Gary Hinshaw NASA/GSFC

From Quantum to Cosmos, Airlie Center VA, July 8 2008

5-year Results from WMAP5-year Results from WMAP with a Glimpse Ahead with a Glimpse Ahead

WMAP MissionWMAP Mission

WMAP’S PURPOSE –

To make a detailed full-sky map of the CMB radiation anisotropy (temperature and polarization) to constrain the cosmology of our universe.

W = WilkinsonW = Wilkinson

WMAP Science TeamWMAP Science Team

WMAP’s Differential Receivers*WMAP’s Differential Receivers*

10 “Differencing Assemblies”

4 @ 94 GHz W-band

2 @ 61 GHz V-band

2 @ 41 GHz Q-band

1 @ 33 GHz Ka-band

1 @ 23 GHz K-band

*based on HEMT design of M. Pospieszalski

WMAP LaunchWMAP Launch

June 30, 2001 at 3:47 EDT

Delta II Model 7425-10Delta Launch Number 286 Star-48 third stage motor Cape Canaveral Air Force StationPad SLC-17B

WMAP at L2WMAP at L2

WMAP at L2WMAP at L2

Taken with ESO 2.2 m telescope, La Silla Chile, for GAIA optical tracking test.

3 images (R,G.B) taken a few minutes apart, V=19.4.

WMAP Sky CoverageWMAP Sky Coverage

Not to scale:Earth — L2 distance is 1% of Sun — Earth Distance

Earth

Sun

MAP at L2

1 Day

3 Months

6 Months - full sky coverage

129 sec. (0.464rpm) Spin

22.5° half-angle1 hour precession cone

A-side line of site

B-side line of site

MAP990159

5-year Temperature Maps5-year Temperature Maps

5-year Polarization Maps5-year Polarization Maps

5-year Absolute Calibration5-year Absolute Calibration

New dipole fitting technique yields absolute gain accuracy of New dipole fitting technique yields absolute gain accuracy of <0.2% (difference between red and black curves).<0.2% (difference between red and black curves).

5-year Beam Calibration5-year Beam Calibration

Major effort to model beam response down to -44 dB allows us to model Major effort to model beam response down to -44 dB allows us to model PSF response with factor of ~2 improvement in accuracy. (Hill et al.)PSF response with factor of ~2 improvement in accuracy. (Hill et al.)

Jupiter data Physical model ResidualJupiter data Physical model Residual

A sideA side

B sideB side

3-year Power Spectrum - TT3-year Power Spectrum - TT

5-year Power Spectrum - TT5-year Power Spectrum - TT

Important DatesImportant Dates

Inflation – initial conditions: A, r, ns

Dark ages → first stars – polarization: τ

Plasma epoch – matter, radiation content: Ωb, Ωc

Large scale structure – dark energy: ΩΛ, σ8

5-year 5-year ΛΛCDM ParametersCDM Parameters

Blue curves/contours – 5-year data

Grey curves/contours – 3-year data

Biggest improvements in:

Optical depth, τ

Amplitude of fluctuations @ 8 Mpc, σ8

Matter densities, Ωbh2, Ωch2

TE EE

Was reionization a complex process?

Low-l TE and EE polarization power spectra can distinguish between different ionization histories.

Plots show mean TE, EE spectra for range of reionization histories.

Reionization - IReionization - I

Reionization - IIReionization - II

Improved polarization data improves measurement of optical depth and/or reionization redshift. Also begin to probe 2nd reionization parameter.

The bulk of the reionization had to occur at z>6, thus it had to be an extended process.

Cosmic Neutrino BackgroundCosmic Neutrino Background

Evidence for the cosmic neutrino background, “would provide the most dramatic possible confirmation of the standard model of the early universe”

The First Three Minutes Steven Weinberg 1977On seeing evidence for the cosmic neutrino background

New limits on gravitational wave amplitude, r<0.2.

Information still largely comes from shape of TT spectrum.

Testing Inflation - ITesting Inflation - I

“Named” inflation models are currently being put to the test.

Many of the models predict an observable gravitational wave background (via the CMB B-mode polarization).

Testing Inflation - IITesting Inflation - II

Future WMAP OperationsFuture WMAP Operations

WMAP is nearing 7 years at L2 and has been approved for 2 final years of operation.

What important questions will more WMAP data help address?

• Reionization - was reionization an extended process? Was the universe partially reionized at z = 20 or 30?

