 60 40 20 Initial FIRS Conditions COBE Ten Viper BAM QMAP SP BOOM ARGO IAC TOCO Sound Waves MAX MSAM Pyth RING Baryon CAT Loading BOOM WD Maxima Radiation OVRO Driving
More informationCMB Anisotropies: The Acoustic Peaks. Boom98 CBI Maxima-1 DASI. l (multipole) Astro 280, Spring 2002 Wayne Hu
CMB Anisotropies: The Acoustic Peaks 80 T (µk) 60 40 20 Boom98 CBI Maxima-1 DASI 500 1000 1500 l (multipole) Astro 280, Spring 2002 Wayne Hu Physical Landscape 100 IAB Sask 80 Viper BAM TOCO Sound Waves
More informationAstro 448 Lecture Notes Set 1 Wayne Hu
Astro 448 Lecture Notes Set 1 Wayne Hu Recombination Equilibrium number density distribution of a non-relativistic species n i = g i ( mi T 2π ) 3/2 e m i/t Apply to the e + p H system: Saha Equation n
More informationRinging in the New Cosmology
Ringing in the New Cosmology 80 T (µk) 60 40 20 Boom98 CBI Maxima-1 DASI 500 1000 1500 l (multipole) Acoustic Peaks in the CMB Wayne Hu Temperature Maps CMB Isotropy Actual Temperature Data COBE 1992 Dipole
More informationLecture I. Thermal History and Acoustic Kinematics. Wayne Hu Tenerife, November 2007 WMAP
Lecture I WMAP Thermal History and Acoustic Kinematics Wayne Hu Tenerife, November 2007 WMAP 3yr Data WMAP 3yr: Spergel et al. 2006 5000 l(l+1)/2π C l (µk 2 ) 4000 3000 2000 1000 0 200 400 600 800 1000
More informationThe Silk Damping Tail of the CMB l. Wayne Hu Oxford, December 2002
The Silk Damping Tail of the CMB 100 T (µk) 10 10 100 1000 l Wayne Hu Oxford, December 2002 Outline Damping tail of temperature power spectrum and its use as a standard ruler Generation of polarization
More informationThe Physics of CMB Polarization
The Physics of CMB Polarization Wayne Hu Chicago, March 2004 Chicago s Polarization Orientation Thomson Radiative Transfer (Chandrashekhar 1960 ;-) Reionization (WMAP 2003; Planck?) Gravitational Waves
More informationKIPMU Set 4: Power Spectra. Wayne Hu
KIPMU Set 4: Power Spectra Wayne Hu Planck Power Spectrum B-modes: Auto & Cross Scalar Primary Power Spectrum 10 3 10 2 temperature Power (µk 2 ) 10 1 10 0 reion. τ=0.1 cross 10-1 E-pol. 10-2 10 1 10 2
More informationThe AfterMap Wayne Hu EFI, February 2003
The AfterMap Wayne Hu EFI, February 2003 Connections to the Past Outline What does MAP alone add to the cosmology? What role do other anisotropy experiments still have to play? How do you use the MAP analysis
More informationAn Acoustic Primer. Wayne Hu Astro 448. l (multipole) BOOMERanG MAXIMA Previous COBE. W. Hu Dec. 2000
An Acoustic Primer 100 BOOMERanG MAXIMA Previous 80 T (µk) 60 40 20 COBE W. Hu Dec. 2000 10 100 l (multipole) Wayne Hu Astro 448 CMB Anisotropies COBE Maxima Hanany, et al. (2000) BOOMERanG de Bernardis,
More informationCMB Episode II: Theory or Reality? Wayne Hu
s p ac 10 1 CMB Episode II: θ (degrees) n n er p ac u ter 10 1 θ (degrees) 100 80 e 100 80 T (µk) 60 T (µk) 60 40 40 20 20 10 100 l (multipole) 10 100 l (multipole) Theory or Reality? Wayne Hu CMB Anisotropies
More informationThe Once and Future CMB
The Once and Future CMB DOE, Jan. 2002 Wayne Hu The On(c)e Ring Original Power Spectra of Maps 64º Band Filtered Ringing in the New Cosmology Gravitational Ringing Potential wells = inflationary seeds
More informationSecondary CMB Anisotropy
Secondary CMB Anisotropy III: Dark Energy Wayne Hu Cabo, January 2009 Integrated Sachs-Wolfe Effect Smooth Energy Density & Potential Decay Regardless of the equation of state an energy component that
More informationSet 9: CMB and Large Scale Structure
Set 9: CMB and Large Scale Structure CMB Temperature Anisotropy Planck 2015 map of the temperature anisotropy (first discovered by COBE) from recombination: 300 200 100 0 µkcmb 100 200 300 CMB Temperature
More informationReally, really, what universe do we live in?
