Ringing in the New Cosmology
|
|
- Blaise Paul
- 5 years ago
- Views:
Transcription
1 Ringing in the New Cosmology 80 T (µk) Boom98 CBI Maxima-1 DASI l (multipole) Acoustic Peaks in the CMB Wayne Hu
2 Temperature Maps
3 CMB Isotropy Actual Temperature Data COBE 1992
4 Dipole Anisotropy our motion 1 part in 1000 COBE 1992
5 Large Angle Anisotropies 1 part in size matters: smallness linear physics COBE 1992
6 Understanding Maps COBE's fuzzy vision W. Hu
7 Understanding Maps COBE's fuzzy vision W. Hu
8 Understanding Maps COBE's imperfect reception W. Hu
9 Understanding Maps Our best guess for the original map W. Hu
10 Precision Cosmology COBE Maxima Hanany, et al. (2000) BOOMERanG de Bernardis, et al. (2000)
11 New DASI Data µK 100µK
12 What MAP Should See Simulated Data
13 Original Power Spectra of Maps 64º Band Filtered
14 Ringing in the New Cosmology
15 Physical Landscape
16 Thermal History
17 A Brief Thermal History Universe cools as it expands, T 1/a = (1+z)
18 A Brief Thermal History CMB photons hotter at high redhift z At z~1000, T~3000K: photons ionize hydrogen
19 A Brief Thermal History Rapid scattering couples photons and baryons Plasma behaves as perfect fluid
20 A Brief Thermal History Redshift-ionization Photon-baryon fluid with pressure
21 Acoustic Oscillations
22 Gravitational Ringing Potential wells = inflationary seeds of structure Fluid falls into wells, pressure resists: acoustic oscillations
23 Plane Waves Potential wells: part of a fluctuation spectrum Plane wave decomposition
24 Harmonic Modes Frequency proportional to wavenumber: ω=kc s Twice the wavenumber = twice the frequency of oscillation
25 Seeing Sound Oscillations frozen at recombination Compression=hot spots, Rarefaction=cold spots
26 Extrema=Peaks First peak = mode that just compresses Recombination T/T Ψ /3 Θ+Ψ k 1 =π/ sound horizon First Peak time N.B.: "compression" short for compression inside potential wells and rarefaction inside potential hills
27 Extrema=Peaks First peak = mode that just compresses Second peak = mode that compresses then rarefies: twice the wavenumber Recombination Recombination T/T Θ+Ψ First Peak T/T Θ+Ψ time time Ψ /3 k 1 =π/ sound horizon Ψ /3 k 2 =2k 1 Second Peak
28 Extrema=Peaks First peak = mode that just compresses Second peak = mode that compresses then rarefies: twice the wavenumber Harmonic peaks: 1:2:3 in wavenumber Recombination Recombination T/T Θ+Ψ First Peak T/T Θ+Ψ time time Ψ /3 k 1 =π/ sound horizon Ψ /3 k 2 =2k 1 Second Peak
29 Angular Peaks
30 Why Anisotropies? Spatial temperature perturbation oscillating in time and frozen in at recombination Providence Oscillations Spatial Inhom.
