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DASI 1st season results Maps: Grid of circles with blue, red, and green blobs. Angular Power Spectrum: Plot of the angular power vs. multipole (l). The COBE measurement is on the far left, blue points from DASI fill in the other bumps and wiggles. The numbers: Vu-graph from 2001 Weak h prior, h> 0.45 and Tau_L <= 0.4 Ω_TOTAL = 1.04±0.06 Ω_B h^2= 0.022 +0.004 - 0.003 Ω_CDM h^2 = 0.14±004 requires dark matter n_s = 1.01 +0.08 -0.06 Strong h prior, h=0.72±0.08 and Tau_L <=0.4 Ω_TOTAL = 1.00 ±0.04 Ω_M = 0.40 ± 0.15 Ω_Lambda= 0.60 ±0.15

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DASI 1st season results Maps: Grid of circles with blue, red, and green blobs. Angular Power Spectrum: Plot of the angular power vs. multipole (l). The COBE measurement is on the far left, blue points from DASI fill in the other bumps and wiggles. The numbers: Vu-graph from 2001 Weak h prior, h> 0.45 and Tau_L <= 0.4 Ω_TOTAL = 1.04±0.06 Ω_B h^2= 0.022 +0.004 - 0.003 Ω_CDM h^2 = 0.14±004 requires dark matter n_s = 1.01 +0.08 -0.06 Strong h prior, h=0.72±0.08 and Tau_L <=0.4 Ω_TOTAL = 1.00 ±0.04 Ω_M = 0.40 ± 0.15 Ω_Lambda= 0.60 ±0.15
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Kelly Lepo (kellylepo@astrodon.social)'s status on Tuesday, 21-Jan-2025 01:35:04 JST Kelly Lepo
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Degree Angular Scale Interferometer at the South Pole made observations of the CMB power spectrum in 1999-2000, a measurement of the size of the fluctuations in the cosmic microwave background in the sky.
These results agreed with the Lambda CDM model of the universe and required the presence of dark matter. The next season they returned and got polarization measurements.

In conversation about 4 months ago from astrodon.social permalink