Inflation, Gravity Waves and the CMB

1
Inflation, Gravity Waves and the CMB

• Dick Bond

LCDM pre-WMAP3 cf. post-WMAP3 - all
observations are broadly consistent with a simple
6 basic parameter model of Gaussian curvature
(adiabatic) fluctuations - so far no need for
gravity waves, a running scalar index,
subdominant isocurvature fluctuations, etc.
Range covered CMB out to horizon ( 10-4
Mpc-1), through to 1 Mpc-1 LSS, higher k,
possible deviations exist. goal - Information
Compression to Fundamental parameters,
phenomenological parameters, nuisance parameters
Bayesian framework conditional probabilities,
Priors/Measure sensitivity, Theory Priors,
Baroqueness/Naturalness/Taste Priors,
Anthropic/Environmental/broad-brush-data Priors.
probability landscapes, statistical Inflation,
statistics of the cosmic web, both observed and
theoretical. mode functions, collective and other
coordinates. tis all statistical physics.
Dynamical Resolution Trajectories/Histories,
for Inflation then now
2
Topics
Inflation Histories
subdominant phenomena
Secondary Anisotropies
Foregrounds
Polarization of the CMB, Gravity Waves
Non-Gaussianity
Dark Energy Histories
3
the nonlinear COSMIC WEB

• Primary Anisotropies
• Tightly coupled Photon-Baryon fluid oscillations
• Linear regime of perturbations
• Gravitational redshifting

• Secondary Anisotropies
• Non-Linear Evolution
• Weak Lensing
• Thermal and Kinetic SZ effect
• Etc.

Decoupling LSS
reionization
19 Mpc
14Gyrs
10Gyrs
today
4
Parameters of Cosmic Structure Formation
Period of inflationary expansion, quantum noise ?
metric perturb.
Density of Baryonic Matter
Spectral index of primordial scalar
(compressional) perturbations
Spectral index of primordial tensor (Gravity
Waves) perturbations
Density of non-interacting Dark Matter
Cosmological Constant
Optical Depth to Last Scattering Surface When did
stars reionize the universe?
Scalar Amplitude
Tensor Amplitude
What is the Background curvature of the
universe?

• Inflation ? predicts nearly scale invariant
  scalar perturbations and background of
  gravitational waves
• Passive/adiabatic/coherent/gaussian perturbations
• Nice linear regime
• Boltzman equation Einstein equations to
  describe the LSS

closed
flat
open
5
WMAP3 thermodynamic CMB temperature fluctuations
Like a 2D Fourier transform, wavenumber Q L
1/2
6
Temperature maps
V band
year 1(pub)
year 3
year 3 - year 1
W band
7
WMAP3 cf. WMAP1
8
TT, EE, BB, TE, TB, EB Angular Power Spectra
9
WMAP3 sees 3rd pk, B03 sees 4th
10
CBI combined TT sees 5th pk (Dec05,Mar06)
11
Quiet2
CBI pol to Apr05
Bicep
CBI2 to Apr07
(1000 HEMTs) Chile
QUaD
Quiet1
Acbar to Jan06
SCUBA2
CBI2
APEX
Spider
(12000 bolometers)
(400 bolometers) Chile
SZA
JCMT, Hawaii
(1856 bolometer LDB)
(Interferometer) California
ACT
Clover
(3000 bolometers) Chile
2017
Boom03
CMBpol
2003
2005
2007
2004
2006
2008
SPT
WMAP ongoing to 2009
ALMA
(1000 bolometers) South Pole
(Interferometer) Chile
DASI
Polarbear
Planck
(300 bolometers) California
CAPMAP
AMI
(84 bolometers) HEMTs L2
GBT
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CMB/LSS Phenomenology

• Dalal
• Dore
• Kesden
• MacTavish
• Pfrommer
• Shirokov

• CITA/CIAR here
• Bond
• Contaldi
• Lewis
• Sievers
• Pen
• McDonald
• Majumdar
• Nolta
• Iliev
• Kofman
• Vaudrevange
• Huang
• El Zant

• CITA/CIAR there
• Mivelle-Deschenes (IAS)
• Pogosyan (U of Alberta)
• Prunet (IAP)
• Myers (NRAO)
• Holder (McGill)
• Hoekstra (UVictoria)
• van Waerbeke (UBC)