Really, really, what universe do we live in? Fluctuations in cosmic microwave background Origin Amplitude Spectrum Cosmic variance CMB observations and cosmological parameters COBE, balloons WMAP Parameters
More information20 Lecture 20: Cosmic Microwave Background Radiation continued
PHYS 652: Astrophysics 103 20 Lecture 20: Cosmic Microwave Background Radiation continued Innocent light-minded men, who think that astronomy can be learnt by looking at the stars without knowledge of
More informationProbing the Dark Side. of Structure Formation Wayne Hu
Probing the Dark Side 1 SDSS 100 MAP Planck P(k) 10 3 T 80 60 0.1 LSS Pψ 10 4 10 5 40 20 CMB 10 100 l (multipole) 0.01 k (h Mpc -1 ) 10 6 10 7 10 100 Lensing l (multipole) of Structure Formation Wayne
More informationDark Energy in Light of the CMB. (or why H 0 is the Dark Energy) Wayne Hu. February 2006, NRAO, VA
Dark Energy in Light of the CMB (or why H 0 is the Dark Energy) Wayne Hu February 2006, NRAO, VA If its not dark, it doesn't matter! Cosmic matter-energy budget: Dark Energy Dark Matter Dark Baryons Visible
More informationLecture 03. The Cosmic Microwave Background
The Cosmic Microwave Background 1 Photons and Charge Remember the lectures on particle physics Photons are the bosons that transmit EM force Charged particles interact by exchanging photons But since they
More informationLecture 2. - Power spectrum of gravitational anisotropy - Temperature anisotropy from sound waves
Lecture 2 - Power spectrum of gravitational anisotropy - Temperature anisotropy from sound waves Bennett et al. (1996) COBE 4-year Power Spectrum The SW formula allows us to determine the 3d power spectrum
More informationA5682: Introduction to Cosmology Course Notes. 11. CMB Anisotropy
Reading: Chapter 8, sections 8.4 and 8.5 11. CMB Anisotropy Gravitational instability and structure formation Today s universe shows structure on scales from individual galaxies to galaxy groups and clusters
More informationisocurvature modes Since there are two degrees of freedom in
isocurvature modes Since there are two degrees of freedom in the matter-radiation perturbation, there must be a second independent perturbation mode to complement the adiabatic solution. This clearly must
More informationLecture 09. The Cosmic Microwave Background. Part II Features of the Angular Power Spectrum
The Cosmic Microwave Background Part II Features of the Angular Power Spectrum Angular Power Spectrum Recall the angular power spectrum Peak at l=200 corresponds to 1o structure Exactly the horizon distance
More informationCMB Anisotropies Episode II :
CMB Anisotropies Episode II : Attack of the C l ones Approximation Methods & Cosmological Parameter Dependencies By Andy Friedman Astronomy 200, Harvard University, Spring 2003 Outline Elucidating the
More informationThermal History of the Universe and the Cosmic Microwave Background. II. Structures in the Microwave Background
Thermal History of the Universe and the Cosmic Microwave Background. II. Structures in the Microwave Background Matthias Bartelmann Max Planck Institut für Astrophysik IMPRS Lecture, March 2003 Part 2:
More informationStructures in the early Universe. Particle Astrophysics chapter 8 Lecture 4
Structures in the early Universe Particle Astrophysics chapter 8 Lecture 4 overview Part 1: problems in Standard Model of Cosmology: horizon and flatness problems presence of structures Part : Need for
More informationLecture 4. - Cosmological parameter dependence of the temperature power spectrum (continued) - Polarisation
Lecture 4 - Cosmological parameter dependence of the temperature power spectrum (continued) - Polarisation Planck Collaboration (2016) Let s understand the peak heights Silk+Landau Damping Sachs-Wolfe
More informationGalaxies 626. Lecture 3: From the CMBR to the first star
Galaxies 626 Lecture 3: From the CMBR to the first star Galaxies 626 Firstly, some very brief cosmology for background and notation: Summary: Foundations of Cosmology 1. Universe is homogenous and isotropic
More informationPhysics 463, Spring 07. Formation and Evolution of Structure: Growth of Inhomogenieties & the Linear Power Spectrum