31 Peaks in Angular Power Standing wave acoustic oscillations in local temperature
32 Peaks in Angular Power Oscillations frozen in at recombination Prompt release of photons
33 Peaks in Angular Power Photons ariving at observer show an anisotropy whose angular scale decreases with time Temperature inhomogeneity anisotropy
34 Peaks in Angular Power The Anisotropy Formation Process
35 Acoustic Landscape
36 The First Peak
37 First Peak Precisely Measured
38 Spatial Curvature Physical scale of peak = distance sound travels Angular scale measured: comoving angular diameter distance test for curvature Flat Closed
39 Curvature in the Power Spectrum Features scale with angular diameter distance Angular location of the first peak
40 A (Nearly?) Flat Universe h<0.8 Ω b h 2 <0.025 ΩΛ BOOMERanG MAXIMA closed open Ω m Hubble constant! (Ω m h 2 : higher peaks) How Flat? Age of the universe
41 What Makes It Flat? h<0.8 Ω b h 2 <0.025 ΩΛ BOOMERanG Clusters MAXIMA closed open Ω m Info on H 0, Ω m, or Ω Λ breaks degeneracy H 0 : currently by assuming flatness, future by measuring Ω m h 2 Cosmic Complementarity
42 A (Nearly?!) Flat Universe ΩΛ h<0.8 Ω b h 2 <0.025 MAXIMA Perlmutter et al. (1998) Riess et al. (1998) BOOMERanG closed open SNe Clusters Ω m Currently showing consistency with Ω Λ >0
43 Dirty Laundry: Standard Rulers Calibrating the Standard Rulers Sound Horizon Damping Scale Baryons Matter/Radiation Baryons Matter/Radiation
44 The Second Peak
45 Baryon & Inertia Baryons add inertia to the fluid Equivalent to adding mass on a spring Same initial conditions Same null in fluctuations Unequal amplitudes of extrema
46 A Baryon-meter Low baryons: symmetric compressions and rarefactions T time Low Baryons
47 A Baryon-meter Load the fluid adding to gravitational force Enhance compressional peaks (odd) over rarefaction peaks (even) T time Baryon Loading
48 A Baryon-meter Enhance compressional peaks (odd) over rarefaction peaks (even) e.g. relative suppression of second peak T time
49 Baryons in the Power Spectrum
50 Second Peak Detected
51 Score Card
52 Third Peak
53 Radiation and Dark Matter Radiation domination: potential wells created by CMB itself Pressure support potential decay Elimation of modulation from baryon loading
54 Dark Matter in the Power Spectrum
55 Third Peak Constrained
56 Driving Effects and Matter/Radiation Potential perturbation: Radiation Potential: k 2 Ψ = 4πGa 2 δρ generated by radiation inside sound horizon δρ/ρ pressure supported δρ hence Ψ decays with expansion Ψ T/T η Θ+Ψ Hu & Sugiyama (1995)
57 Driving Effects and Matter/Radiation Potential perturbation: Radiation Potential: Potential Radiation: Feedback stops at matter domination k 2 Ψ = 4πGa 2 δρ generated by radiation inside sound horizon δρ/ρ pressure supported δρ hence Ψ decays with expansion Ψ decay timed to drive oscillation 2Ψ + (1/3)Ψ = (5/3)Ψ 5x boost Ψ T/T Θ+Ψ η Hu & Sugiyama (1995)
58 Driving Effects and Matter/Radiation Potential perturbation: Radiation Potential: Potential Radiation: Feedback stops at matter domination k 2 Ψ = 4πGa 2 δρ generated by radiation inside sound horizon δρ/ρ pressure supported δρ hence Ψ decays with expansion Ψ decay timed to drive oscillation 2Ψ + (1/3)Ψ = (5/3)Ψ 5x boost Ψ T/T Θ+Ψ η Hu & Sugiyama (1995)
59 Damping Tail
60 Diffusion Damping Random walk during recombination Dissipation as hot meets cold Physical scale for standard ruler or calibration
61 Dissipation / Diffusion Damping Imperfections in the coupled fluid mean free path λ C in the baryons Random walk over diffusion scale: geometric mean of mfp & horizon λ D ~ λ C N ~ λ C η >> λ C Overtake wavelength: λ D ~ λ ; second order in λ C /λ Viscous damping for R<1; heat conduction damping for R>1 N=η / λ C 1.0 λ D ~ λ C N λ Power 0.1 perfect fluid instant decoupling Silk (1968); Hu & Sugiyama (1995); Hu & White (1996) l
62 Dissipation / Diffusion Damping Rapid increase at recombination as mfp Independent of (robust to changes in) perturbation spectrum Robust physical scale for angular diameter distance test (Ω K, Ω Λ ) Recombination 1.0 Power 0.1 perfect fluid instant decoupling recombination Silk (1968); Hu & Sugiyama (1995); Hu & White (1996) l
63 The Peaks
64 Mapping Dark Matter with the Damping Tail Hu (2001)
65 Mapping Dark Matter with the Damping Tail New gradient-divergence statistic: original mass (deflection) map reconstructed 1.5' beam; 30µK-arcmin noise Hu (2001)
66 Mapping Dark Matter with the Damping Tail Resolving the damping tail crucial to mapping Lower resolution expmt measure power spectrum deflection power (x 10 7 ) Planck l
67 Beyond the Peaks
68 Degeneracies Multiple cosmological parameters have (nearly) degenerate effects on the power spectrum Example: reionization and gravity waves
