wmap 9-year results and cosmological implicationskomatsu/presentation/wmap9_paris.pdf · wmap...
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WMAP 9-Year Results and Cosmological Implications:
The Final ResultsEiichiro Komatsu (Max-Planck-Institut für Astrophysik)
17th Paris Cosmology Colloquium 2013Observatoire de Paris, July 24, 2013
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WMAP at Lagrange 2 (L2) PointJune 2001:
WMAP launched!
February 2003:The first-year data release
March 2006:The three-year data release
March 2008:The five-year data release
January 2010:The seven-year data release
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used to be
September 8, 2010:WMAP left L2
December 21, 2012:The final, nine-year data release
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WMAP Science Team
• C.L. Bennett
• G. Hinshaw
• N. Jarosik
• S.S. Meyer
• L. Page
• D.N. Spergel
• E.L. Wright
• M.R. Greason
• M. Halpern
• R.S. Hill
• A. Kogut
• M. Limon
• N. Odegard
• G.S. Tucker
• J. L.Weiland
• E.Wollack
• J. Dunkley
• B. Gold
• E. Komatsu
• D. Larson
• M.R. Nolta
• K.M. Smith
• C. Barnes
• R. Bean
• O. Dore
• H.V. Peiris
• L. Verde
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WMAP 9-Year Papers
• Bennett et al., “Final Maps and Results,” accepted for publication in ApJS, arXiv:1212.5225
• Hinshaw et al., “Cosmological Parameter Results,” accepted for publication in ApJS, arXiv:1212.5226
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9-year Science Highlights
• The effective number of relativistic species is consistent with three
• The joint constraint on the helium abundance and the number of relativistic species from CMB strongly supports Big Bang nucleosynthesis
• Single-field slow-roll inflation continues to be supported by the data, with much restricted range of the parameter space
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9-year temperature Cl
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7-year temperature Cl
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What changed?• An improved analysis! The error bar decreased by more
than expected for the number of years (9 vs 7). Why?
• We now use the optimal (minimum variance) estimator of the angular power spectrum.
• Previously, we estimated Cl for low-l (l<600) and high-l (l>600) separately. No weighting for low-l and inverse-noise-weighting for high-l.
• This results in a sub-optimal estimator near l~600.
• We now use the optimal (S+N)–1 weighting.8
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Vari
ance
(su
b-op
timal
) / V
aria
nce
(opt
imal
)
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9-year (sub-optimal) vs 9-year (optimal)
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Adding the small-scale CMB data
• Atacama Cosmology Telescope (ACT)
• a 6-m telescope in Chile, led by Lyman Page (Princeton)
• Cl from Das et al. (2011)
• South Pole Telescope (SPT)
• a 10-m telescope in South Pole, led by John Carlstrom (Chicago)
• Cl from Keisler et al. (2011); Reichardt et al. (2012)These data are not latest [Story et al. for SPT; Sievers et al. for ACT] 12
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South Pole Telescope (SPT)
Atacama Cosmology Telescope(ACT)
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1000
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Adding the small-scale CMB tends to prefer a lower power at high
multipoles than predicted by the WMAP-only fit (~1σ lower)
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The number of “neutrino” speciestotal radiation density:
photon density:
neutrino density:
neutrino+extra species:
where
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What the extra radiation species does
• Extra energy density increases the expansion rate at the decoupling epoch.
• Smaller sound horizon: peak shifts to the high l
• Large damping-scale-to-sound-horizon ratio, causing more Silk damping at high l
• Massless free-streaming particles have anisotropic stress, affecting modes which entered the horizon during radiation era.
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“Neutrinos” have anisotropic stress
• This changes metric perturbations as
0-0tr(i-j)
• This changes the early Integrated-Sachs-Wolfe effect (ISW)17
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Effect of helium on ClTT
• We measure the baryon number density, nb, from the 1st-to-2nd peak ratio.
• For a given nb, we can calculate the number density of electrons: ne=(1–Yp/2)nb.
• As helium recombined at z~1800, there were even fewer electrons at the decoupling epoch (z=1090): ne=(1–Yp)nb.