Physics 463, Spring 07 Lecture 3 Formation and Evolution of Structure: Growth of Inhomogenieties & the Linear Power Spectrum last time: how fluctuations are generated and how the smooth Universe grows
More informationInvestigation of CMB Power Spectra Phase Shifts
Investigation of CMB Power Spectra Phase Shifts Brigid Mulroe Fordham University, Bronx, NY, 1458 Lloyd Knox, Zhen Pan University of California, Davis, CA, 95616 ABSTRACT Analytical descriptions of anisotropies
More informationCosmic Microwave Background Introduction
Cosmic Microwave Background Introduction Matt Chasse chasse@hawaii.edu Department of Physics University of Hawaii at Manoa Honolulu, HI 96816 Matt Chasse, CMB Intro, May 3, 2005 p. 1/2 Outline CMB, what
More informationUseful Quantities and Relations
189 APPENDIX B. USEFUL QUANTITIES AND RELATIONS 190 Appendix B Useful Quantities and Relations B.1 FRW Parameters The expansion rate is given by the Hubble parameter ( ) 1 H 2 da 2 (ȧ ) a 2 0 = a dt a
More informationA5682: Introduction to Cosmology Course Notes. 11. CMB Anisotropy
Reading: Chapter 9, sections 9.4 and 9.5 11. CMB Anisotropy Gravitational instability and structure formation Today s universe shows structure on scales from individual galaxies to galaxy groups and clusters
More informationThe cosmic microwave background radiation
The cosmic microwave background radiation László Dobos Dept. of Physics of Complex Systems dobos@complex.elte.hu É 5.60 May 18, 2018. Origin of the cosmic microwave radiation Photons in the plasma are
More informationLicia Verde. Introduction to cosmology. Lecture 4. Inflation
Licia Verde Introduction to cosmology Lecture 4 Inflation Dividing line We see them like temperature On scales larger than a degree, fluctuations were outside the Hubble horizon at decoupling Potential
More informationConcordance Cosmology and Particle Physics. Richard Easther (Yale University)
Concordance Cosmology and Particle Physics Richard Easther (Yale University) Concordance Cosmology The standard model for cosmology Simplest model that fits the data Smallest number of free parameters
More informationThe cosmic background radiation II: The WMAP results. Alexander Schmah
The cosmic background radiation II: The WMAP results Alexander Schmah 27.01.05 General Aspects - WMAP measures temperatue fluctuations of the CMB around 2.726 K - Reason for the temperature fluctuations
More informationWe finally come to the determination of the CMB anisotropy power spectrum. This set of lectures will be divided into five parts:
Primary CMB anisotropies We finally come to the determination of the CMB anisotropy power spectrum. This set of lectures will be divided into five parts: CMB power spectrum formalism. Radiative transfer:
More informationLecture 3. - Cosmological parameter dependence of the temperature power spectrum. - Polarisation of the CMB
Lecture 3 - Cosmological parameter dependence of the temperature power spectrum - Polarisation of the CMB Planck Collaboration (2016) Let s understand the peak heights Silk+Landau Damping Sachs-Wolfe Sound
More informationPerturbation Evolution
107 Chapter 5 Perturbation Evolution Although heaven and earth are great, their evolution is uniform. Although the myriad things are numerous, their governance is unitary. Chuang-tzu, 12 Superhorizon and
More informationModern Cosmology / Scott Dodelson Contents
Modern Cosmology / Scott Dodelson Contents The Standard Model and Beyond p. 1 The Expanding Universe p. 1 The Hubble Diagram p. 7 Big Bang Nucleosynthesis p. 9 The Cosmic Microwave Background p. 13 Beyond
More informationarxiv: v1 [astro-ph] 25 Feb 2008
Lecture Notes on CMB Theory: From Nucleosynthesis to Recombination by Wayne Hu arxiv:0802.3688v1 [astro-ph] 25 Feb 2008 Contents CMB Theory from Nucleosynthesis to Recombination page 1 1 Introduction 1
More informationPower spectrum exercise
Power spectrum exercise In this exercise, we will consider different power spectra and how they relate to observations. The intention is to give you some intuition so that when you look at a microwave
More informationPriming the BICEP. Wayne Hu Chicago, March BB
Priming the BICEP 0.05 0.04 0.03 0.02 0.01 0 0.01 BB 0 50 100 150 200 250 300 Wayne Hu Chicago, March 2014 A BICEP Primer How do gravitational waves affect the CMB temperature and polarization spectrum?