• UofT here
• Netterfield
• MacTavish
• Carlberg
• Yee

• Exptal/Analysis/Phenomenology Teams here
  there
• Boomerang03
• Cosmic Background Imager
• Acbar
• WMAP (Nolta, Dore)
• CFHTLS WeakLens
• CFHTLS - Supernovae
• RCS2 (RCS1 Virmos)

Parameter datasets CMBall_pol SDSS P(k), 2dF
P(k) Weak lens (Virmos/RCS1 CFHTLS, RCS2) Lya
forest (SDSS) SN1a gold (157, 9 zgt1),
CFHT futures ACT SZ/opt, Spider. Planck,
21(1z)cm
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Parameters Priors of the Cosmic Standard
Model Even for minimal Gaussian
inflaton-generated fluctuations 17, here 6222
2
EARLY UNIVERSE power spectra, non-Gaussian
3,4,.. Point, topology
Asns At nt Aiso niso
_at_normalization point kn Features functions(k)
krun, kBSI
Wbh2 Wch2 Wnh2 Werh2
CMB PHOTON TRANSPORT_at_Decoupling
Wk WL (WQ wQ)
TRANSPORT_at_ Late Time ISW Effect GEOMETRY
ksound,dec, kdamp,dec, kmn
Near Parameter Degeneracies in CMB need LSS,
SN1a,nclusters,
Map Lsound,dec R(z_at_dec) ksound,dec, want
TOMOGRAPHY R(z)
e.g., R(z) angular-diameter-distance. BROKEN by
ISW. SN1a (RL(z) luminosity distance). z-surveys
Acoustic peaks (z). Abundances Volume(z),
perturbation growth rate (z).
tC
zreh
GASTROPHYSICS Compton Depth from Reionization
redshift
s82 h Wm Wb
LSS kHeq aka G
ksound,dec, kmn
14
What have we learned from the CMB so far?
--gt Consistent with tilted ?CDM model
--gt Spectral index ns ? 1!
--gt Baryons, radiation, neutrinos, cold
dark matter
--gt Dark energy in form of cosmological
constant ?
--gt Initial scalar, adiabatic perturbation
gives rise to acoustic oscillations
--gt Spatially flat geometry
--gt Agreement of all data sets (including
NEW WMAP and NEW 2dF) 1s level
15
CBI combined TT data (Dec05,Mar06)
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s8 Tension of WMAP3 cf. WMAP1
With CBI excess as SZ s8 for Bond et al. SZ
template 1.000.1, for Komatsu Seljak SZ
template 0.930.1. Komatsu Seljak
consistent with latest Chandra M-T relation
(Vikhlinin et al.). Latest XMM M-T (Arnaud et
al.) 50 higher than Chandra s80.85?
Doesnt include errors from non-Gaussianity of
clusters, uncertainty in faint source counts
(35 increase)
Tension with weak lensing
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CBI combined TT data
s8 .77 - .04 , .72-.05 (GW), .80 .03
(GWLSS) s8 .80 - .04 run (-0.05 - .025)
CSLS05 s8 0.86 - .05 if Wm 0.3 -
.05 Virmos-Descartes05 s8 0.83 - .07 RCS1
lens s8 0.85 - .07 RCS1 optical s8 1.05 -
.14 (prelim) Xray version s8 0.78 - larger
- MacTavish etal05 B03 version s8 0.85 - .05
2dF version s8 0.83 - .04 2dF version bg(L)
s8 0.92 - .04
Van Waerbeke etal, CASCA06, slight drop because
of non-Gaussian error inclusion
18
CBI2 bigdish upgrade June2006 GBT for sources
Caltech, NRAO, Oxford, CITA, Imperial by about
Feb07
s8
.85 - .05 CMBallLSS
SZE Secondary
CMB Primary
s8SZ
1.0 - .09 SZ CMBallLSSCBIt
.82 - .11 (CBItBIMAAcbar)WMAP1
s87
on the excess as SZ also SZA (consistent with
s81), APEX, ACT, SPT (Acbar)
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E and B mode patterns
Blue Red -
local Q
local U
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Polarization maps
K band
V band
Ka band
W band
Q band

• Color code P(Q2U2)1/2 smoothed with a 2o fwhm
• Direction shown for S/N gt 1

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CBI Dataset

• CBI observes 4 patches of sky 3 mosaics 1
  deep strip
• Pointings in each area separated by 45. Mosaic
  6x6 pointings, for 4.5o2, deep strip 6x1.
• Lose 1 mode per strip to ground.
• 2.5 years of data, Aug 02 Apr 05.

