WMAP

(Wilkinson Microwave Anisotropy Probe)

Other Web pages: Spires

Useful Links

References

Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation

$\Omega_\Lambda = 0.721 +- 0.015 \Omega_c = 0.233 +- 0.013 \Omega_b = 0.0462 +- 0.0015 H_0 = 70.1 +- 1.3 km \text{s}^{-1} Mpc^{-1}$

$-0.11<1+w_\Lambda<0.14 \text{(95% CL)} -0.0175<\Omega_k<0.0085 (95% CL)$

$\sum m_\nu < 0.61 \text{eV} (95% CL) N_{\rm eff} = 4.4 +- 1.5$

(6 March 2008)

Three-Year WMAP Observations
Implications for Cosmology

Flat Lambda-CDM Model (WMAP data only)
$\left( \Omega_{\text{M}} h^2, \Omega_{B} h^2, h, n_{\text{s}}, \tau, \sigma_8 \right) = \left( 0.127 {}^{+0.007}_{-0.013}, 0.0223 {}^{+0.0007}_{-0.0009}, 0.73 {}^{+0.03}_{-0.03}, 0.951 {}^{+0.015}_{-0.019}, 0.09 {}^{+0.03}_{-0.03}, 0.74 {}^{+0.05 0.06}_{-0.06} \right)$

WMAP + SNLS + $(\Omega_0=1)$ $w_{\Lambda} = -0.97 {}^{+0.07}_{-0.09}$

WMAP + SNLS + $(w_{\Lambda}=-1)$ $\Omega_0 = 1.015 {}^{+0.020}_{-0.016}$

WMAP + HST $\Omega_0 = 1.010 {}^{+0.016}_{-0.009}, \Omega_{\Lambda} = 0.72 +- 0.04$

WMAP + LLS +SNIa $w_{\Lambda} = -1.06 {}^{+0.13}_{-0.08}$

$Flat \ensuremath{\LambdaCDM:}$ $\sum m_\nu <$ $2.0 \text{eV}$ (WMAP)

(WMAP + SDSS)

$0.87 \text{eV}$ (WMAP + 2dFGRS)

(CMB + LLS +SNIa) $\text{(95% C.L.)}$

$Flat \ensuremath{\LambdaCDM:}$ $N_{\nu} =$ $5.92 {}^{+0.25}_{-3.45}$ (WMAP + SDSS)

$2.68 {}^{+0.26}_{-1.67}$ (WMAP + 2dFGRS)

$3.29 {}^{+0.45}_{-2.18}$ (CMB + LLS +SNIa)

Mission Results - Press Release

First Year WMAP Observations

Universe is 13.7 billion years old (±1%)

First stars ignited 200 million years after the Big Bang

Content of the Universe: 4% Atoms, 23% Cold Dark Matter, 73% Dark Energy

$\Omega_\nu h^2 < 0.0076 => m_\nu < 0.23 \text{eV} (95% C.L.)$

Expansion rate (Hubble constant): H₀= 71 km/sec/Mpc (±5%)

New evidence for Inflation (in polarized signal)

Mission Results - Preliminary Maps and Basic Results

Useful Links

LAMBDA, Legacy Archive for Microwave Background Data Analysis

References

References are divided in

1 - Reviews
2 - Articles
3 - Detector
4 - Conference Proceedings

The references in each group are listed in approximate inverted chronological order.
Click on the reference label to search it in Spires.

1 - Reviews

[1-1]: The Wilkinson Microwave Anisotropy Probe, Lyman Page, arXiv:astro-ph/0306381, 2003. Carnegie Observatories Astrophysics Series, Vol. 2: Measuring and Modeling the Universe.

