WMAP data

Nevertheless, for the moment, we prefer the YU, h2 value from D/H measurements due to Kirkman et al.2003, than the lower values from 4He and 7Li. Indeed Deuterium is the most sensitive "baryometer" among the light nuclei. Finally, the baryon density can be constrained efficiently from CMB measurements (Le Dour et al., 2000), leading to values in agreement with Deuterium measurements See in particular recent constraints obtained from BOOMERANG, DASI, MAXIMA, VS A, CBI, ARCHEOPS and WMAP data. de Bernardis... 

The ratios of the anisotropy powers below the peak at l 50, at the big peak at ss 220, in the trough at / 412, and at the second peak at / 546 were precisely determined using the WMAP data which has a single consistent calibration for all Us. Previously, these I ranges had been measured by different experiments having different calibrations so the ratios were poorly determined. Knowing these ratios determined the photon baryon CDM density ratios, and since the photon density was precisely determined by FIRAS on COBE, accurate values for the baryon density and the dark matter density were obtained. These values are Ct h2 = 0.0224 4%, and Vtmh2 = 0.135 7%. The ratio of CDM to baryon densities from the WMAP data is 5.0 1. 

Better numbers, and independent numbers from other considerations for the standard parameters, for instance W from X-ray clusters, the tilt (or not) of the primordial density spectrum, and the optical depth back to recombination from later WMAP data. Supernova work should improve the limits on the equation of state parameter, w quite soon. 

With the increased precision of microwave background anisotropy measurements, it is now possible to use the CMB to independently determine the baryon density. The 3rd year WMAP data implies [8]... 

Multipole fluctuation strength of the cosmic microwave background radiation as a function of the spherical harmonic index I. The location and the height of the first minimum favors a spatially flat Universe, while the level of the fluctuations in the higher multipoles (/ > 400) Indicates the presence of a low-density baryonic component (<5%). The measurements cover already the damping region (/ > 1,000). Wilkinson Microwave Anisotropy Probe (WMAP) data are displayed together with results of earlier balloon observations (Reprinted from Nolta et al. 2009 with kind permission of the first author, the WMAP Science Team, and AAS)... 

Figure 5.4. Left. The overall SZ effect in Coma produced by the combination of various electron populations thermal hot gas with ksT = 8.2 keV and r = 4.9 10-3 (solid blue curve) which best fits the available SZ data relativistic electrons which best fit the radio-halo spectrum (yellow curve) provide a small additional SZ effect (Colafrancesco 2004a) warm gas with ksT v 0.1 keV and n 10-3 cm-3 (cyan curve) provides a small SZ effect due to its low pressure (Colafrancesco 2004c) DM produced secondary electrons with Mx = 10 (black dotted curve), 20 GeV (black solid curve) and 30 GeV (dashed solid curve). A pure-gaugino x reference model is assumed in the computations. The relative overall SZ effect is shown as the dotted, solid and dashed red curves, respectively. A zero peculiar velocity of Coma is assumed consistently with the available limits. SZ data are from OVRO (magenta), WMAP (cyan) and MITO (blue). Right. The constraints on the

The WMAP mission is made possible by the support of the Office of Space Sciences at NASA Headquarters and by the hard and capable work of scores of scientists, engineers, technicians, machinists, data analysts, budget analysts, managers, administrative staff, and reviewers. 

We expect that all of these mysteries will be cleared up — and new ones generated — by the release of further data from WMAP expected in 2004 and beyond, many ongoing ground- and balloon-based observing campaigns, and eventually the Planck Surveyor satellite, due to be launched in 2007. 

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