More informationPhysical Cosmology 6/6/2016
Physical Cosmology 6/6/2016 Alessandro Melchiorri alessandro.melchiorri@roma1.infn.it slides can be found here: oberon.roma1.infn.it/alessandro/cosmo2016 CMB anisotropies The temperature fluctuation in
More informationCosmological Structure Formation Dr. Asa Bluck
Cosmological Structure Formation Dr. Asa Bluck Week 6 Structure Formation in the Linear Regime II CMB as Rosetta Stone for Structure Formation Week 7 Observed Scale of the Universe in Space & Time Week
More informationKey: cosmological perturbations. With the LHC, we hope to be able to go up to temperatures T 100 GeV, age t second
Lecture 3 With Big Bang nucleosynthesis theory and observations we are confident of the theory of the early Universe at temperatures up to T 1 MeV, age t 1 second With the LHC, we hope to be able to go
More informationProbing Primordial Magnetic Fields with Cosmic Microwave Background Radiation
Probing Primordial Magnetic Fields with Cosmic Microwave Background Radiation Department of Physics and Astrophysics University of Delhi IIT Madras, May 17, 2012 Collaborators: K. Subramanian, Pranjal
More informationOverview. Chapter Cosmological Background
1 Chapter 1 Overview Is the azure of the sky its true color? Or is it that the distance into which we are looking is infinite? The P eng never stops flying higher till everything below looks the same as
More informationStructure in the CMB
Cosmic Microwave Background Anisotropies = structure in the CMB Structure in the CMB Boomerang balloon flight. Mapped Cosmic Background Radiation with far higher angular resolution than previously available.
More informationStructures in the early Universe. Particle Astrophysics chapter 8 Lecture 4
Structures in the early Universe Particle Astrophysics chapter 8 Lecture 4 overview problems in Standard Model of Cosmology: horizon and flatness problems presence of structures Need for an exponential
More informationNeoClassical Probes. of the Dark Energy. Wayne Hu COSMO04 Toronto, September 2004
NeoClassical Probes in of the Dark Energy Wayne Hu COSMO04 Toronto, September 2004 Structural Fidelity Dark matter simulations approaching the accuracy of CMB calculations WMAP Kravtsov et al (2003) Equation
More informationThe Outtakes. Back to Talk. Foregrounds Doppler Peaks? SNIa Complementarity Polarization Primer Gamma Approximation ISW Effect
The Outtakes CMB Transfer Function Testing Inflation Weighing Neutrinos Decaying Neutrinos Testing Λ Testing Quintessence Polarization Sensitivity SDSS Complementarity Secondary Anisotropies Doppler Effect
More informationWhat can we Learn from the Cosmic Microwave Background
What can we Learn from the Cosmic Microwave Background Problem Set #3 will be due in part on April 8 and in full on April 11 Solutions to Problem Set #2 are online... graded versions soon Again I m asking
More information4 Evolution of density perturbations
Spring term 2014: Dark Matter lecture 3/9 Torsten Bringmann (torsten.bringmann@fys.uio.no) reading: Weinberg, chapters 5-8 4 Evolution of density perturbations 4.1 Statistical description The cosmological
More informationInflation and the origin of structure in the Universe
Phi in the Sky, Porto 0 th July 004 Inflation and the origin of structure in the Universe David Wands Institute of Cosmology and Gravitation University of Portsmouth outline! motivation! the Primordial
More informationInflationary Cosmology and Alternatives
Inflationary Cosmology and Alternatives V.A. Rubakov Institute for Nuclear Research of the Russian Academy of Sciences, Moscow and Department of paricle Physics abd Cosmology Physics Faculty Moscow State
More informationChapter 4. COSMOLOGICAL PERTURBATION THEORY
Chapter 4. COSMOLOGICAL PERTURBATION THEORY 4.1. NEWTONIAN PERTURBATION THEORY Newtonian gravity is an adequate description on small scales (< H 1 ) and for non-relativistic matter (CDM + baryons after
