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Cosmology from Maxima-1, Boomerang and COBE/DMR CMB Observations
Astrophysics · Submitted 22 Jul 2000
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Taken together with other cosmological observations, they imply the existence of both non-baryonic dark matter and dark energy in the universe.
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The abstract, sentence by sentence
Recent results from BOOMERANG-98 and MAXIMA-1, taken together with COBE-DMR, provide consistent and high signal-to-noise measurements of the CMB power spectrum at spherical harmonic multipole bands over $2<\ell\lta800$. Analysis of the combined data yields 68% (95%) confidence limits on the total density, $\Omega_{\rm {tot}}\simeq 1.11 \pm 0.07 (^{+0.13}_{-0.12})$, the baryon density, $\Omega_b h^2\simeq 0.032^{+0.005}_{-0.004} (^{+0.009}_{-0.008})$, and the scalar spectral tilt, $n_s\simeq1.01^{+0.09}_{-0.07} (^{+0.17}_{-0.14})$. These data are consistent with inflationary initial conditions for structure formation. Taken together with other cosmological observations, they imply the existence of both non-baryonic dark matter and dark energy in the universe.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Recent results from BOOMERANG-98 and MAXIMA-1, taken together with COBE-DMR, provide consistent and high signal-to-noise measurements of the CMB power spectrum at spherical harmonic multipole bands over $2<\ell\lta800$. | result 0.39 | 0.47 | 0.05 | asserted 1.00 |
| s1 | Analysis of the combined data yields 68% (95%) confidence limits on the total density, $\Omega_{\rm {tot}}\simeq 1.11 \pm 0.07 (^{+0.13}_{-0.12})$, the baryon density, $\Omega_b h^2\simeq 0.032^{+0.005}_{-0.004} (^{+0.009}_{-0.008})$, and the scalar spectral tilt, $n_s\simeq1.01^{+0.09}_{-0.07} (^{+0.17}_{-0.14})$. | result 1.00 | 0.93 | 0.30 | asserted 1.00 |
| s2 | These data are consistent with inflationary initial conditions for structure formation. | interpretation 0.98 | 0.50 | 0.12 | hedged possibility 0.94 |
| s3 | Taken together with other cosmological observations, they imply the existence of both non-baryonic dark matter and dark energy in the universe. | interpretation 1.00 | 0.45 | 0.50 | asserted 0.80 |
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The paper
Original abstract
Recent results from BOOMERANG-98 and MAXIMA-1, taken together with COBE-DMR, provide consistent and high signal-to-noise measurements of the CMB power spectrum at spherical harmonic multipole bands over $2<\ell\lta800$. Analysis of the combined data yields 68% (95%) confidence limits on the total density, $\Omega_{\rm {tot}}\simeq 1.11 \pm 0.07 (^{+0.13}_{-0.12})$, the baryon density, $\Omega_b h^2\simeq 0.032^{+0.005}_{-0.004} (^{+0.009}_{-0.008})$, and the scalar spectral tilt, $n_s\simeq1.01^{+0.09}_{-0.07} (^{+0.17}_{-0.14})$. These data are consistent with inflationary initial conditions for structure formation. Taken together with other cosmological observations, they imply the existence of both non-baryonic dark matter and dark energy in the universe.
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References
How the literature uses it
20 arXiv papers cite this in 25 sentences
Papers citing it · 19 sentences without a confident label
Uses its data or values 2 papers
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In the year 2000, data from the Boomerang and MAXIMA experiments (with supernova measurements) gave $_m h^2 = 0.13 ±0.05$ with error bars that shrink to $±0.01$ taking into account other measurements or assumptions (e.g., LSS, Hubble-constant, and supernova measurements, and/or the assumption of a flat Universe) [ref] .
Dark Matter Astrophysics · Cosmic Microwave Background and Large-Scale Structure · 0.99
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The uniform and isotropic radiation observed corresponds to the most perfect black-body radiation ever measured, peaking at $λ= 1.9 mm$, with a red-shifted temperature of $T_CMB = 2.725 Kelvin$ [ref] .
Primordial Black Holes in non-linear perturbation theory · Cosmological observations and the Big Bang · 0.94
Cites it as background 4 papers
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This combined with measurements of the Cosmic Microwave Background (CMB) radiation [ref] and the Baryonic Acoustic Oscillations (BAO) [ref] , gave rise to the currently preferred $Λ$CDM model of cosmology, according to which our universe has a positive and small cosmological constant.
A new light on the darkest corner of the landscape · Introduction · 0.86
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Shortly before the turn of the millennium we learned that the universe is currently undergoing a phase of accelerated expansion [ref] , which reveals the existence of what is usually referred to as dark energy.
Out of the Swampland with Multifield Quintessence? · Introduction · 0.96
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The standard $Λ$CDM model of cosmology provides the most successful description of the large-scale Universe, accounting for observations across widely separated cosmic epochs and physical scales, from primordial Big Bang Nucleosynthesis (BBN) [ref] and the Cosmic Microwave Background (CMB) [ref] to late-time probes such as baryon acoustic oscillations (BAO) [ref] , galaxy surveys [ref] , and Type Ia supernovae (SNIa) [ref] .
Intertwined Constraints in Extended Cosmologies: Dark Energy, Curvature, Neutrinos, and Inflation · Introduction · 0.96
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