• More helium = Fewer electrons = Longer photon mean free path 1/(σTne) = Enhanced Silk damping
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Simultaneous Fit toHelium and Neff
=WMAP9+ACT+SPT
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Results consistent with the BBN prediction
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Implications for Inflation
• Two-point function analysis: the tensor-to-scalar ratio, r, and the primordial spectral tilt, ns
• Three-point function analysis: are fluctuations consistent with Gaussian?
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Assuming no tensor modes
• WMAP9 only: ns = 0.972 ± 0.013
• WMAP9+CMB: ns = 0.965 ± 0.010
• WMAP9+CMB+BAO: ns = 0.958 ± 0.008
• WMAP9+CMB+BAO+H0: ns = 0.961 ± 0.008
• Confirmed by Planck+WMAP9pol: ns = 0.960 ± 0.007
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WMAP 9-year results(Hinshaw, Larson, Komatsu, et al. 2012)
r<0.12 (95%CL)
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WMAP9+ACT+SPT
WMAP9+ACT+SPT+BAO+H0
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WMAP 9-year results(Hinshaw, Larson, Komatsu, et al. 2012)
Planck confirms our results
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Planck Collaboration XXII (2013)
r<0.12 (95%CL)
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Congratulations, Slava and Alexei!
July 11, 2013
ns~0.96 [Mukhanov & Chibisov 1981], now observed;
and the R2 inflation [Starobinsky 1980], continues to fit the data rather well
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R2 Inflation [Starobinsky 1980]
• This theory is conformally equivalent to a theory with a canonically normalized scalar field with a potential given by
where
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[very flat potential for large Ψ –> smaller r]
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ξφ2R [Futamase & Maeda1989]
• The predictions of this model for the tilt and tensor-to-scalar ratio are identical to R2 inflation! Komatsu & Futamase (1999) showed:
33• So, the tensor-to-scalar ratio is tiny.
~ 0.005
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Bispectrum
• Three-point function!
• Bζ(k1,k2,k3) = <ζk1ζk2ζk3> = (amplitude) x (2π)3δ(k1+k2+k3)F(k1,k2,k3)
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model-dependent function
k1
k2
k3
Primordial fluctuation ”fNL”
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MOST IMPORTANT
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Probing Inflation (3-point Function)• Inflation models predict that primordial fluctuations are very
close to Gaussian.
• In fact, ALL SINGLE-FIELD models predict a particular form of 3-point function to have the amplitude of fNL=0.02.
• Detection of fNL>1 would rule out ALL single-field models!
• No detection of 3-point functions of primordial curvature perturbations. The 68% CL limit is:
• fNL = 37 ± 20 (1σ)
• The WMAP data are consistent with the prediction of simple single-field inflation models: 1–ns≈r≈fNL 36
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Komatsu&Spergel (2001)
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Planck Result: fNL = 2.7 ± 5.8 (68%CL)
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Statistical Anisotropy• Is the power spectrum anisotropic?
• P(k) = P(|k|)[1+g*(cosθ)2]
• This makes shapes of temperature spots anisotropic on the sky.
• Statistically significant detection of g*
• Is this cosmological?
• The answer is no: the same (identical!) effect can be caused by ellipticity of beams
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This is coupled with the scan pattern
• WMAP scans the ecliptic poles many more times and from different orientations.
• Thus, the averaged beam is nearly circular in the poles.
• The ecliptic plane is scanned less frequently and from limited orientations.
• Thus, the averaged beam is more elliptical in the plane.
• This is exactly what the anisotropic power spectrum gives.
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Creating a map with a circular beam
• We create a map in which the elliptical beam shape is deconvolved. The resulting map has an effective circular beam.
• This map is not used for cosmology, but used for the analysis of foregrounds and statistical anisotropy.
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• A deconvolved image of a supernova remnant “Tau A” at 23 GHz
• Deconvolved image is more circular, as expected
• Deconvolved map does not show the anisotropic power spectrum anymore!
-5 5
Beam Sym. Map Residuals
-5 5
Normal Map Residuals
0 100
Beam Sym. Map
0 100
mK
mK
mK
mK
Normal Map
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a”
Summary• The minimal, 6-parameter ΛCDM model continues to
describe all the data we have
• No significant deviation from the minimal model
• Rather stringent constraints on inflation models
• Strong support for Big Bang nucleosynthesis with the standard effective number of neutrino species
• Anisotropic power spectrum is due to elliptical beams
...“(Hinshaw et al. 2012)
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