cmb anisotropy thru wmap iii
DESCRIPTION
CMB Anisotropy thru WMAP III. Ned Wright, UCLA. True Contrast CMB Sky. 33, 41 & 94 GHz as RGB, 0-4 K scale. Enhanced Contrast:. Conklin 1969 - 2 Henry 1971 - 3 Corey & Wilkinson 1976 - 4 Smoot et al. 1977 - 6. A Big Media Splash in 1992:. 25 April 1992. - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/1.jpg)
CMB Anisotropy thru WMAP III
Ned Wright, UCLA
![Page 2: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/2.jpg)
True Contrast CMB Sky
33, 41 & 94 GHz as RGB, 0-4 K scale
![Page 3: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/3.jpg)
Enhanced Contrast:
• Conklin 1969 - 2• Henry 1971 - 3• Corey & Wilkinson
1976 - 4• Smoot et al. 1977 - 6
![Page 4: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/4.jpg)
A Big Media Splash in 1992:
Prof. Stephen Hawking of Cambridge University, not usually noted for overstatement, said: “It is the discovery of the century, if not of all time.”
25 April 1992
![Page 5: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/5.jpg)
Animated View of Inflation
• Quantum fluctuations occur uniformly throughout space-time
• Future light cones have radii of (c/H)[exp(Ht)-1]
![Page 6: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/6.jpg)
COBE DMR vs EPAS
“Chi-by-eye” suggests that the “Equal Power on All Scales” prediction of inflation is correct.
![Page 7: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/7.jpg)
Sachs-Wolfe Effect: Gravitational potential = 3c2T/T Leads to
Large-Scale Structure
![Page 8: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/8.jpg)
Prediction of Acoustic Peaks in CDM
Bond & Efstathiou, 1987, MNRAS, 226, 655-687
![Page 9: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/9.jpg)
Two Fluids in the Early Universe• Most of the mass is dark matter
– 80-90% of the density– Zero pressure– Sound speed is zero
• The baryon-photon fluid– baryons are protons & neutrons = all ordinary
matter– energy density of the photons is bigger than c2
times the density of baryons– Pressure of photons = u/3 = (1/3) c2
– Sound speed is about c/3 = 170,000 km/sec
![Page 10: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/10.jpg)
Traveling Sound Wave: cs c/3
![Page 11: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/11.jpg)
Stay at home Dark Matter
![Page 12: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/12.jpg)
Interference at last scattering• For the wavelength illustrated [1/2 period
between the Big Bang and recombination], the denser = hotter effect and potential well = cooler effect have gotten in phase.
• For larger wavelengths they are out of phase at recombination:
![Page 13: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/13.jpg)
![Page 14: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/14.jpg)
![Page 15: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/15.jpg)
![Page 16: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/16.jpg)
![Page 17: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/17.jpg)
Spherical Harmonic Decomposition
![Page 18: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/18.jpg)
Many parameters to measure
Careful measurements of the power at various angular scales can determine the Hubble constant, the matter density, the baryon density, and the vacuum density.
![Page 19: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/19.jpg)
COBE View was Blurry
![Page 20: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/20.jpg)
Pre-WMAP Power Spectrum
Flat, n=1; b = 0.021, c = 0.196, Ho = 47; b = 0.022, c = 0.132, Ho = 68, = 2/3
![Page 21: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/21.jpg)
Calibration Uncertainties• Each experiment (except for COBE and
later WMAP) has amplitude uncertainty of several percent that is correlated across all the data from that experiment.
• I have done fits and plots that solve separately for calibration adjustment “nuisance parameters” which are included in the 2 but not in the errorbars.
• Combining data from many experiments gives a “flexible” observed spectrum due to these calibration errors.
![Page 22: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/22.jpg)
![Page 23: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/23.jpg)
The WMAP RF plumbing is very complexwith 10 horns per side, 20 DA’s, 40 amplifier chains.
![Page 24: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/24.jpg)
![Page 25: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/25.jpg)
Huge Amount of Data• 5 bands.• 23, 33, 41, 61 & 94 GHz.• 2, 2, 4, 4 & 8 temperature differences per
band. Two detectors for each differential T.• 128, 128, 102.4, 76.8 & 51.2 ms/sample.• 279 temperature differences per second.• 53 billion samples in 3 years.• About 2108 samples per low l polarization.• Systematic error control is critical!
![Page 26: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/26.jpg)
Systematic Error Control
![Page 27: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/27.jpg)
MAP’s Orbit
![Page 28: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/28.jpg)
Temperature Stability• 7% p-p yearly
insolation modulation from eccentricity of Earth’s orbit
• Slow change in thermal properties: 3%/yr in albedo or emissivity.