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E/B Deep Stripsignal maps cf. raw
Variance of E in raw data 2.45 times B (llt1000).
B consistent with noise. E,B mixing 5 in power.
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Polarization EE2.5 yrs of CBI, Boom03,DASI,WMAP3
(CBI04, DASI04, CAPmap04 _at_ COSMO04) DASI02 EE
WMAP306
Phenomenological parameter analysis Lsound_at_dec
vs As CBIB03DASI EE,TE cf. CMB TT
Sievers et al. astro-ph/0509203
Montroy et al. astro-ph/0509203
Readhead et al. astro-ph/0409569
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Does TT Predict EE? (incl wmap3 TT data)
EE is in excellent agreement with prediction from
TT.
pattern shift parameter 1.002 - 0.0043
WMAP1CBIDASIB03 TT/TE/EE Evolution Jan00 11
Jan02 1.2 Jan03 0.9 Mar03 0.4 EE 0.973
- 0.033, phase check of CBI EE cf. TT pk/dip
locales amp EETE 0.997 - 0.018 CBIB03DASI
(amp0.93-0.09)
25
Physical cosmology Probes of Early Late
universe physics CMB polarization frontier
(B-futures)
Inflation Then Trajectories Primordial Power
Spectrum Constraints
26
The Parameters of Cosmic Structure Formation
27
SPIDER
Balloon-borne
stray light baffle
antenna-coupled bolometer array
2312 detectors cooled to 250 mK
Each pixel has two orthogonally polarized antenna
Spins in azimuth, fixed elevation (45º)
Six telescopes, five Frequencies 70 to 300 GHz
solar arrays
cryostat
1º resolution at 100GHz
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SPIDER Tensor Signal

• Simulation of large scale polarization signal
• This is what we are after!!