• Dark Energy - upcoming dark energy experiments will be limited by WMAP cosmological parameter uncertainties. Additional WMAP data will improve these uncertainties.

• Physics of Inflation - primordial gravity waves, primordial non-Gaussianity, deviations from scale invariance.

• Also: polarized synchrotron data, radio source & planet data, calibration source for ground/balloon-based experiments

4/24/2008 WMAP 2008 Senior Review 23

Output counts per unit of input temperature difference changes with time due to changes in spacecraft temperature and amplifier properties.

Multiple years of data help to separate these effects and improve uncertainty in the gain model.

Change in instrument offset vs. time. Additional years of data improve our knowledge of the sources of offset: thermal emission, gain variation, etc.

Detailed Understanding of InstrumentDetailed Understanding of Instrument

TT 5-Yr

TT 9-Yr

TE 5-Yr

TE 9-Yr

EE

Dark EnergyDark Energy

WMAP5 and the Cluster Mass FunctionK. Rines, A. Diaferio & P. Natarajan

arXiv:0803.1843

Growth FunctionCombined LSS and CMB measurements probe Dark Energy. Improvements in cluster counts (Chandra, ROSAT, SDSS, DES, Pan-STARRS, etc.) and weak lensing surveys will demand better measurements of 8 and m to constrain w(z).

The predicted number of massive clusters (alternatively, the SZ power spectrum) scales as 8

7 !

Acoustic scale WMAP measures the sound horizon at z=1090. This acoustic scale is the fundamental calibration for on-going and planned baryon acoustic oscillation measurements.

lA = 302.08 ± 0.84 (5 yr) → ± 0.64 (9 yr)(30% improvement)

Closing in on Closing in on 88 and and mm

2006

2006

2006

Chandra cluster counts: Vikhlinin et al.Chandra cluster counts: Vikhlinin et al.

2008+

InflationInflation

• Have we detected deviations from scale-invariance?

~2.5 σ

• Is there a running spectral index?

Probably not.

• Is there primordial non-Gaussianity?

Not yet…

• What is the amplitude of tensor modes (gravitational waves)?

r<0.2

Testing InflationTesting Inflation

Future CMB From SpaceFuture CMB From Space• Planck

Spacecraft is integrated, launch is imminent! See next talk.

• CMBPol

High sensitivity polarization to probe gravity waves from Inflation.

Inflation and Gravity Waves - IInflation and Gravity Waves - I• Inflation predicts two forms of fluctuations:

– Scalar modes (density perturbations) with slope ns:

• generate CMB anisotropy and lead to structure formation

– Tensor modes (gravity waves) with slope nt:

• generate CMB anisotropy but do not contribute to structure formation• Gravity wave amplitude, r, proportional to energy scale of inflation:

• Both types of fluctuations contribute to CMB temperature anisotropy:

scalar

tensor

pl kP

kPr

E

mr

)(

)( with

GeV103.3

V

0

016

infl

1/44/1

Inflation and Gravity Waves – IIInflation and Gravity Waves – II• Both types of fluctuations contribute to CMB polarization anisotropy:

– Scalar modes produce only “E-mode” polarization patterns, by symmetry– Tensor modes produce both “E-mode” and “B-mode” polarization patterns (see

below)• The observation of B-mode polarization uniquely separates scalar and tensor modes

from inflation and measures the energy scale of inflation.• Only known probe of physics at E ~ 1016 GeV… 12 orders of magnitude higher than

planned accelerators.

E – scalar+tensor B – tensor only

Sensitivity & Foreground EstimatesSensitivity & Foreground Estimates

Blue band -Galactic foreground estimate from WMAP3, frequency dependent

Green line -Lensing (EE→BB), frequency independent

Red lines -Gravity wave signal(s)

Grey shaded band - 1-sigma sensitivity for 1000-channel system with 1-yr integration, 1°FWHM resolution

r=0.01

r=0.3

Candidate CMBPol ConceptCandidate CMBPol Concept

Multiple copies of basic polarimeter module, scaled in frequency, packaged in focal plane, co-aligned along s/c symmetry axis.

4/24/2008 WMAP 2008 Senior Review 38

Monodromy in the CMB: Gravity Waves and String InflationEva Silverstein and Alexander Westphal

http://arxiv.org/abs/0803.3085v2

Large-field inflation (hence gravitational waves) from string theory compactified on twisted tori.