69 Polarization Thomson of quadrupole temperature anisotropy Linear polarization:
70 Polarization Generation Quadrupole anisotropies generated in optically thin regime Anisotropies <10% polarized
71 Why Polarization is Difficult Source of polarization is the scattering of quadrupole anisotropies Rapid scattering destroys quadrupole anisotropies Polarization only from the optically thin period before full transparency T (µk) < 10% l
72 Polarization Patterns Pattern reflects the projection of quadrupole anisotropies Three types: density, vorticity, gravity waves Potential to isolate gravity waves hot m=0 m=1 m=2 v cold hot v v Density Vorticity Gravity Waves
73 Local vs. Observable Polarization Thomson scattering generates a pure E-pattern locally Plane wave perturbation modulates the amplitude If modulation: in a 0º or 90º direction then E in a 45º direction as polarization then B Last Scat. Surface hot cold θ observer Plane Wave Modulation Hu & White (1997)
74 Secondary Anisotropies CMB photons traverse the large-scale structure of the universe Scattering (~few%), gravitational redshift, lensing
75 Power in Secondaries Gravitational ISW (redshift) Effect Weak Lensing Scattering Doppler Effect Vishniac Effect Kinetic SZ Effect Patchy Reionization Thermal SZ Effect Separation Arcminute Scales Spectrum Non-Gaussianity Polarization Power primary ISW doppler linear l nonlin SZ lensing linear nonlin patch Vishniac
76 Summary Precision cosmology has arrived Sound physics seen (pun intended) Consistent with inflationary initial conditions
77 Summary Precision cosmology has arrived Sound physics seen (pun intended) Consistent with inflationary initial conditions First peak nailed: nearly flat universe Second detected: baryonic dark matter (consistent with Big Bang Nucleosynthesis) Third constrained: cold dark matter required
78 Summary Precision cosmology has arrived Sound physics seen (pun intended) Consistent with inflationary initial conditions First peak nailed: nearly flat universe Second detected: baryonic dark matter (consistent with Big Bang Nucleosynthesis) Third constrained: cold dark matter required Degeneracies remain dark energy: complementary measures gravitational waves: polarization reionization: polarization & secondaries
79 Maps Power Spectrum Thermal History Ringing Plane Waves Harmonics Extrema Seing Sound Peaks First Peak Data Index Geometry C l 's: curvature Flatness Second Peak Baryon Inertia Baryonmeter C l 's: baryons Radiation C l 's: dark matter Damping Diffusion C l 's: rulers Degeneracies Polarization Generation Patterns Secondaries C l 's: secondaries Summary Details & Outtakes Microsoft
CMB 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 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 informationLecture 3+1: Cosmic Microwave Background
Lecture 3+1: Cosmic Microwave Background Structure Formation and the Dark Sector Wayne Hu Trieste, June 2002 Large Angle Anisotropies Actual Temperature Data Really Isotropic! Large Angle Anisotropies
More informationLecture 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 informationCMB Polarization and Cosmology
CMB Polarization and Cosmology Wayne Hu KIPAC, May 2004 Outline Reionization and its Applications Dark Energy The Quadrupole Gravitational Waves Acoustic Polarization and Initial Power Gravitational Lensing
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 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 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 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 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 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 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 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 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 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 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 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 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 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 informationSimulating Cosmic Microwave Background Fluctuations
Simulating Cosmic Microwave Background Fluctuations Mario Bisi Emma Kerswill Picture taken from: http://astro.uchicago.edu/~tyler/omegab.html Introduction What is the CMB and how was it formed? Why is
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 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 information3 Observational Cosmology Evolution from the Big Bang Lecture 2
