third year wmap results dave wilkinson. nasa/gsfc bob hill gary hinshaw al kogut michele limon nils...
TRANSCRIPT
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Third Year WMAP Results
Dave Wilkinson
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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
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What’s New in the Measurement?
Three times as much data, sqrt(3) smaller errors in maps: more than 50x reduction in model parameter space.
Direct measurement of CMB polarization.
Much better understanding of instrument, noise, gain, beams, and mapmaking.
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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
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Stability of instrument is critical
Physical temperature of B-side primary over three years. This is the largest change on the instrument.
Jarosik et al.
Three parameter fit to gain over three years leads to a clean separation of gain and offset drifts.
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K Band, 22 GHz
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Ka Band, 33 GHz
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Q Band, 41 GHz
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V Band, 61 GHz
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W Band, 94 GHz
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Compare Spectra
Cosmic variance limited to l=400.
First peak
Window function dominates difference
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Reionization
Best fit model
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Maps of Multipoles
Too aligned?
Too symmetric?
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Summary of Temperature Maps
Data + completely new pipeline consistent with first year.
Maximum likelihood for low l (Efstathiou, Seljak et al.)
New improved power spectrum. No clear glitches, low-l less anomalous, clear second peak.
Calibration error still 0.5%
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Polarization
New measurement of optical depth to the surface of last scattering.
First all sky measurement of polarized foreground emission.
Direct measurement of low-l E modes.
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K Band, 22 GHz 50
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Ka Band, 33 GHz
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Q Band, 41 GHz
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V Band, 61 GHz
CMB 6 uK
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W Band, 94 GHz
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Q&U Maps
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Blowouts
Berkhuijsen et al.
Loops
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Polarized Foreground Emission
B-field
Synchrotron emission
Starlight polarization
Dust emission
Dust grain
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5 GHz Polarization & B field
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Polarized Foreground Emission
B field from K band B field from model
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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
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Raw vs. Cleaned
Maps
Galaxy masked in analysis
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Mask
Use 75% of sky for cosmological analysis
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High l TE
Crittenden et al.
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High l EE
All direct polarization measurements to date.
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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
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Low l EE/BB “Features”
Still, though, even accounting for this, EE W-band l=5,7 is problematic. All others OK.
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Low-l EE/BB
EE (solid)
BB (dash)
BB model at 60 GHz
r=0.3
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Frequency space
“Spikes” from correlated polarized sync and dust.
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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.
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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.
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OpticaL Depth
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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
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BB r=0.3
EE
TE
TT
Approx EE/BB foreground
BB Lensing
BB inflation
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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.
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Degeneracy
Knowledge of optical depth breaks the degeneracy
1yr WMAP
3yr WMAP
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Best Fit LCDM Model
WMAP-1
WMAP-3 1.037 for 3162 DOF TT+TE+EE
Mean
= 0.92+-0.1 = 0.29+-0.07
WMAP-10.0230.1450.68…0.100.970.880.32Max L
0.02220.1280.73…0.0920.9580.770.24
Smaller error bars and better fit that year 1
WMAP-3
Max L
WMAP-3 SZ Marg0.02233 +/-0.00080.1268 +/-0.010.734 +/- 0.03…0.088 +/- 0.030.951 +/- 0.0170.744 +/- 0.0550.238 +/- 0.035
Max L, sym err
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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.
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What Does the Model Need?
Model needs , 8
Model needs not unity, 8
Model needs dark matter, 248
Model does not need: running, r, or massive neutrinos, le 3.
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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:
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Inflation Parameters, No Running
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Equation of State & Curvature
WMAP+CMB+2dFGRS+SDSS+SN
Interpret as amazing consistency between data sets.
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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.
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New ILC
Now can be used for l=2,3!
However, some non-Gaussanity persists!
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THANK YOU