WMAP

Other Web pages: Spires

References

Useful Links

References

[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.

[2-1]

Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Are There Cosmic Microwave Background Anomalies?, C. L. Bennett et al., Astrophys. J. Suppl. 192 (2011) 17, arXiv:1001.4758.

[2-2]

Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Sky Maps, Systematic Errors, and Basic Results, N. Jarosik et al., Astrophys. J. Suppl. 192 (2011) 14, arXiv:1001.4744.

[2-3]

Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Planets and Celestial Calibration Sources, J. L. Weiland et al., Astrophys. J. Suppl. 192 (2011) 19, arXiv:1001.4731.

[2-4]

Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Power Spectra and WMAP-Derived Parameters, D. Larson et al., Astrophys. J. Suppl. 192 (2011) 16, arXiv:1001.4635.

[2-5]

Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Galactic Foreground Emission, B. Gold et al., Astrophys. J. Suppl. 192 (2011) 15, arXiv:1001.4555.

[2-6]

Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation, E. Komatsu et al. (WMAP), Astrophys. J. Suppl. 192 (2011) 18, arXiv:1001.4538.
From the abstract: Notable examples of improved parameters are the total mass of neutrinos, , and the effective number of neutrino species, , 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 model.... We detect no convincing deviations from the minimal model....
,..., , , ,...
We obtain tight, simultaneous limits on the (constant) equation of state of dark energy and the spatial curvature of the universe: and ....
We find the limit on the total mass of massive neutrinos of , 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 (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: , the equation of state of the dark energy, (95% confidence limit), and the energy density in neutrinos, (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 after the Big Bang at a redshift of . The thickness of the decoupling surface was . The matter density of the universe is , the baryon density is , and the total mass-energy of the universe is .... This flat universe model is composed of 4.4% baryons, 22% dark matter and 73% dark energy.... Inflation theory is supported with , , 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.

[3-1]

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.

[4-1]

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.

Useful Links

LAMBDA, Legacy Archive for Microwave Background Data Analysis

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