Cosmic Microwave Background

Cosmic Microwave Background

Acoustic Oscillations, Angular Power Spectrum, Imaging and Implications

for Cosmology

Carlo Baccigalupi, March 31, 2004

Outline…Outline…• Present: angular powerPresent: angular power• Future: ImagingFuture: Imaging• CMB cleaningCMB cleaning• Primordial non-GaussianityPrimordial non-Gaussianity• ReionizationReionization• LensingLensing• ……

The Present CMB: Measuring Angular Power

Before And After The First Light

From COBE to WMAP

Courtesy of the NASA/WMAP Science Team

WMAP Maps

23 GHz, 0.82o , 6 mK/Nobs



61 GHz, 0.33o ,

1.4 mK/Nobs

94 GHz, 0.21o ,

1.4 mK/Nobs

Nobs ' 103


The CMB Angular Power Spctrum

Throwing Pebbles In The Primordial Pond

Homogeneity& Isotropy

Black Body Spectrum

+

+

+


The Sound Of The Early Universe

Isocurvature

Adiabatic

The Window On The Early Universe

T/T// 0 on all scales

Cosmological Parameters

Basic Analysis: h, ns, k ¢ dns/dk, b h2, m h2, A,

WMAP, WMAP+ACBAR+CBI+2dF+LymanExtension: , m ,wDE, r

h=0.71§ 0.06, 0.71+0.04

ns=0.91§ 0.06, 0.93§ 0.03k ¢ dns/dk =..., -0.031

+0.016-0.017

b h2 =0.022§ 0.001, 0.0224 § 0.0009m h2 =0.14§ 0.01, 0.135

+0.008-0.009

A=0.9 § 0.1, 0.83+0.09-0.08

-0.03

=0.20§ 0.07, 0.17 § 0.06

Extension: WMAP+ACBAR+CBI+HST+SNIa+(H0>50 km/sec/Mpc):

=1.02 § 0.02Extension: m

Extension: wDE

Extension: r

WMAP+ACBAR+CBI+2dF:

h2=imi/93.5 eV < 0.0076 ´ m <0.23 eV

WMAP+ACBAR+CBI+HST+SNIa+2dF:

wDE < -0.78

WMAP+ACBAR+CBI+2dF+infl.cons.rel.:

r < -0.71

Reionisation

ClT/ exp(-2) on l > lrh

ClT,TE,E,B boosted on l < lrh

' 0.12

The Future CMB: Imaging

Cosmology

CMB Spectrum…

CMB Spectrum…

Reionization: Non-Gaussian Lensing: Non-GaussianPrimordial GWs

Primordial Density Perts.: non-Gaussian?

CMB Spectrum…

Planck According To Dodelson & Hu 2003

True CMB…

WMAP CMB…

True CMB…

Planck CMB…

True CMB…

CMBpol CMB…

CMB CMB CorruptedCorrupted

The Future CMB:

Foreground Removal

CMB CMB CorruptedCorrupted

Fast Independent Component Fast Independent Component Analysis (FastICA)Analysis (FastICA)

x=As+nx=As+n, find W such that, find W such that Wx=s+WnWx=s+Wn FastICA main loop: construct FastICA main loop: construct

W W row by rowrow by rowChoose Choose initial initial wwUpdate Update throughthrough

wwnewnew=E[xg(w=E[xg(wTTx)]-x)]-wE(g’(wwE(g’(wTTx))x))Compare with Compare with ww. If not . If not

converged go back; if converged go back; if converged start up next converged start up next row, keeping orthogonalityrow, keeping orthogonality

OUT

IN

FastICA on Planck SimulationsFastICA on Planck SimulationsMaino et al. 2002Maino et al. 2002

Planck nominal Planck nominal performanceperformance

See Baccigalupi et al. 2003 for results with See Baccigalupi et al. 2003 for results with Planck nominal performancePlanck nominal performance

Component Separation in Component Separation in PolarisationPolarisation

• Perform Monte Carlo simulations to Perform Monte Carlo simulations to quantify the effect of noise distribution quantify the effect of noise distribution

• Build Criteria to Identify Physical Build Criteria to Identify Physical Components in a Heavy Noise EnviromentComponents in a Heavy Noise Enviroment

• Add priors to check quality and consistency Add priors to check quality and consistency of the resultsof the results

• Extract Cosmological Parameters and Extract Cosmological Parameters and Foreground ScienceForeground Science

FastICA and FastICA and COBECOBE

Maino et al. Maino et al. 20032003

FastICA & COBE FastICA & COBE Maino et al. 2003Maino et al. 2003

BlinBlindd

Non-Non-BlindBlind

The Future CMB: Imaging

Physical Cosmology

Primordial non-Primordial non-GaussianityGaussianity

Liguori et al. 2003Liguori et al. 2003

=L+fNL(L2-<L

2>)

The simplest inflationary scenario predicts fNL' 10-1

WMAP: -58< fNL< -134

Planck forecast in progress

Imaging Reionization…Imaging Reionization…

9.5 arcminutes

T/T

Salvaterra, Ferrara et al. 2004 in prep.Salvaterra, Ferrara et al. 2004 in prep.