Pioneer anomaly could be explained by 3% emissivity anisotropy.
![Page 29: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/29.jpg)
Scan Strategy• 6 Months for full sky
coverage1 hour precession 2 minute spin
Not to scale:Earth — L2 distance is 1% of Sun — Earth Distance
![Page 30: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/30.jpg)
Noise Pattern is not Uniform
• Stokes I, Q, U & <QU> all have different noise patterns.
![Page 31: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/31.jpg)
Combination to remove foreground
![Page 32: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/32.jpg)
QVW as RGB
![Page 33: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/33.jpg)
![Page 34: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/34.jpg)
Scattering creates Polarization
Reionization puts scatterers at A: many degree scale
Scatterers during recombination are at B: degree scale
![Page 35: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/35.jpg)
Top view of same S-T Diagram• Electrons at A or
B see a somewhat different piece of the surface of last scattering than we do.
• If electrons at A or B see a quadrupole anisotropy then we get polarization.
![Page 36: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/36.jpg)
ROM Foreground Fit in P06 Cut
• m = -0.6• EE
– Bs = 0.36, s = -3.0
– Bd = 1.0, d = 1.5
• BB:– Bs = 0.30, s = -2.8
– Bd = 0.50, d = 1.5
![Page 37: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/37.jpg)
Final Results
EE only: = 0.10 0.03
TT, TE & EE: = 0.09 0.03
![Page 38: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/38.jpg)
Foreground vs CMB Polarization
![Page 39: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/39.jpg)
Foreground vs CMB T
![Page 40: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/40.jpg)
![Page 41: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/41.jpg)
Comparison to Previous Best Fit
• Now we have = 0.09 0.03 instead of = 0.117 0.055 for the WMAP I best fit.
• But quite a bit less than the old WMAP I TE only = 0.17 0.04
![Page 42: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/42.jpg)
Effects on Peak Position: lpk
+ Open or vacuum dominated Universes give larger distance to last scattering surface
+ High matter density gives smaller wavelength
![Page 43: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/43.jpg)
CMB alone does not imply flatness
• But CMB + Ho (or other data) do imply flatness and a dark energy dominated Universe.
![Page 44: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/44.jpg)
CDM is a Good Fit
![Page 45: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/45.jpg)
But so is “super Sandage”
![Page 46: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/46.jpg)
![Page 47: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/47.jpg)
Non-flat Dark Energy Fitting!
k = 0, w = -1 is OK: -0.93 > w > -1.14
With many datasets combined, the equation of state w and the curvature can be measured together.
![Page 48: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/48.jpg)
Late ISW Effect: Another test for
Potential only changes if m 1 (or in non-linear collapse, but that’s another story [Rees-Sciama effect]).
![Page 49: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/49.jpg)
Potential decays at z 0.6
![Page 50: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/50.jpg)
CMB-LSS correlation seen by WMAP
• This late ISW effect occurs on our past light cone so the T we see is due to structures we also see.
• Correlation between WMAP and LSS seen by:– Boughn & Crittenden (astro-ph/0305001) at 2.75 with hard X-ray
background and 2.25 with NVSS– Nolta et al. (astro-ph/0305097) at 2 with NVSS– Afshordi et al (astro-ph/0308260) at 2.5 with 2MASS
![Page 51: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/51.jpg)
2MASS galaxies reach z = 0.1
Credit: Tom Jarrett, IPAC
![Page 52: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/52.jpg)
WIDE-FIELD INFRARED SURVEY EXPLORER
I am the PI on a MIDEX called WISE, an all-sky survey in 4 bands from 3.3 to 23 m. WISE will find and study the closest stars to the Sun, the most luminous galaxies in the Universe, and also map the large-scale structure out to redshift z=1, covering the era when the late ISW effect should be generated.
WISE might fly in 2009, but is being delayed by NASA’s budget woes.
![Page 53: CMB Anisotropy thru WMAP III](https://reader035.vdocument.in/reader035/viewer/2022062316/56816849550346895dde36af/html5/thumbnails/53.jpg)
CONCLUSIONS• The intrinsic anisotropy of the CMB, first
observed by the COsmic Background Explorer (COBE), has now become an extremely significant tool for the study of the Universe in the hands of the Wilkinson Microwave Anisotropy Probe - another Explorer mission.
• WMAP will continue for a few more years. • ESA’s Planck mission will continue to exploit
the CMB with higher angular resolution, higher sensitivity and higher frequency data.