Recent Results from WMAP Dave Wilkinson L. Page, DESY, September, 2006.

Recent Results from WMAP

Dave Wilkinson

L. Page, DESY, September, 2006

The Standard Cosmological Model

Surface of last scattering at “decoupling.”

“Reionization”

QuickTime™ and aMicrosoft Video 1 decompressorare needed to see this picture.

Mark Subbarao & SDSS Collaboration

The New Science

Inflation-like models, based on field theories of the t<10-20s Universe, predict the gravitational landscape to which the contents respond, differ by 5% from the historic (PHZ) phenomenological description.

Basic model agrees with virtually all cosmological measurements.

The DM/DE composition is parametrized phenomenologically.

WMAP observes this difference.

What’s New in the Measurement?

Three times as much data, smaller errors in maps: more than 50x reduction in model parameter space.

Direct measurement of CMB polarization at >100 angular scales. The error bars are near 300 nK.

Much better understanding of instrument, noise, gain, beams, and mapmaking.

NASA/GSFCBob Hill Gary Hinshaw Al KogutMichele LimonNils OdegardJanet WeilandEd Wollack

PrincetonNorm Jarosik Lyman PageDavid Spergel.

UBCMark Halpern

ChicagoStephan MeyerHiranya Peiris

BrownGreg Tucker

UCLANed Wright

Science Team:

WMAPA partnership between NASA/GSFC and Princeton

QuickTime™ and aCinepak decompressorare needed to see this picture.

Johns HopkinsChuck Bennett (PI)

CornellRachel Bean Microsoft

Chris Barnes

CITAOlivier DoreMike Nolta

PennLicia Verde

UT AustinEiichiro Komatsu

One of 20

A-B-A-B B-A-B-A

Amplifiers from NRAO, M. Pospieszalski design

For temperature: measure difference in power from both sides. CMB: 30 uK rms

For polarization: measure the difference between differential temperature measurements with opposite polarity. CMB 0.3 uK rms

<ExEx> <ExEy><EyEx> <EyEy>

* ***

=0

0I/2I/2

(( )

))(+ Q/2

-Q/2U/2

U/2

Coherency matrix

(>100)

Intensity Stokes Q&U

Stability of instrument is critical

Physical temperature of B-side primary over three years.

Jarosik et al.

Three parameter fit to gain over three years leads to a clean separation of gain and offset drifts.

3yr ModelData based on dipole

Model based on yr1 alone

K Band, 22 GHz

Ka Band, 33 GHz

Q Band, 41 GHz

V Band, 61 GHz

W Band, 94 GHz

Power spectrum~10

~0.40

Physical size = plasma speed X age of universe at decoupling

The overall tilt of this spectrum--- encoded in the “scalar spectral index” ns--- is the new handle on inflation.

Angular Power Spectrum.

early in inflation

later in inflation

“Geometric Degeneracy”

CMB alone tells us we are on the “geometric degeneracy” line

Reduced

closed

open

Assume flatness

WMAP3 only best fit LCDM

{

Large Angular Scale Polarization

The formation of the first stars produces free electrons that:

(1) rescatter CMB photons thereby reducing the anisotropy and

(2) polarize the CMB at large angular scales.

These effects mimic a change in ns:

“the ns - tau” degeneracy

WMAP measures (2) to break the degeneracy

K Band, 22 GHz 50

Ka Band, 33 GHz

Q Band, 41 GHz

V Band, 61 GHz

CMB 6 uK

W Band, 94 GHz

From Wayne Hu

Polarization of the CMB is produced by Thompson scattering of a quadrupolar radiation pattern.

Seljak & Zaldarriaga

2 deg

CMB Polarization

Whenever there are free electrons, the CMB is polarized.

The polarization field is decomposed into “E” and “B” modes.

E

B

Gravitational wave

Density wave

Terminology: E/B Modes

E-modes B-modes

k k

Types of Cosmological Perturbations

Tensors: h (GW strain)

Temperature

E polarization

E polarization

B polarization

Temperature

Scalars: ,

Or less!0.3

n and r are predicted by models of inflation.

