The locations and amplitudes of three acoustic peaks and two dips in the Boomerang , MAXIMA and DASI measurements of the cosmic microwave background ( CMB ) anisotropy power spectra as well as their statistical confidence levels are determined in a model-independent way .
It is shown that the Boomerang-2001 data ( ( Netterfield et al .
2001 ) ) fixes the location and amplitude of the first acoustic peak at more than 3 \sigma confidence .
The next two peaks and dips are determined at a confidence level above 1 \sigma but below 2 \sigma .
The locations and amplitudes of the first three peaks and two dips are \ell _ { p _ { 1 } } = 212 \pm 17 , A _ { p _ { 1 } } = 5426 \pm 1218 \mu K ^ { 2 } , \ell _ { d _ { 1 } } = 413 \pm 50 , A _ { d _ { 1 } } = 1960 \pm 503 \mu K ^ { 2 } , \ell _ { p _ { 2 } } = 544 \pm 56 , A _ { p _ { 2 } } = 2266 \pm 607 \mu K ^ { 2 } , \ell _ { d _ { 2 } } = 746 \pm 89 , A _ { d _ { 2 } } = 1605 \pm 650 \mu K ^ { 2 } , \ell _ { p _ { 3 } } = 843 \pm 35 , A _ { p _ { 3 } } = 2077 \pm 876 \mu K ^ { 2 } respectively ( 1 \sigma errors include statistical and systematic errors ) .
The MAXIMA and DASI experiments give similar values for the extrema which they determine .
For MAXIMA these are the 1st and 3rd peaks , for DASI the 1st and 2nd peaks and the 1st dip .
Moreover , the locations and amplitudes of the extrema determined from the combined data of all experiments are quite close to the corresponding values extracted from the Boomerang data alone .

In order to use these data in a fast search for cosmological parameters an accurate analytic approximation to calculate CMB peak and dip positions and amplitudes in mixed dark matter models with cosmological constant and curvature is derived and tested .

The determined cosmological parameters from the CMB acoustic extrema data show good agreement with other determinations , especially with the baryon content as deduced from standard nucleosynthesis constraints ( ( Burles et al .
2001 ) ) .
These data supplemented by constraints from direct measurements of some cosmological parameters and data on large scale structure ( LSS ) lead to a best-fit model which agrees with practically all the used experimental data within 1 \sigma .
The best-fit parameters are : \Omega _ { \Lambda } = 0.64 ^ { +0.14 } _ { -0.27 } , \Omega _ { m } = 0.36 ^ { +0.21 } _ { -0.11 } , \Omega _ { b } = 0.047 ^ { +0.093 } _ { -0.024 } , n _ { s } = 1.0 ^ { +0.59 } _ { -0.17 } , h = 0.65 ^ { +0.35 } _ { -0.27 } and \tau _ { c } = 0.15 ^ { +0.95 } _ { -0.15 } .
The best-fit values of \Omega _ { \nu } and T / S are close to zero , their 1 \sigma upper limits are 0.17 and 1.7 respectively .