More informationDetails create the big picture the physics behind the famous image of the cosmic microwave background. Marieke Postma
Details create the big picture the physics behind the famous image of the cosmic microwave background Marieke Postma last week Inflation period of accelerated expansion a(t) eht - creates homogeneous and
More informationAstronomy 422. Lecture 20: Cosmic Microwave Background
Astronomy 422 Lecture 20: Cosmic Microwave Background Key concepts: The CMB Recombination Radiation and matter eras Next time: Astro 422 Peer Review - Make sure to read all 6 proposals and send in rankings
More informationAST5220 lecture 2 An introduction to the CMB power spectrum. Hans Kristian Eriksen
AST5220 lecture 2 An introduction to the CMB power spectrum Hans Kristian Eriksen Cosmology in ~five slides The basic ideas of Big Bang: 1) The Big Bang model The universe expands today Therefore it must
More informationThe Cosmic Microwave Background and Dark Matter. Wednesday, 27 June 2012
The Cosmic Microwave Background and Dark Matter Constantinos Skordis (Nottingham) Itzykson meeting, Saclay, 19 June 2012 (Cold) Dark Matter as a model Dark Matter: Particle (microphysics) Dust fluid (macrophysics)
More informationProbing the Dark Side. of Structure Formation Wayne Hu
Probing the Dark Side 1 SDSS 100 MAP Planck P(k) 10 3 T 80 60 0.1 LSS Pψ 10 4 10 5 40 20 CMB 10 100 l (multipole) 0.01 k (h Mpc -1 ) 10 6 10 7 10 100 Lensing l (multipole) of Structure Formation Wayne
More informationWeek 10: Theoretical predictions for the CMB temperature power spectrum
Week 10: Theoretical predictions for the CMB temperature power spectrum April 5, 2012 1 Introduction Last week we defined various observable quantities to describe the statistics of CMB temperature fluctuations,
More informationToward Higher Accuracy: A CDM Example
197 Appendix A Toward Higher Accuracy: A CDM Example The scale invariant cold dark matter (CDM) model with Ω 0 = 1.0 andω b h 2 near the nucleosynthesis value Ω b h 2 0.01 0.02 is elegantly simple and
More informationTheory of galaxy formation
Theory of galaxy formation Bibliography: Galaxy Formation and Evolution (Mo, van den Bosch, White 2011) Lectures given by Frank van den Bosch in Yale http://www.astro.yale.edu/vdbosch/teaching.html Theory
More informationPolarization from Rayleigh scattering
Polarization from Rayleigh scattering Blue sky thinking for future CMB observations Previous work: Takahara et al. 91, Yu, et al. astro-ph/0103149 http://en.wikipedia.org/wiki/rayleigh_scattering Antony
More informationThe early and late time acceleration of the Universe
The early and late time acceleration of the Universe Tomo Takahashi (Saga University) March 7, 2016 New Generation Quantum Theory -Particle Physics, Cosmology, and Chemistry- @Kyoto University The early
More informationAST5220 lecture 2 An introduction to the CMB power spectrum. Hans Kristian Eriksen
AST5220 lecture 2 An introduction to the CMB power spectrum Hans Kristian Eriksen Cosmology in ~five slides The basic ideas of Big Bang: 1) The Big Bang model The universe expands today Therefore it must
More informationCosmology II: The thermal history of the Universe
.. Cosmology II: The thermal history of the Universe Ruth Durrer Département de Physique Théorique et CAP Université de Genève Suisse August 6, 2014 Ruth Durrer (Université de Genève) Cosmology II August
More informationCosmology: An Introduction. Eung Jin Chun
Cosmology: An Introduction Eung Jin Chun Cosmology Hot Big Bang + Inflation. Theory of the evolution of the Universe described by General relativity (spacetime) Thermodynamics, Particle/nuclear physics
More informationIntroduction. How did the universe evolve to what it is today?