3 Observational Cosmology Evolution from the Big Bang Lecture 2 http://www.sr.bham.ac.uk/~smcgee/obscosmo/ Sean McGee smcgee@star.sr.bham.ac.uk http://www.star.sr.bham.ac.uk/~smcgee/obscosmo Nucleosynthesis
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 informationCMB studies with Planck
CMB studies with Planck Antony Lewis Institute of Astronomy & Kavli Institute for Cosmology, Cambridge http://cosmologist.info/ Thanks to Anthony Challinor & Anthony Lasenby for a few slides (almost) uniform
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 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 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 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 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 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 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 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 informationGravitational Lensing of the CMB
Gravitational Lensing of the CMB SNAP Planck 1 Ω DE 1 w a.5-2 -1.5 w -1 -.5 Wayne Hu Leiden, August 26-1 Outline Gravitational Lensing of Temperature and Polarization Fields Cosmological Observables from
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 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 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 informationAstr 2320 Thurs. May 7, 2015 Today s Topics Chapter 24: New Cosmology Problems with the Standard Model Cosmic Nucleosynthesis Particle Physics Cosmic
Astr 2320 Thurs. May 7, 2015 Today s Topics Chapter 24: New Cosmology Problems with the Standard Model Cosmic Nucleosynthesis Particle Physics Cosmic Inflation Galaxy Formation 1 Chapter 24: #3 Chapter
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 informationCMB beyond a single power spectrum: Non-Gaussianity and frequency dependence. Antony Lewis
CMB beyond a single power spectrum: Non-Gaussianity and frequency dependence Antony Lewis http://cosmologist.info/ Evolution of the universe Opaque Transparent Hu & White, Sci. Am., 290 44 (2004) CMB temperature
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 informationBrief Introduction to Cosmology
Brief Introduction to Cosmology Matias Zaldarriaga Harvard University August 2006 Basic Questions in Cosmology: How does the Universe evolve? What is the universe made off? How is matter distributed? How
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 informationSecondary Polarization
Secondary Polarization z i =25 0.4 Transfer function 0.2 0 z=1 z i =8 10 100 l Reionization and Gravitational Lensing Wayne Hu Minnesota, March 2003 Outline Reionization Bump Model independent treatment
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 informationH 0 is Undervalued BAO CMB. Wayne Hu STSCI, April 2014 BICEP2? Maser Lensing Cepheids. SNIa TRGB SBF. dark energy. curvature. neutrinos. inflation?
H 0 is Undervalued BICEP2? 74 Maser Lensing Cepheids Eclipsing Binaries TRGB SBF SNIa dark energy curvature CMB BAO neutrinos inflation? Wayne Hu STSCI, April 2014 67 The 1% H 0 =New Physics H 0 : an end
More informationThe Cosmic Microwave Background and Dark Matter
The Cosmic Microwave Background and Dark Matter (FP7/20072013) / ERC Consolidator Grant Agreement n. 617656 Constantinos Skordis (Institute of Physics, Prague & University of Cyprus) Paris, 30 May 2017
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 informationMODERN COSMOLOGY LECTURE FYTN08
1/43 MODERN COSMOLOGY LECTURE Lund University bijnens@thep.lu.se http://www.thep.lu.se/ bijnens Lecture Updated 2015 2/43 3/43 1 2 Some problems with a simple expanding universe 3 4 5 6 7 8 9 Credit many
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 informationThe first light in the universe
The first light in the universe Aniello Mennella Università degli Studi di Milano Dipartimento di Fisica Photons in the early universe Early universe is a hot and dense expanding plasma 14 May 1964, 11:15
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 informationPhysics 661. Particle Physics Phenomenology. October 2, Physics 661, lecture 2
Physics 661 Particle Physics Phenomenology October 2, 2003 Evidence for theory: Hot Big Bang Model Present expansion of the Universe Existence of cosmic microwave background radiation Relative abundance
More informationPhysics 218: Waves and Thermodynamics Fall 2003, James P. Sethna Homework 11, due Monday Nov. 24 Latest revision: November 16, 2003, 9:56
Physics 218: Waves and Thermodynamics Fall 2003, James P. Sethna Homework 11, due Monday Nov. 24 Latest revision: November 16, 2003, 9:56 Reading Feynman, I.39 The Kinetic Theory of Gases, I.40 Principles
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 informationModern Cosmology April 4, Lecture 3 1