Normal Stars in proto-galaxiesNormal Stars in proto-galaxies

20% escape fraction20% escape fraction

CMB scattering on moving electornsCMB scattering on moving electorns

compatible with WMAP compatible with WMAP

Dark Energy & CMB: beyond CDark Energy & CMB: beyond Cl l s s

Giovi et al. 2003, PRD in press, astro-ph/0308118 Giovi et al. 2003, PRD in press, astro-ph/0308118

CMB bispectrum CMB bispectrum

BBllm m

l`l`m`m`

l``l``m``m``=a=almlm a al`m`l`m` a al``m``l``m``

aalmlm==ss ( ( )Y )Ylmlm(( )d )d

BBl l`l``l l`l``==m m` m``m m` m`` ( (mmllm`m`

l`l`m``m``

l``l``) a) almlm a al`m`l`m` a al``m``l``m``

ll

l`l`l``l``

(( ) ) ´́ T(T( )/T )/T

CMB bispectrum & Structure Formation CMB bispectrum & Structure Formation

< B< Bllm m

l`l`m`m`

l``l``m`` m`` >=0>=0

< B< Bllm m

l`l`m`m`

l``l``m`` m`` >> 0 0


<B<Bl l`l``l l`l``>=[(2l+1)(2l`+1)(2l``+1)/16>=[(2l+1)(2l`+1)(2l``+1)/16]]1/21/2((00ll00

l`l`0``0``

l``l``) ) ¢¢

¢ ¢ [l(l+1)- l`(l`+1)+ l``(l``+1) ][l(l+1)- l`(l`+1)+ l``(l``+1) ] CCl l Q(l``)Q(l``) +Perm.+Perm.

Q(l)=Q(l)=ss00dec dec D(z) F(z) D(z) F(z)

dzdz

D(z)=[r(zD(z)=[r(zdecdec)-r(z)]/r(z)-r(z)]/r(zdecdec)r(z))r(z)33

F(z)=dPF(z)=dP/dz|/dz|k=l/r(z)k=l/r(z)

PP=(3=(3m0 m0 /2)/2)22(H(H00/ck)/ck)44P(k,z)(1+z)P(k,z)(1+z)22 P(k,z)=AkP(k,z)=AknnT(k,z)T(k,z)22

(( ) = ) =lsslss((++)+)+ISW ISW '' lsslss(()+)+rrlsslss(())¢¢

ISWISW(( )=2 )=2ss00decdecdr ddr d (r, (r, )/d )/d

=2=2ss00decdecdr[(r-rdr[(r-rdecdec)/r)/rdecdecr]r]r,r,))

Hu & White 1997, Bartelmann & Schneider 2001, Hu & White 1997, Bartelmann & Schneider 2001, Komatsu & Spergel 2001, Verde & Spergel 2002Komatsu & Spergel 2001, Verde & Spergel 2002


ll-1-1

=2=2 /k=r(z /k=r(z33)/l)/l

=r(z=r(z22)/l)/l

=r(z=r(z11)/l)/l

r(zr(z11))

r(zr(z22))

r(zr(z33))

zz11

zz22

zz33

zzrr

CMB bispectrum line of sight chronology CMB bispectrum line of sight chronology

ll-1-1

horizon crossing, horizon crossing, decaying linearly, dQ/dz>0 decaying linearly, dQ/dz>0

zz!1!1 :super-horizon scales in a flat :super-horizon scales in a flat CDM universe, dPCDM universe, dP/d/d =0, dQ/dz =0, dQ/dz!! 0 0

zzrr

Non-linearity, Non-linearity, grows, dQ/dz<0 grows, dQ/dz<0

zz!! 0, 0, vanishes, dQ/dz vanishes, dQ/dz!! 0 0

onset of acceleration, change in cosmic onset of acceleration, change in cosmic equation of state, equation of state, decaying linearly, dQ/dz>0 decaying linearly, dQ/dz>0

CMB bispectrum line of sight distributionCMB bispectrum line of sight distribution


CMB bispectrum & Dark Energy CMB bispectrum & Dark Energy Quintessence reference modelsQuintessence reference models

SUGRASUGRA

RPRP

CMB bispectrum & Dark Energy CMB bispectrum & Dark Energy


Ma et al. Ma et al. 1999, 1999,

Smith et Smith et al. 2003al. 2003

CMB bispectrum & Dark Energy CMB bispectrum & Dark Energy



< B< Bllm m

l`l`m`m`

l``l``m`` m`` >=0>=0

< B< Bllm m

l`l`m`m`

l``l``m`` m`` >> 0 0

Giovi, Liguori et al. 2004, in preparation Giovi, Liguori et al. 2004, in preparation

=2=2ss00decdecdr[(r-rdr[(r-rdecdec)/r)/rdecdecr]r]r,r,))

Continua…Continua…• Component Separation & WMAP…Component Separation & WMAP…• Impact of CMB bispectrum on Planck Impact of CMB bispectrum on Planck

Cosmological Parameter Estimation…Cosmological Parameter Estimation…• Weakly Lensed CMB Templates, Semi-Weakly Lensed CMB Templates, Semi-

analytical…analytical…• Weakly Lensed CMB Templates, Numerical…Weakly Lensed CMB Templates, Numerical…• Weakly Lensed CMB Templates, Weakly Lensed CMB Templates,

Polarisation…Polarisation…• Weakly Lensed CMB Templates, Comparison Weakly Lensed CMB Templates, Comparison

with Gravitational Wave Signal…with Gravitational Wave Signal…

Cosmic Microwave Background

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