Cosmology 8 1 Introduction 8 2 Cosmology: science of the universe as a whole How did the universe evolve to what it is today? Based on four basic facts: The universe expands, is isotropic, and is homogeneous.
More informationBAO & RSD. Nikhil Padmanabhan Essential Cosmology for the Next Generation VII December 2017
BAO & RSD Nikhil Padmanabhan Essential Cosmology for the Next Generation VII December 2017 Overview Introduction Standard rulers, a spherical collapse picture of BAO, the Kaiser formula, measuring distance
More informationCOSMIC MICROWAVE BACKGROUND Lecture I
COSMIC MICROWAVE BACKGROUND Lecture I Isabella Masina Univ. & INFN Ferrara, Italy CP3-Origins SDU, Denmark 18/10/2010 CP3-Origins SUGGESTED BIBLIOGRAPHY 1. W. Hu Lectures and animations http://background.uchicago.edu/~whu/physics/physics.html
More informationn=0 l (cos θ) (3) C l a lm 2 (4)
Cosmic Concordance What does the power spectrum of the CMB tell us about the universe? For that matter, what is a power spectrum? In this lecture we will examine the current data and show that we now have
More informationThe physics of the cosmic microwave background
The physics of the cosmic microwave background V(φ) φ Hiranya Peiris STFC Advanced Fellow University of Cambridge Before we start... Acknowledgment: Anthony Challinor (University of Cambridge) for invaluable
More informationLecture 12. Inflation. What causes inflation. Horizon problem Flatness problem Monopole problem. Physical Cosmology 2011/2012
Lecture 1 Inflation Horizon problem Flatness problem Monopole problem What causes inflation Physical Cosmology 11/1 Inflation What is inflation good for? Inflation solves 1. horizon problem. flatness problem
More informationBAO AS COSMOLOGICAL PROBE- I
BAO AS COSMOLOGICAL PROBE- I Introduction Enrique Gaztañaga, ICE (IEEC/CSIC) Barcelona PhD Studenships (on simulations & galaxy surveys) Postdoctoral oportunities: www.ice.cat (or AAS Job: #26205/26206)
More informationPhysical Cosmology 18/5/2017
Physical Cosmology 18/5/2017 Alessandro Melchiorri alessandro.melchiorri@roma1.infn.it slides can be found here: oberon.roma1.infn.it/alessandro/cosmo2017 Summary If we consider perturbations in a pressureless
More informationInhomogeneous Universe: Linear Perturbation Theory
Inhomogeneous Universe: Linear Perturbation Theory We have so far discussed the evolution of a homogeneous universe. The universe we see toy is, however, highly inhomogeneous. We see structures on a wide
More informationThe Physics Behind the Cosmic Microwave Background
The Physics Behind the Cosmic Microwave Background Without question, the source of the most precise information about the universe as a whole and about its early state is the cosmic microwave background
More informationEl Universo en Expansion. Juan García-Bellido Inst. Física Teórica UAM Benasque, 12 Julio 2004
El Universo en Expansion Juan García-Bellido Inst. Física Teórica UAM Benasque, 12 Julio 2004 5 billion years (you are here) Space is Homogeneous and Isotropic General Relativity An Expanding Universe
More informationCosmology. Jörn Wilms Department of Physics University of Warwick.
