Third Year WMAP Results

1
Third Year WMAP Results
Dave Wilkinson
2
WMAP
A partnership between NASA/GSFC and Princeton
Science Team
NASA/GSFC Bob Hill Gary Hinshaw Al
Kogut Michele Limon Nils Odegard Janet Weiland Ed
Wollack
Johns Hopkins Chuck Bennett (PI)
UCLA Ned Wright
Brown Greg Tucker
Chicago Stephan Meyer Hiranya Peiris
UBC Mark Halpern
Princeton Norm Jarosik Lyman Page David Spergel.
CITA Olivier Dore Mike Nolta
Penn Licia Verde
UT Austin Eiichiro Komatsu
Cornell Rachel Bean
Microsoft Chris Barnes
3
Whats New in the Measurement?
Much better understanding of instrument, noise,
gain, beams, and mapmaking.
Direct measurement of CMB polarization.
Three times as much data, sqrt(3) smaller errors
in maps more than 50x reduction in model
parameter space.
4
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
)
(


ltExExgt
ltExEygt


ltEyExgt
ltEyEygt
(
(
A-B-A-B
B-A-B-A
)
)

0
I/2

Q/2
U/2
One of 20
0
I/2
-Q/2
U/2
Amplifiers from NRAO, M. Pospieszalski design
Coherency matrix
5
Stability of instrument is critical
Physical temperature of B-side primary over three
years. This is the largest change on the
instrument.
Three parameter fit to gain over three years
leads to a clean separation of gain and offset
drifts.
Jarosik et al.
6
K Band, 22 GHz
7
Ka Band, 33 GHz
8
Q Band, 41 GHz
9
V Band, 61 GHz
10
W Band, 94 GHz
11
Compare Spectra
First peak
Cosmic variance limited to l400.
Window function dominates difference
12
(No Transcript)
13
Best fit model
Reionization
14
Maps of Multipoles
Too aligned?
Too symmetric?
15
Summary of Temperature Maps
New improved power spectrum. No clear glitches,
low-l less anomalous, clear second peak.
Maximum likelihood for low l (Efstathiou, Seljak
et al.)
Data completely new pipeline consistent with
first year.
Calibration error still 0.5
16
Polarization
First all sky measurement of polarized foreground
emission.
New measurement of optical depth to the surface
of last scattering.
Direct measurement of low-l E modes.
17
K Band, 22 GHz
50
18
Ka Band, 33 GHz
19
Q Band, 41 GHz
20
V Band, 61 GHz
CMB 6 uK
21
W Band, 94 GHz
22
QU Maps
23
Blowouts
Loops
Berkhuijsen et al.
24
Polarized Foreground Emission
Dust grain
B-field
Dust emission
Starlight polarization
Synchrotron emission
25
5 GHz Polarization B field
26
Polarized Foreground Emission
B field from K band
B field from model
27
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.

Band
Pre-Cleaned
Cleaned
Table of
Ka 2.14 1.096 Q
1.29 1.02 V 1.05
1.02 W 1.06
1.05
4534 DOF
28
Raw vs. CleanedMaps
Galaxy masked in analysis
29
Mask
Use 75 of sky for cosmological analysis
30
High l TE
Crittenden et al.
31
High l EE
All direct polarization measurements to date.
32
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

33
Low l EE/BB Features
Still, though, even accounting for this, EE
W-band l5,7 is problematic. All others OK.
34
Low-l EE/BB
EE (solid)
BB (dash)
BB model at 60 GHz
r0.3
35
Frequency space
Spikes from correlated polarized sync and dust.
36
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.
37
Low-l EE/BB
EE
BB
BB Polarization null check and limit on
gravitational waves.
EE Polarization from reionization of first stars
rlt2.2 (95 CL) from just EE/BB
Just Q and V bands.
38
OpticaL Depth
39
Optical Depth
Knowledge of the optical depth affects the
determination of the cosmological parameters,
especially ns
Bands
EE only
EE TE only
0.111 /- 0.022 0.100 /- 0.029 0.111 /-
0.021 0.107 /- 0.018
0.111 /- 0.022 0.092 /- 0.029 0.101 /-
0.023 0.106 /- 0.019
KaQV QV QVW KaQVW
Best overall with 6 parameters 0.088 /-
0.031
40
TT
TE
EE
Approx EE/BB foreground
BB inflation
BB r0.3
BB Lensing
41
New Cosmological Parameters
Knowledge of optical depth breaks the n-tau
degeneracy.
New analysis based primarily on WMAP alone.
Take WMAP and project to other experiments to
test for consistency.
42
Degeneracy
1yr WMAP
3yr WMAP
Knowledge of optical depth breaks the
degeneracy
43
Best Fit LCDM Model
WMAP-1
WMAP-1
WMAP-3 SZ Marg
WMAP-3
0.023 0.145 0.68 0.10 0.97 0.88 0.32
0.0222 0.128 0.73 0.092 0.958 0.77 0.24
0.02233 /-0.0008 0.1268 /-0.01 0.734 /-
0.03 0.088 /- 0.03 0.951 /- 0.017 0.744 /-
0.055 0.238 /- 0.035
0.92-0.1
0.29-0.07
Mean
Max L
Max L
Max L, sym err
WMAP-3 1.037 for 3162 DOF
TTTEEE
Smaller error bars and better fit that year 1
44
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.
45
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.
46
Gravitational Waves
WMAP alone, rlt0.55 (95 CL)
WMAP2dF, rlt0.30 (95 CL)
WMAPSDSS, rlt0.28 (95 CL)
In all cases, n_s rises to compensate.
WMAP-1SDSS Tegmark et al
Similar behavior
WMAP-1SDSSLya Seljak et al
47
Inflation Parameters, No Running
48
Equation of State Curvature
Interpret as amazing consistency between data
sets.
WMAPCMB2dFGRSSDSSSN
49
Final Bits
Sum of mass of light neutrinos is lt0.68 eV (95
CL). Has not changed significantly.
No evidence for non-Gaussanity in any of our
tests Minkowski functionals, bispectrum,
trispectrum..
50
New ILC
However, some non-Gaussanity persists!
Now can be used for l2,3!
51
THANK YOU