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Cosmic Microwave Background

发布时间:2014-02-11 14:04:18  

Cosmic Microwave

Background

Acoustic Oscillations, Angular Power Spectrum, Imagingand Implications for Cosmology

Carlo Baccigalupi, March 31, 2004

Outline…???????Present: angular powerFuture: ImagingCMB cleaningPrimordial non-GaussianityReionizationLensing…

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

33 GHz, 0.62o,3 mK/?Nobs23 GHz, 0.82o,6 mK/?NobsNobs '103 41 GHz, 0.49o

2 mK/?Nobs,

94 GHz, 0.21o,

1.4 mK/?Nobs

61 GHz, 0.33o,

1.4 mK/?Nobs

Courtesy of the NASA/WMAP Science Team

The CMB Angular Power Spctrum

Throwing Pebbles In The Primordial Pond

Homogeneity

& Isotropy

Black Body Spectrum+

+

+

Courtesy of the NASA/WMAP Science Team

The Sound Of The Early Universe

Adiabatic

Isocurvature

+

The Window On The Early Universe

dT/T/dr/r?

0 on all scales

Cosmological Parameters

Basic Analysis: h, ns, k ¢22dns/dk, ?b h, ?m h, A, ?Extension: ?, m?,wDE, r

WMAP, WMAP+ACBAR+CBI+2dF+Lyman?

2?b h=0.022§0.001,0.0224 §0.00092?m h=0.14§0.01,0.135

h=0.71§0.06,0.71?=0.20§0.07,0.17 §0.06

ns=0.91§0.06,0.93§0.03

k ¢dns/dk =...,-0.031

A=0.9 §0.1,0.83+0.008-0.009+0.04-0.03+0.016-0.017+0.09

-0.08

Extension: ?

WMAP+ACBAR+CBI+HST+SNIa+(H0>50 km/sec/Mpc):Extension: m??=1.02 §0.02

′m?<0.23 WMAP+ACBAR+CBI+2dF:

eVExtension: wDE

Extension: r2??h=?imi/93.5 eV < 0.0076WMAP+ACBAR+CBI+HST+SNIa+2dF:wDE< -0.78

r < -0.71WMAP+ACBAR+CBI+2dF+infl.cons.rel.:

Reionisation

TCl/exp(-2?T,TE,E,BCl

?'0.12

The Future CMB:

Imaging Cosmology

CMB Spectrum…

CMB Spectrum…Primordial Density Perts.: non-Gaussian?Reionization: Non-GaussianPrimordial GWsLensing: Non-Gaussian

Planck According T

o Dodelson & Hu 2003

True CMB…

WMAP CMB…

True CMB…

Planck CMB…

True CMB…

CMBpol CMB…

CMB Corrupted

The Future CMB: Foreground Removal

CMB Corrupted

Fast Independent Component Analysis (FastICA)x=As+n, find W such thatWx=s+WnFastICA main loop: construct W row by rowChoose initial wUpdate throughwnewTwE(g’(wx))Comparewithw.Ifnotconvergedgo

back;ifconvergedstartupnextrow,keepingorthogonalityT=E[xg(wx)]-

FastICA on Planck SimulationsMaino et al. 2002

INOUTPlanck nominal performance

Component Separation in Polarisation

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

FastICA and COBE

?

?

?

?PerformMonteCarlosimulationstoquantifytheeffectofnoisedistributionBuild Criteria to Identify Physical Components in a Heavy Noise EnviromentAdd priors to check quality and consistency of the resultsExtractCosmologicalParametersandForegroundScienceMaino et al. 2003

FastICA & COBE

Maino et al. 2003BlindNon-Blind

The Future CMB: Imaging Physical Cosmology

Primordial non-Gaussianity

Y22=YL+fNL(YL-<YL>)

-110The simplest inflationary scenario predicts fNL'

WMAP: -58< fNL< -134

Planck forecast in progress

Liguori et al. 2003

Imaging Reionization…

9.5 arcminutes

Normal Stars in proto-galaxies20% escape fractionCMB scattering on moving electornsdT/Ttcompatible with WMAP

Salvaterra, Ferrara et al. 2004 in prep.

Dark Energy & CMB: beyond Cl s

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

CMB bispectrum

Q(?) ′dT(?)/T

alm=sQ(?)Ylm(?)d?

Blm l`m`l``m``=almal`m`al``m``

l`l``Bl l`l``=?m m` m``(mm`m``) almlal`m`al``m``ll`l``

CMB bispectrum & Structure Formation < Blm l`m`l``m`` >=0

m m`m`` < Bll`l``>?

CMB bispectrum & Structure Formation Q(?) =Qlss(? +d?)+QISW 'Qlss(?)+rQlss(?)¢d?

QISW(?)=2s0decdr dY(r,?)/dh

d? =2s0decdr[(r-rdec)/rdecr]Y(r,?)

<Bl l`l``>=[(2l+1)(2l`+1)(2l``+1)/16p]1/2(0l0l`0``l``) ¢

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

3D(z)=[r(zdec)-r(z)]/r(zdec)r(z)Q(l)=s0dec D(z) F(z) dzF(z)=dPY/dz|k=l/r(z)

PY=(3?m0 /2)2(H0/ck)4P(k,z)(1+z)2P(k,z)=AknT(k,z)2

Hu & White 1997, Bartelmann & Schneider 2001,

Komatsu & Spergel 2001, Verde & Spergel 2002

CMB bispectrum & Structure Formation

CMB bispectrum line of sight chronology

:super-horizon scales in a flat

Y/dh=0, dQ/dz!0

Ydecaying linearly, dQ/dz>0

acceleration,changeincosmic

ofstate,Ydecayinglinearly,dQ/dz>0

Ygrows, dQ/dz<0

!0

CMB bispectrum line of sight distribution

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

CMB bispectrum & Dark Energy Quintessence reference modelsSUGRA

RP

CMB bispectrum & Dark Energy

Ma et al. 1999,

Smith et al. 2003

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

CMB bispectrum & Dark Energy

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

CMB bispectrum & Dark Energy

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

CMB bispectrum & Dark Energy

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

CMB bispectrum & Structure Formation < Blm l`m`l``m`` >=0< Blm l`m`l``m`` >?0 decd? =2s0dr[(r-rdec)/rdecr]Y(r,?)

Giovi, Liguori et al. 2004, in preparation

Continua…?????

?Component Separation & WMAP…Impact of CMB bispectrum on Planck Cosmological Parameter Estimation…Weakly Lensed CMB Templates, Semi-analytical…Weakly Lensed CMB Templates, Numerical…Weakly Lensed CMB Templates, Polarisation…Weakly Lensed CMB Templates, Comparison with Gravitational Wave Signal…

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