Cosmology Jörn Wilms Department of Physics University of Warwick http://astro.uni-tuebingen.de/~wilms/teach/cosmo Contents 2 Old Cosmology Space and Time Friedmann Equations World Models Modern Cosmology
More informationCosmology with CMB & LSS:
Cosmology with CMB & LSS: the Early universe VSP08 lecture 4 (May 12-16, 2008) Tarun Souradeep I.U.C.A.A, Pune, India Ω +Ω +Ω +Ω + Ω +... = 1 0 0 0 0... 1 m DE K r r The Cosmic Triangle (Ostriker & Steinhardt)
More informationSecond Order CMB Perturbations
Second Order CMB Perturbations Looking At Times Before Recombination September 2012 Evolution of the Universe Second Order CMB Perturbations 1/ 23 Observations before recombination Use weakly coupled particles
More informationThe Growth of Structure Read [CO 30.2] The Simplest Picture of Galaxy Formation and Why It Fails (chapter title from Longair, Galaxy Formation )
WMAP Density fluctuations at t = 79,000 yr he Growth of Structure Read [CO 0.2] 1.0000 1.0001 0.0001 10 4 Early U. contained condensations of many different sizes. Current large-scale structure t = t 0
More informationObservational Cosmology
The Cosmic Microwave Background Part I: CMB Theory Kaustuv Basu Course website: http://www.astro.uni-bonn.de/~kbasu/obscosmo CMB parameter cheat sheet 2 Make your own CMB experiment! Design experiment
More informationCosmic sound: near and far
Cosmic sound: near and far Martin White UCB/LBNL for the Planck & BOSS teams Planck BOSS 1 Outline! The standard cosmological model and the CMB. Acoustic oscillations in the infant Universe.! Planck: mission.!
More informationPAPER 71 COSMOLOGY. Attempt THREE questions There are seven questions in total The questions carry equal weight
MATHEMATICAL TRIPOS Part III Friday 31 May 00 9 to 1 PAPER 71 COSMOLOGY Attempt THREE questions There are seven questions in total The questions carry equal weight You may make free use of the information
More informationCOSMOLOGY The Origin and Evolution of Cosmic Structure
COSMOLOGY The Origin and Evolution of Cosmic Structure Peter COLES Astronomy Unit, Queen Mary & Westfield College, University of London, United Kingdom Francesco LUCCHIN Dipartimento di Astronomia, Universita
More informationPhysical Cosmology 12/5/2017
Physical Cosmology 12/5/2017 Alessandro Melchiorri alessandro.melchiorri@roma1.infn.it slides can be found here: oberon.roma1.infn.it/alessandro/cosmo2017 Structure Formation Until now we have assumed
More informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 11 Nov. 13, 2015 Today Cosmic Microwave Background Big Bang Nucleosynthesis Assignments This week: read Hawley and Holcomb,
More informationCOSMIC MICROWAVE BACKGROUND ANISOTROPIES
COSMIC MICROWAVE BACKGROUND ANISOTROPIES Anthony Challinor Institute of Astronomy & Department of Applied Mathematics and Theoretical Physics University of Cambridge, U.K. a.d.challinor@ast.cam.ac.uk 26
More informationRayleigh Scattering and Microwave Background Fluctuations
Rayleigh Scattering and Microwave Background Fluctuations Qingjuan Yu, David N. Spergel 1 & Jeremiah P. Ostriker Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 ABSTRACT
More informationAnalyzing the CMB Brightness Fluctuations. Position of first peak measures curvature universe is flat
Analyzing the CMB Brightness Fluctuations (predicted) 1 st rarefaction Power = Average ( / ) 2 of clouds of given size scale 1 st compression 2 nd compression (deg) Fourier analyze WMAP image: Measures
More informationFrom inflation to the CMB to today s universe. I - How it all begins
From inflation to the CMB to today s universe I - How it all begins Raul Abramo Physics Institute - University of São Paulo abramo@fma.if.usp.br redshift Very brief cosmic history 10 9 200 s BBN 1 MeV
More informationVariation in the cosmic baryon fraction and the CMB
Variation in the cosmic baryon fraction and the CMB with D. Hanson, G. Holder, O. Doré, and M. Kamionkowski Daniel Grin (KICP/Chicago) Presentation for CAP workshop 09/24/2013 arxiv: 1107.1716 (DG, OD,
More informationCosmic Microwave Background Anisotropies
1 Annu. Rev. Astron. and Astrophys. 2002 Parameter Sensitivity.................................... 26 Cosmic Microwave Background Anisotropies Wayne Hu 1,2,3 and Scott Dodelson 2,3 1 Center for Cosmological
More information