2 - Articles

[2-1]: Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Are There Cosmic Microwave Background Anomalies?, C. L. Bennett et al., arXiv:1001.4758, 2010.
[2-2]: Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Sky Maps, Systematic Errors, and Basic Results, N. Jarosik et al., arXiv:1001.4744, 2010.
[2-3]: Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Planets and Celestial Calibration Sources, J. L. Weiland et al., arXiv:1001.4731, 2010.
[2-4]: Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Power Spectra and WMAP-Derived Parameters, D. Larson et al., arXiv:1001.4635, 2010.
[2-5]: Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Galactic Foreground Emission, B. Gold et al., arXiv:1001.4555, 2010.
[2-6]: Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation, E. Komatsu et al., arXiv:1001.4538, 2010.
From the abstract: Notable examples of improved parameters are the total mass of neutrinos, $\sum m_\nu < 0.58 eV \text{(95% CL)}$ , and the effective number of neutrino species, $N_{eff} = 4.34^{+ 0.86}_{- 0.88} \text{(68%~CL)}$ , which benefit from better determinations of the third peak and .
[2-7]: Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Data Processing, Sky Maps, and Basic Results, G. Hinshaw et al. (WMAP), Astrophys. J. Suppl. 180 (2009) 225-245, arXiv:0803.0732.
[2-8]: Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Galactic Foreground Emission, B. Gold et al. (WMAP), Astrophys. J. Suppl. 180 (2009) 265-282, arXiv:0803.0715.
[2-9]: Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Angular Power Spectra, M. R. Nolta et al. (WMAP), Astrophys. J. Suppl. 180 (2009) 296-305, arXiv:0803.0593.
[2-10]: Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Likelihoods and Parameters from the WMAP data, J. Dunkley et al. (WMAP), Astrophys. J. Suppl. 180 (2009) 306-329, arXiv:0803.0586.
[2-11]: Five-Year Wilkinson Microwave Anisotropy Probe (WMAP)Observations: Beam Maps and Window Functions, R. S. Hill et al. (WMAP), Astrophys. J. Suppl. 180 (2009) 246-264, arXiv:0803.0570.
[2-12]: Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation, E. Komatsu et al. (WMAP), Astrophys. J. Suppl. 180 (2009) 330-376, arXiv:0803.0547.
From the abstract: The WMAP 5-year data provide stringent limits on deviations from the minimal, 6-parameter $\LambdaCDM$ model.... We detect no convincing deviations from the minimal model....
$\Omega_\Lambda = 0.721 +- 0.015$ ,..., $H_0 = 70.1 +- 1.3 \text{km} s^{-1} \text{Mpc}^{-1}$ , $\Omega_b = 0.0462 +- 0.0015$ , $\Omega_c = 0.233 +- 0.013$ ,...
We obtain tight, simultaneous limits on the (constant) equation of state of dark energy and the spatial curvature of the universe: and $-0.0175<\Omega_k<0.0085 \text{(95% CL)}$ ....
We find the limit on the total mass of massive neutrinos of $\sum m_\nu < 0.61 eV \text{(95% CL)}$ , which is free from the uncertainty in the normalization of the large-scale structure data. The number of relativistic degrees of freedom, expressed in units of the effective number of neutrino species, is constrained as $N_{\rm eff} = 4.4 +- 1.5$ (68%), consistent with the standard value of 3.04.
[2-13]: Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Beam Profiles, Data Processing, Radiometer Characterization and Systematic Error Limits, N. Jarosik et al. (WMAP), Astrophys. J. Suppl. 170 (2007) 263, arXiv:astro-ph/0603452. http://lambda.gsfc.nasa.gov/product/map/dr2/pub_papers/threeyear/syserr/wmap_3yr_syserr.pdf.
[2-14]: Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Temperature Results, G. Hinshaw et al. (WMAP), Astrophys. J. Suppl. 170 (2007) 288, arXiv:astro-ph/0603451. http://lambda.gsfc.nasa.gov/product/map/dr2/pub_papers/threeyear/temperature/wmap_3yr_temp.pdf.
[2-15]: Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Polarization Analysis, L. Page et al. (WMAP), Astrophys. J. Suppl. 170 (2007) 335, arXiv:astro-ph/0603450. http://lambda.gsfc.nasa.gov/product/map/dr2/pub_papers/threeyear/polarization/wmap_3yr_pol.pdf.
[2-16]: Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Cosmology, D.N. Spergel et al. (WMAP), Astrophys. J. Suppl. 170 (2007) 377, arXiv:astro-ph/0603449. http://lambda.gsfc.nasa.gov/product/map/dr2/pub_papers/threeyear/parameters/wmap_3yr_param.pdf.
[2-17]: Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Three Year Explanatory Supplement, M. Limon et al. (WMAP), 2006. http://lambda.gsfc.nasa.gov/product/map/dr2/pub_papers/threeyear/supplement/wmap_3yr_supplement.pdf.
[2-18]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Inflation, Peiris, H. V. et al. (WMAP), Astrophys. J. Suppl. 148 (2003) 213, arXiv:astro-ph/0302225.
[2-19]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: On-Orbit Radiometer Characterization, Jarosik, N. et al. (WMAP), Astrophys. J. Suppl. 148 (2003) 29, arXiv:astro-ph/0302224.
[2-20]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Tests of Gaussianity, Komatsu, E. et al. (WMAP), Astrophys. J. Suppl. 148 (2003) 119, arXiv:astro-ph/0302223.
[2-21]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Data Processing Methods and Systematic Errors Limits, Hinshaw, G. et al. (WMAP), Astrophys. J. Suppl. 148 (2003) 63, arXiv:astro-ph/0302222.
[2-22]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Interpretation of the TT and TE Angular Power Spectrum Peaks, Page, L. et al. (WMAP), Astrophys. J. Suppl. 148 (2003) 233, arXiv:astro-ph/0302220.
[2-23]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Parameter Estimation Methodology, Verde, L. et al. (WMAP), Astrophys. J. Suppl. 148 (2003) 195, arXiv:astro-ph/0302218.
[2-24]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Angular Power Spectrum, Hinshaw, G. et al. (WMAP), Astrophys. J. Suppl. 148 (2003) 135, arXiv:astro-ph/0302217.
[2-25]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Galactic Signal Contamination from Sidelobe Pickup, Barnes, C. et al. (WMAP), Astrophys. J. Suppl. 148 (2003) 51, arXiv:astro-ph/0302215.
[2-26]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Beam Profiles and Window Functions, Page, L. et al. (WMAP), Astrophys. J. Suppl. 148 (2003) 39, arXiv:astro-ph/0302214.
[2-27]: Wilkinson Microwave Anisotropy Probe (WMAP) First Year Observations: TE Polarization, Kogut, A. et al. (WMAP), Astrophys. J. Suppl. 148 (2003) 161, arXiv:astro-ph/0302213.
[2-28]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters, Spergel, D. N. et al. (WMAP), Astrophys. J. Supp. Ser. 148 (2003) 175-194, arXiv:astro-ph/0302209.
From the abstract: By combining WMAP data with other astronomical data sets, we constrain the geometry of the universe: $\Omega_{tot} = 1.02 +- 0.02$ , the equation of state of the dark energy, (95% confidence limit), and the energy density in neutrinos, $\Omega_\nu h^2 < 0.0076$ (95% confidence limit). For 3 degenerate neutrino species, this limit implies that their mass is less than 0.23 eV (95% confidence limit). The WMAP detection of early reionization rules out warm dark matter.
[2-29]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Foreground Emission, Bennett, C. et al. (WMAP), Astrophys. J. Suppl. 148 (2003) 97, arXiv:astro-ph/0302208.
[2-30]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Preliminary Maps and Basic Results, Bennett, C. L. et al. (WMAP), Astrophys. J. Supp. Ser. 148 (2003) 1-27, arXiv:astro-ph/0302207.
From the abstract: A best-fit cosmological model to the CMB and other measures of large scale structure works remarkably well with only a few parameters. The age of the best-fit universe is old. Decoupling was $t_{dec} = 379^{+ 8}_{- 7} \text{ kyr}$ after the Big Bang at a redshift of $z_{dec} = 1089 +- 1$ . The thickness of the decoupling surface was $\Delta z_{dec} = 195 +- 2$ . The matter density of the universe is $\Omega_mh^2 = 0.135^{+ 0.008}_{- 0.009}$ , the baryon density is $\Omega_bh^2 = 0.0224 +- 0.0009$ , and the total mass-energy of the universe is $\Omega_{tot} = 1.02 +- 0.02$ .... This flat universe model is composed of 4.4% baryons, 22% dark matter and 73% dark energy.... Inflation theory is supported with , $\Omega_{tot} =~ 1$ , Gaussian random phases of the CMB anisotropy, and superhorizon fluctuations implied by the TE anticorrelations at decoupling.
[2-31]: Design, Implementation and Testing of the MAP Radiometers, N. Jarosik et al., arXiv:astro-ph/0301164, 2003.
[2-32]: The Optical Design and Characterization of the Microwave Anisotropy Probe, L. Page et al., Astrophys. J. 585 (2003) 566, arXiv:astro-ph/0301160.
[2-33]: The MAP Satellite Feed Horns, C. Barnes et al., Astrophys. J. Supp. 143 (2002) 567, arXiv:astro-ph/0301159.
[2-34]: The Microwave Anisotropy Probe (MAP) Mission, C. L. Bennett et al. (WMAP), Astrophys. J. 583 (2003) 1, arXiv:astro-ph/0301158.
[2-35]: CMB Anisotropy Correlation Function and Topology from Simulated Maps for MAP, Park, Changbom et al., Astrophys. J. 506 (1998) 473-484, arXiv:astro-ph/9711057.

