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What Can Cosmic Microwave Background Observations Already Say About Cosmological Parameters in Open and Critical-Density Cold Dark Matter Models?
Astrophysics · Submitted 8 Jun 1997
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Using an approximate joint likelihood to combine our CMB constraint on Omegta_o h^{1/2} with other cosmological constraints we obtain h=0.58 +/- 0.11 and Omega_o=0.65^+0.16_-0.15.
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The abstract, sentence by sentence
We use a combination of the most recent cosmic microwave background (CMB) flat -band power measurements to place constraints on Hubble's constant h and the total density of the Universe Omega_o in the context of inflation-based cold dark matter (CDM) models with no cosmological constant. We use chisquared minimization to explore the 4-dimensional parameter space having as free parameters, h, Omega_o, the power spectrum slope n and the power spectrum normalization at L=10. Conditioning on Omega_o=1 we obtain h=0.33 +/- 0.08. Allowing Omega_o to be a free parameter reduces the ability of the CMB data to constrain h and we obtain 0.26 < h < 0.97 with a best-fit value at h=0.40. We obtain Omega_o=0.85 and set a lower limit Omega_o > 0.53. A strong correlation between acceptable h and Omega_o values leads to a new constraint: Omega_o h^1/2=0.55 +/- 0.10. A favored open model with Omega_o=0.3 and h=0.70 is more than ~4 sigma from the CMB data best-fit model and is rejected at the 99% CL. High baryonic models (Omega_b h^2 ~0.026) yield the best CMB chi-squared fits and are more consistent with other cosmological constraints. The best-fit model has n=0.91^{+0.29}_{-0.09} and Q=18.0^+1.2_-1.5 uK. The amplitude and position of the dominant peak in the best-fit power spectrum are A_peak=76^+3_-7 uK and L_peak = 260^+30_-20. Unlike the Omega_o=1 case we considered previously, CMB h results are now consistent with the higher values favored by local measurements of h but only if 0.55 >~ Omega_o >~ 0.85. Using an approximate joint likelihood to combine our CMB constraint on Omegta_o h^{1/2} with other cosmological constraints we obtain h=0.58 +/- 0.11 and Omega_o=0.65^+0.16_-0.15.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We use a combination of the most recent cosmic microwave background (CMB) flat -band power measurements to place constraints on Hubble's constant h and the total density of the Universe Omega_o in the context of inflation-based cold dark matter (CDM) models with no cosmological constant. | contribution 0.81 | 0.94 | 0.08 | asserted 0.99 |
| s1 | We use chisquared minimization to explore the 4-dimensional parameter space having as free parameters, h, Omega_o, the power spectrum slope n and the power spectrum normalization at L=10. | method 0.99 | 0.95 | 0.02 | asserted 0.97 |
| s2 | Conditioning on Omega_o=1 we obtain h=0.33 +/- 0.08. | result 1.00 | 0.96 | 0.09 | asserted 1.00 |
| s3 | Allowing Omega_o to be a free parameter reduces the ability of the CMB data to constrain h and we obtain 0.26 < h < 0.97 with a best-fit value at h=0.40. | result 1.00 | 0.96 | 0.15 | asserted 1.00 |
| s4 | We obtain Omega_o=0.85 and set a lower limit Omega_o > 0.53. | result 1.00 | 0.96 | 0.12 | asserted 1.00 |
| s5 | A strong correlation between acceptable h and Omega_o values leads to a new constraint: Omega_o h^1/2=0.55 +/- 0.10. | result 0.97 | 0.95 | 0.32 | asserted 1.00 |
| s6 | A favored open model with Omega_o=0.3 and h=0.70 is more than ~4 sigma from the CMB data best-fit model and is rejected at the 99% CL. | result 0.96 | 0.92 | 0.13 | asserted 1.00 |
| s7 | High baryonic models (Omega_b h^2 ~0.026) yield the best CMB chi-squared fits and are more consistent with other cosmological constraints. | result 0.85 | 0.83 | 0.08 | asserted 0.95 |
| s8 | The best-fit model has n=0.91^{+0.29}_{-0.09} and Q=18.0^+1.2_-1.5 uK. | result 1.00 | 0.95 | 0.08 | asserted 1.00 |
| s9 | The amplitude and position of the dominant peak in the best-fit power spectrum are A_peak=76^+3_-7 uK and L_peak = 260^+30_-20. | result 1.00 | 0.93 | 0.04 | asserted 1.00 |
| s10 | Unlike the Omega_o=1 case we considered previously, CMB h results are now consistent with the higher values favored by local measurements of h but only if 0.55 >~ Omega_o >~ 0.85. | interpretation 0.89 | 0.89 | 0.23 | hedged possibility 0.75 |
| s11 | Using an approximate joint likelihood to combine our CMB constraint on Omegta_o h^{1/2} with other cosmological constraints we obtain h=0.58 +/- 0.11 and Omega_o=0.65^+0.16_-0.15. | result 0.98 | 0.95 | 0.36 | asserted 1.00 |
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Original abstract
We use a combination of the most recent cosmic microwave background (CMB) flat -band power measurements to place constraints on Hubble's constant h and the total density of the Universe Omega_o in the context of inflation-based cold dark matter (CDM) models with no cosmological constant. We use chisquared minimization to explore the 4-dimensional parameter space having as free parameters, h, Omega_o, the power spectrum slope n and the power spectrum normalization at L=10. Conditioning on Omega_o=1 we obtain h=0.33 +/- 0.08. Allowing Omega_o to be a free parameter reduces the ability of the CMB data to constrain h and we obtain 0.26 < h < 0.97 with a best-fit value at h=0.40. We obtain Omega_o=0.85 and set a lower limit Omega_o > 0.53. A strong correlation between acceptable h and Omega_o values leads to a new constraint: Omega_o h^1/2=0.55 +/- 0.10. A favored open model with Omega_o=0.3 and h=0.70 is more than ~4 sigma from the CMB data best-fit model and is rejected at the 99% CL. High baryonic models (Omega_b h^2 ~0.026) yield the best CMB chi-squared fits and are more consistent with other cosmological constraints. The best-fit model has n=0.91^{+0.29}_{-0.09} and Q=18.0^+1.2_-1.5 uK. The amplitude and position of the dominant peak in the best-fit power spectrum are A_peak=76^+3_-7 uK and L_peak = 260^+30_-20. Unlike the Omega_o=1 case we considered previously, CMB h results are now consistent with the higher values favored by local measurements of h but only if 0.55 >~ Omega_o >~ 0.85. Using an approximate joint likelihood to combine our CMB constraint on Omegta_o h^{1/2} with other cosmological constraints we obtain h=0.58 +/- 0.11 and Omega_o=0.65^+0.16_-0.15.
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