No Tensor
Tensor
http//www.astro.caltech.edu/lgg/spider_front.htm
29
forecast Planck2.5 100143 Spider10d 95150
Synchrotron poln lt .004 ?? Dust poln lt 0.1
?? Template removals from multi-frequency data
30
forecast Planck2.5 100143 Spider10d 95150
GW/scalar curvature current from CMBLSS r lt
0.6 or lt 0.3 95 CL good shot at 0.02 95 CL
with BB polarization (- .02 PL2.5Spider) BUT
fgnds/systematics??
31
tensor (gravity wave) power to curvature power,
r, a direct measure of e (q1), qdeceleration
parameter during inflation q (ln Ha) may be
highly complex (scanning inflation
trajectories) many inflaton potentials give the
same curvature power spectrum, but the degeneracy
is broken if gravity waves are measured (q1)
0 is possible - low energy scale inflation
upper limit only Very very difficult to get at
this with direct gravity wave detectors even in
our dreams Response of the CMB photons to the
gravitational wave background leads to a unique
signature within the CMB at large angular scales
of these GW and at a detectable level. Detecting
these B-modes is the new holy grail of CMB
science. Inflation prior on e only 0 to 1
restriction, lt 0 supercritical possible
GW/scalar curvature current from CMBLSS r lt
0.7 or lt 0.36 95 CL good shot at 0.02 95 CL
with BB polarization (- .02 PL2.5Spider), .01
target BUT fgnds/systematics?? But r-spectrum.
But low energy inflation
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Potential of the Hybrid D3/D7 Inflation Model
String Theory Landscape Inflation
Phenomenology for CMBLSS
running index as simplest breaking, radically
broken scale invariance, 2-field inflation,
isocurvatures, Cosmic strings/defects,
compactification topology, other baroque
add-ons. subdominant String/Mtheory-motivated,
extra dimensions, brane-ology, reflowering of
inflaton/isocon models (includes curvaton),
modified kinetic energies, k-essence,
Dirac-Born-Infeld sqrt(1-momentum2), DBI in
the Sky Silverstein etal 2004, etc.
f fperp
KKLT, KKLMMT
any acceleration trajectory will do?? q (ln
Ha) H(ln a,) V(phi,) Measure?? anti-baroque
prior
14 std inflation parameters
many many more e.g. blind search for patterns
in the primordial power spectrum
33
Kahler/axion moduli Inflation Conton Quevedo
hep-th/0509012
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Bond, Contaldi, Kofman, Vaudrevange 06
N-ln(a/ae), k Ha , e (1q), e dlnH/dN, Ps
H2 /e, Pt H2
V(f) MPl2 H2 (1-e/3) , f inflaton
collective coordinate, d f - sqrt(e)dN
36
Beyond P(k) Inflationary trajectories
HJ expand about uniform acceleration, 1q, V
and power spectra are derived
37
Trajectories cf. WMAP1B03CBIDASIVSAAcbarMaxi
ma SDSS 2dF Chebyshev 7 10 H(N) and RG Flow
7
10
38
r(ln a)/16 -nt/2 /(1-nt/2) small (1q)
small
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Displaying Trajectory constraints If Gaussian
likelihood, compute c2 where 68 probability, and
follow the ordered trajectories to ln L/Lm - c2
/2, displaying a uniformly sampled subset.
Errors at nodal points in trajectory
coefficients can also be displayed.
Chebyshev nodal modes (order 3, 5, 15) Chebyshev
modes are linear combinations ? Fourier at high
order
40
lnPs Pt (nodal 2 and 1) 4 params cf lnPs (nodal
2 and 0) 4 params reconstructed from CMBLSS
data using Chebyshev nodal point expansion MCMC
Power law scalar and constant tensor 4
params effective r-prior makes the limit
stringent r .082- .08 (lt.22)
Usual basic 6 parameter case Power law scalar and
no tensor r 0
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lnPs Pt (nodal 2 and 1) 4 params cf Ps Pt
(nodal 5 and 5) 4 params reconstructed from
CMBLSS data using Chebyshev nodal point
expansion MCMC
Power law scalar and constant tensor 4
params effective r-prior makes the limit
stringent r .082- .08 (lt.22)
no self consistency order 5 in scalar and tensor
power r .21- .17 (lt.53)
42
lnPs Pt (nodal 2 and 1) 4 params cf e (ln Ha)
nodal 2 amp 4 params reconstructed from
CMBLSS data using Chebyshev nodal point
expansion MCMC
Power law scalar and constant tensor 4 cosmic
7 effective r-prior makes the limit stringent r
.082- .08 (lt.22)
The self consistent running acceleration 7
parameter case ns .967- .02 nt -.021- .009
r .17- .07 (lt.32)
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e (ln Ha) order 1 amp 4 params cf. order 2
reconstructed from CMBLSS data using Chebyshev
nodal point expansion MCMC
The self consistent uniform acceleration 6
parameter case ns .978- .007 nt -.022- .007
r .17- .05 (lt. 28)
The self consistent running acceleration 7
parameter case ns .967- .02 nt -.021- .009
r .17- .07 (lt.32)
44
e (ln Ha) order 3 amp 4 params cf. order 2
reconstructed from CMBLSS data using Chebyshev
nodal point expansion MCMC
The self consistent running acceleration 8
parameter case ns .81- .05 nt -.043- .02
r .35- .13 (lt.54)
The self consistent running acceleration 7
parameter case ns .967 - .02 nt -.021- .009
r .17- .07 (lt.32)
45
e (ln Ha) order 10 amp 4 params cf. order 2
reconstructed from CMBLSS data using Chebyshev
nodal point expansion MCMC
The self consistent running acceleration 7
parameter case ns .967- .02 nt -.021- .009
r .17- .07 (lt.32)
The self consistent running acceleration 15
parameter case ns .90- .09 nt -.086- .01
r .69- .08 (lt.82)
514 case is in between
e1q Spider may get gt 0.001 Planck may get gt
0.002
46
e(ln k) reconstructed from CMBLSS data using