Low-l EE/BB

EE (solid)

BB (dash)

EE/BB model at 60 GHz

r=0.3

Since reionization is late we see it at large angular scales. This is our handle on the optical depth.

Raw vs. Cleaned

Maps

Galaxy masked in analysis

Low-l EE/BB

EE Polarization: from reionization by the first stars

BB Polarization: null check and limit on gravitational waves.

r<2.2 (95% CL) from just EE/BB

EE BB

Just Q and V bands.

Degeneracy

Knowledge of optical depth breaks the degeneracy

1yr WMAP

3yr WMAP

LWMAP1+ACBAR+CBI

No SZ marg

BB r=0.3

EE

TE

TT

Approx EE/BB foreground

BB Lensing (not primordial)

BB inflation

What Does the Model Need to Describe the Data?

Model needs , 8

Model needs not unity, 8

Model needs dark matter, 248

Model does not need: “running,” r, or massive neutrinos, < 3.

changing one of the 6 parameters at a time….

The data are, of course, less restrictive when there are more parameters.

(“2.8 sigma”)

(“15 sigma”)

….but Eriksen & Huffenberger

0.959+/-0.016 WMAP

0.947+/-0.015 (all){

Equation of State & Curvature

WMAP+CMB+2dFGRS+SDSS+SN

Interpret as amazing consistency between data sets.

Thank You!

Maps of Multipoles

Too aligned?

Too symmetric?

What’s Next?The CMB is still a scientific gold mine.

Small scale anisotropy Polarization at all angular scales

Better known parameters

Non-gaussanity?

Non-adiabatic modes ?

Neutrino mass?

W not -1?

Formation and growth of cosmic structure.

Tests of field theories at 10-35 s.

Something new?

Selected Bolometer-Array and SZ Roadmap

2005 2006 2007 2008

Polarbear-I(300 bolometers) California

SZA(Interferometer) Owens Valley

APEX(~400 bolometers) Chile

SPT(1000 bolometers) South Pole

ACT(3000 bolometers) Chile

Planck(50 bolometers) L2

(12000 bolometers)SCUBA2QUAD

BiCEP

BRAINQUIETCLOVER

“large scale” (unique to satellite)2 bumpsR=0.01

Cluster (SZ, KSZ

X-rays, & optical) Diffuse SZ

OV/KSZ

CMB: l>1000

Lensing

Observations: Science: Growth of structure

Eqn. of state

Neutrino mass

Ionization history

ACT Atacama Cosmology Telescope

Optical

X-ray

Theory

InflationPower spectrum

Columbia HaverfordU. KwaZulu-NatalRutgers U. Catolica

Cardiff

UMassCUNY

UBCNISTINAOE NASA/GSFC

UPenn U. Pittsburgh U. TorontoPrinceton

Collaboration:

More simulations of mm-wave sky.

1.40<1%

≈2%Survey area

High quality area

150 GHz SZ Simulation MBAC on ACT PLANCK

WMAP

PLANCKTarget Sensitivity (i.e. ideal stat noise only)

de Oliveira-Costa

Burwell/Seljak

1.5’ beam

ACT

SPT & APEX as well.

/ Diffuse KSZ / Diffuse KSZ

Need picture

SCUBA

Completed “close-packed” 12x32 bolometer array

Linear array after folding

Torsional yoke attachment

SHARC II 12x32 Popup Array

One element of array

1 mm

3.2 mm

PI D. Dowell

Arrays of bolometersMoseley et al, NASA/GSFC

Irwin et al.

Warm electronics based on SCUBA2

Halpern et al. UBC

S. Staggs is lead

Pulse Tube3He Fridge

40K Shield 3 feet

Camera (MBAC) Layout

D. Swetz

Filters: CardiffAR Coated Si lenses.

0.6K

New Type of TelescopeM. Devlin is lead

Telescope at AMEC in Vancouver. Ship to Chile in 2006.

First Light Dec 05

Moon

Measured from Jadwin Hall at 150 GHz with x11 attenuation.

CCAM

CCAM: A 1x32 muxed TES array prototype on the WMAP spare.

