LAMBDA News
Wilkinson Microwave Anisotropy Probe
The data made available through this page has been updated. The most recent version of this data may be accessed through /product/map/current/
Analysis of the WMAP data involved the computation of cosmological parameters assuming a variety of models and including a variety of datasets in addition to the WMAP dataset. The various model/dataset combinations that were tested are displayed in a matrix; the combinations that were analyzed have links in the corresponding cells to individual display pages that show the cosmological parameters computed using that combination of model and dataset. A printable version of each list of parameters is made available as a Postscript file through a link its corresponding the individual display page.
Mnemonics are used to identify the models and datasets in the table and the individual model/dataset displays. The following table translate the mnemonics:
| Mnemonic | Description |
|---|---|
| Models | |
| lcdm | ΛCDM |
| lcdm+kcutlin | ΛCDM + primordial spectrum with sharp cutoff and linear prior |
| lcdm+kcutlog | ΛCDM + primordial spectrum with sharp cutoff and log prior |
| lcdm+mnu | ΛCDM + massive neutrinos |
| lcdm+mnu+nrel | ΛCDM + massive neutrinos + number of relativistic species |
| lcdm+nrel | ΛCDM + number of relativistic species |
| lcdm+ns=1 | ΛCDM + scale invariant fluctuations (ns=1) |
| lcdm+run | ΛCDM + running scalar spectral index |
| lcdm+run+tens | ΛCDM + running spectral index + Tensor Modes |
| lcdm+sz=0 | ΛCDM with the SZ amplitude set to zero. |
| lcdm+tau=0 | ΛCDM + no reionization (τ=0) |
| lcdm+tens | ΛCDM + Tensor Modes |
| lcdm+xe1step | ΛCDM + step reionization |
| m2phi2 | ΛCDM assuming m2&phi2 inflation with N=60 e-folds. |
| ocdm | Open CDM |
| ocdm+omegac=0 | Open CDM + No Dark Matter (Ωc=0, ΩΛ≠0) |
| ocdm+omegal=0 | Open CDM + No Cosmological Constant (Ωc≠0, ΩΛ=0) |
| ocdm+w | Open CDM + w, (w = constant) |
| pkrec | primordial spectrum freely varying in 15 bins in k space |
| wcdm+mnu | wCDM + massive neutrinos, (w = constant) |
| wcdm+nopert | wCDM + no perturbtaions, (w = constant) |
| wcdm+pert | wCDM + perturbations, (w = constant) |
| Datasets | |
| wmap | WMAP 3 year data set |
| 2df | 2dF Galaxy Redshift Survey (Cole, et.al., 2005) |
| bao | Baryonic Acoustic Oscillations (Eisenstein, et.al., 2005) |
| boom+acbar | BOOMERanG + ACBAR (Montroy, et.al., 2005, Kuo, et.al., 2004) |
| cbi+vsa | CBI + VSA (Readhead, et.al., 2004, Dickinson, et.al., 2004) |
| hst | Hubble Space Telescope Key Project (Freedman, et.al., 2001) |
| sdss | Sloan Digital Sky Survey, (Tegmark, et.al., 2004; Eisenstein, et.al., 2005) |
| sn astier | Supernova Legacy Survey (SNLS) (Astier, et.al., 2005) |
| sn gold | Supernova "Gold Sample" (Riess, et.al., 2004) |
| wl | Weak Lensing (Semboloni, et.al., 2005; Hoekstra, et.al., 2005) |
| all | All data sets combined, excludes BAO, HST and Weak Lensing |
As mentioned previously, each model/dataset combination has an individual display page that shows the WMAP measurements of the cosmological parameters, with a link to a Postscript file showing the same parameters. These display pages also contain links to files containing WMAP's best fit Cl's, best fit matter power spectra, and Monte Carlo Markov Chains. The Markov Chain are supplied in a compressed tarball that contains a README file describing the contents. The spectra files contain:
- Best fit Cl scalar files contain four columns: l, TT, EE, and TE. The tensor and total files contain five columns: l, TT, EE, BB, and TE. The Cl columns are scaled: T02 l (l + 1) Cl / 2&pi in µK2;
- Best fit matter power spectra files contain two columns. The first column is k/h in units of Mpc-1. The second column is the linear matter power spectrum P(k), defined such that the variance is: σ2 = (2π)-3 ∫d3k P(k)
Additional Information
- Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Beam Profiles, Data Processing, Radiometer Characterization and Systematic Error Limits, N. Jarosik, et.al. (2006)
- Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Temperature Analysis, G. Hinshaw, et.al. (2006)
- Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Polarization Analysis, L. Page, et.al. (2006)
- Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Cosmology, D. Spergel, et.al (2006).
- WMAP Three Year Explanatory Supplement
- Cole, et.al., 2005, MNRAS, 362, 505
- Eisenstein, et.al., 2005, ApJ, 633, 560
- Montroy, et.al., 2005, ApJ, submitted
- Kuo, et.al., 2004, ApJ, 600, 32
- Readhead, et.al., 2004, ApJ, 609, 498
- Dickinson, et.al., 2004, MNRAS, 353, 732
- Freedman, et.al., 2004, ApJ, 553, 47
- Tegmark, et.al., 2004, ApJ, 606, 702
- Astier, et.al., 2006, AA, 447, 31
- Riess, et.al., 2004, ApJ, 607, 665
- Semboloni, et.al., 2005, ApJ, submitted
- Hoekstra, et.al., 2005, ApJ, submitted
