WMAP final nine-year results David Larson Johns Hopkins University - - PowerPoint PPT Presentation

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WMAP final nine-year results David Larson Johns Hopkins University - - PowerPoint PPT Presentation

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WMAP final nine-year results David Larson Johns Hopkins University June 10, 2013 OIST, Okinawa, Japan Monday, June 10, 2013 WMAP Science Team Chuck Bennett (PI) Chris Barnes Steve Meyer Rachel Bean Mike Nolta Olivier Dor Nils Odegard

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WMAP final nine-year results

David Larson Johns Hopkins University June 10, 2013

OIST, Okinawa, Japan

Monday, June 10, 2013

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Chris Barnes Rachel Bean Olivier Doré Jo Dunkley Ben Gold Mike Greason Mark Halpern Bob Hill Gary Hinshaw Norm Jarosik Al Kogut Eiichiro Komatsu David Larson Michele Limon Steve Meyer Mike Nolta Nils Odegard Lyman Page Hiranya Peiris Kendrick Smith David Spergel Greg Tucker Licia Verde Janet Weiland Dave Wilkinson Ed Wollack Ned Wright

WMAP Science Team

Chuck Bennett (PI)

Monday, June 10, 2013

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WMAP took data for nine years

Launch: June 30, 2001 Data taking from L2: August 10, 2001 - August 10, 2010

Monday, June 10, 2013

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K1 23 GHz Ka1 33 GHz Q1, Q2 41 GHz V1, V2 61 GHz W1, W2, W3, W4 94 GHz

WMAP is differential to minimize systematic errors, with 10 differencing assemblies

map.gsfc.nasa.gov

Monday, June 10, 2013

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WMAP frequencies were chosen to surround maximum CMB to foreground ratio

Lines correspond to foregrounds

  • utside KQ85 and KQ75 masks

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KQ85 KQ75 Bennett et al. 2013

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WMAP scans feedhorn pairs across the sky

Bennett et al, 2003

This cross-linked pattern is for one hour of scanning

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Q band (41 GHz)

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Q band, with 3.3 mK dipole

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Q band, with 3.3 mK dipole, masked

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WMAP 1-hour scan

Dipole due to WMAPʼs motion around SSB (270 μK amplitude) not shown

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WMAP 1-hour scan

Dipole due to WMAPʼs motion around SSB (270 μK amplitude) not shown

Monday, June 10, 2013

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WMAP 1-hour scan

Dipole due to WMAPʼs motion around SSB (270 μK amplitude) not shown

Monday, June 10, 2013

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WMAP 1-hour scan

Dipole due to WMAPʼs motion around SSB (270 μK amplitude) not shown

Monday, June 10, 2013

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dipole gain anisotropy baseline intensity polarization Calibration (gain and baseline) iteratively fit using WMAP-velocity modulation of the dipole data

Hinshaw et al. (2009), Bennett et al. (2013)

Final absolute calibration accuracy is 0.2% Each of 10 DAs is independently calibrated

Monday, June 10, 2013

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Data is dropped during infrequent (~3x per year) L2 station keeping maneuvers

WMAP achieved 98.4% observing efficiency

  • ver the nine-year survey

Monday, June 10, 2013

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Beam estimation

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Based on 17 seasons of Nyquist sampled Jupiter observations, and physical mirror model fit to this data (two ~50 day seasons every ~400 days) High S/N region: binned data are used Low S/N region (< 0.25% of integrated response): model is used Full far-sidelobe treatment is included in data analysis, based on ground measurements, early flight moon observations, and analytic models Sidelobe effects are iteratively updated in the gain/baseline calibration: dipole: ΔTvi = ΔTv,main,i + ΔTv,side,i anisotropy: ΔTai = ΔTa,main,i + ΔTa,side,i

Monday, June 10, 2013

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New in WMAP9: an additional mapmaking process deconvolves beam asymmetry

Residual maps after subtracting circularly symmetric profiles Residuals are much smaller after symmetrization This is Tau A in K-band, a worst-case scenario Bennett et al, 2013

Monday, June 10, 2013

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K band, 23 GHz, temperature

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Ka band, 33 GHz, temperature

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Q band, 41 GHz, temperature

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V band, 61 GHz, temperature

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W band, 94 GHz, temperature

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K band, 23 GHz, polarization

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Ka band, 33 GHz, polarization

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Q band, 41 GHz, polarization

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V band, 61 GHz, polarization

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W band, 94 GHz, polarization

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Foreground results

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Bennett et al. 2013

WMAP band differences show foregrounds

Red = W - V is mostly dust Green = (K - Ka) - 1.7 (Q - W) is synchrotron and spinning dust Blue = Q - W is mostly free-free

Monday, June 10, 2013

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Bennett et al. 2013 ± 200 μK

The ILC removes most foregrounds

The ILC provides a region-by-region “Internal Linear Combination” of 5 band maps that minimizes the variance of each region. It keeps the CMB and some small linear combination of foregrounds that partially cancels the CMB fluctuations.