THANK YOU

Angular Power Spectrum

Q&U Maps

Foreground Model•Template fits (not model just shown).•Use all available information on polarization directions.•Sync: Based on K band directions•Dust: Based on directions from starlight polarization.•Increase errors in map for subtraction.•Examine power spectrum l by l and frequency.•Examine results with different bands.•Examine the results with different models.

Ka 2.14 1.096Q 1.29 1.02V 1.05 1.02W 1.06 1.05

Band Pre-Cleaned Cleaned

4534 DOF

Table of

High l TE

Crittenden et al.

Frequency space

“Spikes” from correlated polarized sync and dust.

The Standard Cosmological Model

At a very early time a “quantum field” impressed on the universe a gravitational landscape.

Abbreviated

This is literally a picture of a quantum field from the birth of the universe.

Matter fell into the valleys to form eventually “structure.” But only 1/6 of this matter is familiar to us.

The dynamics of the universe is now driven not so much by the matter but by a new form of energy: “The Dark Energy.”

Compare Spectra

Cosmic variance limited to l=400.

First peak

Window function dominates difference

Foreground Model•Template fits (not model just shown).•Use all available information on polarization directions.•Sync: Based on K band directions•Dust: Based on directions from starlight polarization.•Increase errors in map for subtraction.•Examine power spectrum l by l and frequency.•Examine results with different bands.•Examine the results with different models.

Ka 2.14 1.096Q 1.29 1.02V 1.05 1.02W 1.06 1.05

Band Pre-Cleaned Cleaned

4534 DOF

Table of

Low-l TE

New noise, new mapmaking, pixel space foreground subtaction, different sky cut, different band combination.

New results consistent with original results.

New results also consistent with zero!

4 to model

Low-l EE/BB

EE (solid)

BB (dash)

BB model at 60 GHz

r=0.3

Frequency space

“Spikes” from correlated polarized sync and dust.

Spectrum of Foreground Subtraction

Pre-cleaned error bars do not include 2NF term.

Recall, foreground subtraction is done on maps, not spectra.

We use QV for analysis, check with other channels.

Low-l EE/BB

EE Polarization: from reionization of first stars

BB Polarization: null check and limit on gravitational waves.

r<2.2 (95% CL) from just EE/BB

EE BB

Just Q and V bands.

OpticaL Depth

Optical Depth

Knowledge of the optical depth affects the determination of the cosmological parameters, especially ns

0.111 +/- 0.0220.100 +/- 0.0290.111 +/- 0.0210.107 +/- 0.018

0.111 +/- 0.0220.092 +/- 0.0290.101 +/- 0.0230.106 +/- 0.019

KaQVQVQVWKaQVW

Bands EE only EE +TE only

Best overall with 6 parameters

=0.088 +/- 0.031

New Cosmological Parameters

New analysis based primarily on WMAP alone.

Knowledge of optical depth breaks the n-tau degeneracy.

Take WMAP and project to other experiments to test for consistency.

Degeneracy

Knowledge of optical depth breaks the degeneracy

1yr WMAP

3yr WMAP

Add 2dFGRS, SDSS, CMB,SN,WL

The general trend is:

drops to 0.945-0.950 +0.015/-0/017

drops when CMB added & rises when

galaxies added A “working number” is 0.26

The scalar spectral index is 0.97+/- 0.02 Seljak et al. and 0.98+/-0.03 (Tegmark et al.) for WMAP-1 +SDSS.

Gravitational Waves

WMAP alone, r<0.55 (95% CL)

WMAP+2dF, r<0.30 (95% CL)

WMAP+SDSS, r<0.28 (95% CL)

In all cases, n_s rises to compensate.

WMAP-1+SDSS Tegmark et alWMAP-1+SDSS+Lya Seljak et al

Similar behavior:

Final Bits

No evidence for non-Gaussanity in any of our tests: Minkowski functionals, bispectrum, trispectrum…..

Sum of mass of light neutrinos is <0.68 eV (95% CL). Has not changed significantly.

New ILC

Now can be used for l=2,3!

However, some non-Gaussanity persists!

BB r=0.3

EE

TE

TT

Approx EE/BB foreground

BB Lensing

BB inflation