Chebyshev expansions (uniform order 15 nodal
point) cf. (monotonic order 15 nodal point) and
Markov Chain Monte Carlo methods. T/S consistency
function imposed..
V MPl2 H2 (1-e/3)/(8p/3)
Near critical 1q Low energy inflation
gentle braking approach to preheating
wide open braking approach to preheating
47
V(f) reconstructed from CMBLSS data using
Chebyshev expansions (uniform order 15 nodal
point) cf. (uniform order 3 nodal point) cf.
(monotonic order 15 nodal point) and Markov Chain
Monte Carlo methods...
gentle braking approach to preheating
wide open braking approach to preheating
V MPl2 H2 (1-e/3)/(8p/3)
48
CL TT BB for e (ln Ha) inflation trajectories
reconstructed from CMBLSS data using Chebyshev
nodal point expansion (order 15) MCMC
49
CL TT BB for e (ln Ha) monotonic inflation
trajectories reconstructed from CMBLSS data
using Chebyshev nodal point expansion (order 15)
MCMC
50
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summary
The basic 6 parameter with no allowed GW fits all
of the data OK Usual GW limits from adding r with
fixed GW spectrum, no consistency (7
params) Adding minimal consistency does not make
that much difference (7 params) r constraints
come from relating high k region of s8 to low k
region of GW CL Prior probabilities on the
inflation trajectories are crucial and cannot be
decided at this time. Philosophy here is to be as
wide open and least prejudiced about inflation as
possible Complexity of trajectories could come
out of many moduli string models Uniform prior in
e nodal point Chebyshev coefficients Cheb
coefficients give similar results, more GW
allowed as the parameter space opens up. In
particular scalar power downturns at low L if
there is freedom in the mode expansion to do
this. Adds GW to compensate. Monotonic uniform
prior in e drives us to low energy inflation and
low gravity wave content. Even with low energy
inflation prospects are good with Spider and even
Planck to detect the B-mode of polarization. Both
have strong Canadian roles.
52
CL EE TE for e (ln Ha) inflation trajectories
reconstructed from CMBLSS data using Chebyshev
nodal point expansion (order 15) MCMC
53
CL EE TE for e (ln Ha) monotonic trajectories
reconstructed from CMBLSS data using Chebyshev
nodal point expansion (order 15) MCMC
54
Kahler/axion moduli Inflation Conton Quevedo
hep-th/0509012
55
(No Transcript)
56
(No Transcript)
57
(No Transcript)
58
How will SPIDER measure B-modes?
--gt New antenna-coupled bolometer array
technology
--gt Each pixel has two orthogonally polarized
antenna
--gt Single 145 GHz detector sensitivity
100 ?KCMBs1/2
--gt No feeds, low mass, close- packed
lots of detectors
59
H (ln Ha) / (10-5 mP) inflation trajectory
reconstructed from CMBLSS data using Chebyshev
expansion (order 10) MCMC.
60
Ps, Pt (ln Ha) / (10-5 mP) inflation trajectory
reconstructed from CMBLSS data using Chebyshev
nodal expansion (order 3 and 2) MCMC.
Expand scalar power in slope and running index
Tensor power in slope (not usual to do both, and
not usual to allow tensor slope to be
unslaved) Parameters come out OK cf. more
restrictive treatments Nodal point uniform prior
implies different measures on r, n_t, n_s,
dn_s/dlnk than usual uniform cf. isocurvature
pivots cf. r_is n_is
61
The Parameters of Cosmic Structure Formation
WMAP3 WMAP3CBIcombinedTTCBIpol CMBall
Boom03polDASIpol VSAMaximaWMAP3CBIcombinedTT
CBIpol
62
The Parameters of Cosmic Structure Formation
pre-WMAP3
Cosmic Numerology pre-WMAP3 CMBall LSS, stable
consistent pre-WMAP1 post-WMAP1 (BCP03),
Jun03 data (BCLP04), CMBallCBIpol04,
CMBallBoom03LSS Jul21 05, CMBallAcbar
Jul05 LSS2dF, SDSS (weak lensing, cluster
abundances) also HST, SN1a
As 22 - 3 x 10-10 ns .95 - .02 (.97 - .02
with tensor) (- .004 PL1) rAt / As lt 0.36 95
CL (- .02 PL2.5Spider) nt consistency
relation dns /dln k -.07 - .04 to -.05 - .03
(- .005 P1) -.002 - .01
(Lya McDonald etal 04) (Aiso / As lt 0.3 large
scale, lt 3 small scale niso 1.1-.6)
63
The Parameters of Cosmic Structure Formation
post-WMAP3
Cosmic Numerology WMAP3CMBallpol (incl
CBITTpol) WMAP3 x
As 22 - 2 x 10-10 ns .95 - .015 (.99 .02
-.04 with tensor) rAt / As lt 0.28 95 CL lt.55
wmap3, lt1.5 run nt consistency relation dns /dln
k -.055 - .025 to -.06 - .03
-.10 - .05 (wmap3tensors)
64
The Parameters of Cosmic Structure Formation
pre-WMAP3
Wbh2 .0227 - .0008 (.0002 PL1) Wch2 .126 -
.007 (.0015 PL1) Wnh2 Sm/94 ev lt .1 if equal
mass (m lt 0.4 ev, bias info lt 0.16 ev Boom03,
Lya lt 0.18 ev cf. 3 ev H3 Dm2
8x10-5,2.5x10-3) Wk -.03 - .02 WL .70 -
.03 (wQ lt -0.75 95 .94 - .10 incl SN)
Werh2 1.68 Wgh2 4.1x 10-5 tC .11 - .05
(.005 PL1)
derived
s8 .85 - .05 h .70 - .03 Wm .30 - .03 Wb
.045 - zreh 13 - 4
65
The Parameters of Cosmic Structure Formation
post-WMAP3
Wbh2 .0222 - .0007 Wch2 .107 - .007 Wnh2
Sm/94 ev lt .1 if equal mass (m lt bias info
lt 0.23 ev cf. 3 ev H3 Dm2 8x10-5,2.5x10-3) Wk
-.02 - .02 (HST) WL .75 - .03 (wQ lt
-0.83 95 .97 - .09 incl SN)
Werh2 1.68 Wgh2 4.1x 10-5 tC .087 - .03
(.005 PL1)
derived
s8 .77 - .04 h .73 - .03 Wm .25 - .03
Wb .045 - zreh 11 - 3
66
Polarization EE WMAP3 sees 1st pk, part of 2nd,
DASI sees 2nd pk, B03 sees 2nd and 3rd , CBI sees
3rd, 4th, 5th
Sievers et al. astro-ph/0509203
Montroy et al. astro-ph/0509203
Readhead et al. astro-ph/0409569
67
CBI Polarization Power Spectra Sept 05
CBI8 poln detection Science 306,836 CBI9
Astro-ph/0509203 54 10s