The Age of Precision Cosmology Can we see the Big Bang? What s s our Universe made of? The Cooling Universe Expanding cooling (diluting energy content): must ve been really hot early on You can t begin
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. Introduction Geometry and expansion history (Cosmic Background Radiation) Growth Secondary anisotropies Large Scale Structure
Cosmology Introduction Geometry and expansion history (Cosmic Background Radiation) Growth Secondary anisotropies Large Scale Structure Cosmology from Large Scale Structure Sky Surveys Supernovae Ia CMB
More informationRayleigh scattering:
Rayleigh scattering: blue sky thinking for future CMB observations arxiv:1307.8148; previous work: Takahara et al. 91, Yu, et al. astro-ph/0103149 http://en.wikipedia.org/wiki/rayleigh_scattering Antony
More informationThe Expanding Universe
Cosmology Expanding Universe History of the Universe Cosmic Background Radiation The Cosmological Principle Cosmology and General Relativity Dark Matter and Dark Energy Primitive Cosmology If the universe
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 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 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 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 informationCosmology in a nutshell + an argument against
Cosmology in a nutshell + an argument against Ω Λ = based on the inconsistency of the CMB and supernovae results Charles H Lineweaver arxiv:astro-ph/983v Mar 998 University of New South Wales, Sydney,
More informationPhysics Nobel Prize 2006
Physics Nobel Prize 2006 Ghanashyam Date The Institute of Mathematical Sciences, Chennai http://www.imsc.res.in shyam@imsc.res.in Nov 4, 2006. Organization of the Talk Organization of the Talk Nobel Laureates
More informationMicrocosmo e Macrocosmo
Microcosmo e Macrocosmo Paolo de Bernardis Dipartimento di Fisica Sapienza Università di Roma Lezioni della Cattedra Fermi 23 Gennaio 2014 Dipartimento di Fisica Sapienza Università di Roma Friedman s
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 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: 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 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 informationCOSMOLOGY PHYS 30392 COSMIC MICROWAVE BACKGROUND RADIATION Giampaolo Pisano - Jodrell Bank Centre for Astrophysics The University of Manchester - April 2013 http://www.jb.man.ac.uk/~gp/ giampaolo.pisano@manchester.ac.uk
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 informationModeling the Universe A Summary
Modeling the Universe A Summary Questions to Consider 1. What does the darkness of the night sky tell us about the nature of the universe? 2. As the universe expands, what, if anything, is it expanding
More informationCosmology & CMB. Set6: Polarisation & Secondary Anisotropies. Davide Maino
Cosmology & CMB Set6: Polarisation & Secondary Anisotropies Davide Maino Polarisation How? Polarisation is generated via Compton/Thomson scattering (angular dependence of the scattering term M) Who? Only
More informationLecture 19 Nuclear Astrophysics. Baryons, Dark Matter, Dark Energy. Experimental Nuclear Physics PHYS 741
Lecture 19 Nuclear Astrophysics Baryons, Dark Matter, Dark Energy Experimental Nuclear Physics PHYS 741 heeger@wisc.edu References and Figures from: - Haxton, Nuclear Astrophysics - Basdevant, Fundamentals
More informationIntroduction to Cosmology
Introduction to Cosmology True progress in cosmology began in the 20th century: General Relativity Powerful tools of observational astronomy Two critical observations: 1. Hubble's Law (1929): Measure both
More informationCosmological Signatures of a Mirror Twin Higgs
Cosmological Signatures of a Mirror Twin Higgs Zackaria Chacko University of Maryland, College Park Curtin, Geller & Tsai Introduction The Twin Higgs framework is a promising approach to the naturalness
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 informationThe Cosmic Background Radiation
The Cosmic Background Radiation 1. Expansion history of the universe At time of inflation, we have three fundamental scalar fields: Higgs, inflaton, dark energy. We still don t know what dark energy is,
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 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 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 informationModern Cosmology Final Examination Solutions 60 Pts
Modern Cosmology Final Examination Solutions 6 Pts Name:... Matr. Nr.:... February,. Observable Universe [4 Pts] 6 Pt: Complete the plot of Redshift vs Luminosity distance in the range < z < and plot (i)
More information