3 - Detector

[3-1]: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Explanatory Supplement, M. Limon et al., 2003. http://lambda.gsfc.nasa.gov/product/map/pub_papers/firstyear/supplement/WMAP_supplement.pdf.

4 - Conference Proceedings

[4-1]: Comparing and combining Wilkinson Microwave Anisotropy (WMAP) probe results and Large Scale Structure, Licia verde, arXiv:astro-ph/0306272, 2003. Davis Inflation Meeting, 2003.
[4-2]: WMAP First Year Results, Wright, E. L., arXiv:astro-ph/0306132, 2003. The Cosmic Microwave Background and its Polarization, New Astronomy Reviews.
[4-3]: WMAP Polarization Results, A. Kogut, arXiv:astro-ph/0306048, 2003. "The Cosmic Microwave Background and its Polarization", New Astronomy Reviews.
[4-4]: Future Cosmic Microwave Background Experiments, Halpern, Mark, Scott, Douglas, arXiv:astro-ph/9904188, 1999. ASP, San Francisco, 1999.

Neutrino Unbound

We Can Put an End to Word Attachments

Authors:
Carlo Giunti / giunti@to.infn.it
Marco Laveder / marco.laveder@pd.infn.it

Last Update: Tue 16 Mar 2010, day 75 of the year 2010, 10:03:00 UTC