• 2nd measurement of E-type CMB polarization
  spectrum, best so far (DASI02, CBI04, DASI04,
  CAPmap04 _at_ COSMO04) WMAP1 03 TE, B03, CBI9,
  WMAP3 -soon

Red os Science04 Blue xs CBI9 Black best fit
Magenta WMAPext Black s predicted

• 7-band spectra (Dl 150 for 600ltllt1200)
• Polarization data consistent with WMAPext model
  (TT from WMAP, Acbar, 0001 CBI) best-fit from
  TT

68
Lsound_at_dec vs As CBIB03DASI EE,TE cf. CMB
TT
pattern shift parameter 1.002 - 0.0043
WMAP1CBIDASIB03 TT/TE/EE Evolution Jan00 11
Jan02 1.2 Jan03 0.9 Mar03 0.4 EE 0.973
- 0.033, phase check of CBI EE cf. TT pk/dip
locales amp EETE 0.997 - 0.018 CBIB03DASI
(amp0.93-0.09)
69
Does TT Predict EE? (incl wmap3 TT data)
EE is in excellent agreement with prediction from
TT.
Take the same TT curvature plot from before and
then show its EE spectrum against the data.
There are 0 free parameters in the EE model yet
it agrees extremely well with the data (in fact
?2 is a bit too good - but not unreasonably so).
EE-only measures the angular scale of the CMB to
3, and gets the same answer as TT. Other
parameters (dark matter, baryons) from EE agree
as well, but precision isnt great yet (30-40
accuracies, typically).
70
CBI 20002001, WMAP, ACBAR, BIMA
Readhead et al. ApJ, 609, 498 (2004)
s8
.85 - .05 CMBallLSS
SZE Secondary
CMB Primary
.82 - .11
s87
Kuo et al. (2005, in prep)
Boom03 Acbar05 very nice TT, Dec05. parameters
new excess analysis as SZ
71
WMAP3 WMAP3CBIcombinedTTCBIpol CMBall
Boom03polDASIpol VSAMaximaWMAP3CBIcombinedTT
CBIpol
The Parameters of Cosmic Structure Formation
72
CBI combined TT data
s8SZ 0.814 - .12 cf. s8 0.89 - .07 (cf.
0.89 - .04 slaved) cbibimaacbar (wmap1boom03
vsamaxima) s8SZ 0.96 - .12 cf. s8 0.87 -
.07 (cf. 0.92 - .06 slaved) cbi (wmap1boom03
vsamaxima) NO SZ CORRECTION 0.92 - .08
(cbiacbarwmap1boom03vsamaxima)
s8 .77 - .04 , .79 .04-.07 (GW) s8 .81 -
.04 run (0.32 - .06)
CSLS05 s8 0.86 - .05 if Wm 0.3 -
.05 Virmos-Descartes05 s8 0.83 - .07 RCS1
lens s8 0.85 - .07 RCS1 optical s8 1.05 -
.14 (prelim) Xray version s8 0.78 - larger
- MacTavish etal05 B03 version s8 0.85 - .05
2dF version s8 0.83 - .04 2dF version bg(L)
s8 0.92 - .04