Monday, June 10, 2013

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An estimate of the CMB-foreground covariance error in the ILC

Color bar goes up to 66 μK = 1σ of CMB fluctuations This error is small for a large fraction

  • f the sky

Monday, June 10, 2013

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Bennett et al. 2013

χ2 > 10

Detailed foreground models

Frequencies fit: 0.408, 23, 33, 41, 61, 94 GHz

Monday, June 10, 2013

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WMAP 408 MHz Model 9 uses Strong et al. 2011 synchrotron model with -0.5 < Δβ < 0.5

This is a physical model (A step function works equally well for us)

β

Monday, June 10, 2013

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@ 40 GHz

Strong et al. βsynchrotron free-free βdust = 1.8 spinning dust 6 bands (Haslam+WMAP) 7 degrees of freedom

Bennett et al. 2013

Model 9 fits each pixel independently

Monday, June 10, 2013

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Degeneracies in the fit parameters make the model susceptible to noise

Since fits are independent between pixels, foreground reconstruction shows noise

For Model 9, Bennett et al. 2013

βsynch free-free synch SD SD peak therm dust SD peak SD free-free βsynch

Monday, June 10, 2013

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Cosmological Results

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New in WMAP9: an optimal C-1 estimator for the TT power spectrum, instead of MASTER C-1 MASTER

C-1 algorithm: Bennett et al. 2013 Smith et al. 2007 Bond et al. 1998 Tegmark et al. 1997 Hinshaw et al. 2013 7-17% reduction in σ2(Cl), depending on l

Monday, June 10, 2013

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7-17% reduction in σ2(Cl), depending on l Bennett et al. 2013

Optimal C-1 estimator reduces error bars

Most improvement is around l = 600 where S ~ N

Monday, June 10, 2013

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Nine years of WMAP data reduce the CMB-only allowed parameter space by a factor of 68,000

Ωbh2 = 0.02264 ± 0.00050 Ωch2 = 0.1138 ± 0.0045 ΩΛ = 0.721 ± 0.025 109Δ2R = 2.41 ± 0.10 ns = 0.972 ± 0.013 τ = 0.089 ± 0.014

Bennett et al. 2013 Comparison of sqrt(det(cov)) of a Markov chain using likelihood from “Last stand before WMAP” Wang et al, 2003 with WMAP9-only parameter chain

Monday, June 10, 2013

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Super-horizon adiabatic modes

TE spectrum is well fit with the same ΛCDM model

Bennett et al. 2013 Reionization

Monday, June 10, 2013

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EE spectrum: determines reionization optical depth

Bennett et al. 2013

BB spectrum

Monday, June 10, 2013

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WMAP measures an angle: location of first peak

WMAP measures this angle

  • n the sky

If the universe is flat (Euclidean), this lets us measure the distance to last scattering, which gives us the Hubble constant: H0 = 70.0 ± 2.2 km s-1 Mpc-1 (and dA above) If we measure the expansion of the universe (H0 = 73.8 ± 2.4), we find it is flat Ratio of first two peak heights gives the physical baryon density: Ωbh2 = 0.02264 ± 0.00050 Photon to baryon ratio modifies the speed of sound: cs = c / [3(1 + 3Ωb/4Ωr)]1/2 Baryons, photons, and FRW give time to last scattering. Integrating sound speed over this time gives the horizon. WMAP9+eCMB+BAO+H0:

Monday, June 10, 2013

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WMAP9 has a tight curvature-H0 degeneracy:

  • ne determines the other

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Bennett et al. 2013

axis

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5-year WMAP data, Komatsu et al, 2009

WMAP limits tensors mostly through TT

r = 10, τ = 0.050 r = 1.2, τ = 0.075 r = 0.2, τ = 0.080 WMAP9 only: r < 0.38 (95% CL)

Monday, June 10, 2013

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WMAP limits tensors mostly through TT

r < 0.13 (95% CL), ns = 0.9636 ± 0.0084 WMAP9+eCMB+BAO+H0 r < 0.17 (95% CL), ns = 0.970 ± 0.011 WMAP9+eCMB

Hinshaw et al, 2013

Monday, June 10, 2013

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WMAP does not detect bispectrum non-Gaussianity: fNL

fNLlocal = 37.2 ± 19.9 (Bennett et al, 2013) Expected to be 0.015, from ns measurements Can be created from a local perturbation: Weights squeezed triangles positively: k1 = k2 >> k3. fNLeq = 51 ± 136 Can be created by inflation models with non-canonical kinetic terms (i.e. Dirac-Born-Infeld) Weights equilateral triangles positively: k1 = k2 = k3. fNLorth = -245 ± 100 Can be created by a linear combination of higher derivative scalar-field interaction terms FNLorth mostly orthogonal to FNLlocal and FNLeq. Weights equilateral triangles positively, and squeezed and folded triangles negatively These are not all possible ways to search for a bispectrum Komatsu 2010

+

  • Monday, June 10, 2013
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Some key WMAP accomplishments

Inflation Superhorizon fluctuations directly observed in TE Primordial power spectrum ns < 1 (5σ) Curvature: |Ωk| < 0.0094 (95% CL) Fluctuations are adiabatic Limits on fNL Other ΛCDM model still works in 68,000x less parameter space Sum of light neutrino masses < 0.44 eV (95% CL) Neff = 3.84 ± 0.40 t0 = 13.772 ± 0.059 Gyr zreion = 10.1 ± 1.0 Geometric measurement of dark energy confirmed SNe Dark energy consistent with cosmological constant Helium fraction (measured by CMB) consistent with BBN

Monday, June 10, 2013

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Comparison to Planck

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W band, cleaned with Planck low frequency and dust (353 GHz) templates Full sky least squares fit Planck SMICA map 5ʼ resolution 12ʼ resolution

Monday, June 10, 2013

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Distribution of WMAP9 allowed flat ΛCDM models

Figure 6 (Hinshaw et al, 2013) contains SZ contribution

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±1σ

Monday, June 10, 2013

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Distribution of WMAP9 allowed flat ΛCDM models

Figure 6 (Hinshaw et al, 2013) SZ contribution removed ±1σ

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Planck data show the same structure

Planck data are systematically lower,

  • ver most of ell range

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Planck flat ΛCDM theory is also similar

Planck theory is systematically lower,

  • ver most of ell range

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Questions?

New in WMAP9: Beam deconvolved maps New physical full-sky foreground models Optimal C-1 power spectrum estimation

Monday, June 10, 2013