Logo
ScienceStack
Table of Contents
Fetching ...
Sign In

Cosmology from Maxima-1, Boomerang and COBE/DMR CMB Observations

A. H. Jaffe, P. A. R. Ade, A. Balbi, J. J Bock, J. R. Bond, J. Borrill, A. Boscaleri, K. Coble, B. P. Crill, P. de Bernardis, P. Farese, P. G. Ferreira, K. Ganga, M. Giacometti, S. Hanany, E. Hivon, V. V. Hristov, A. Iacoangeli, A. E. Lange, A. T. Lee, L. Martinis, S. Masi, P. D. Mauskopf, A. Melchiorri, T. Montroy, C. B. Netterfield, S. Oh, E. Pascale, F. Piacentini, D. Pogosyan, S. Prunet, B. Rabii, S. Rao, P. L. Richards, G. Romeo, J. E. Ruhl, F. Scaramuzzi, D. Sforna, G. F. Smoot, R. Stompor, C. D. Winant, J. H. P. Wu

TL;DR

Results from BOOMERANG-98 and MAXIMA-1 provide consistent and high signal-to-noise measurements of the cosmic microwave background power spectrum at spherical harmonic multipole bands over 2<l less similar to 800, implying the existence of both nonbaryonic dark matter and dark energy in the Universe.

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, $Ω_{\rm {tot}}\simeq 1.11 \pm 0.07 (^{+0.13}_{-0.12})$, the baryon density, $Ω_b h^2\simeq 0.032^{+0.005}_{-0.004} (^{+0.009}_{-0.008})$, 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.

Cosmology from Maxima-1, Boomerang and COBE/DMR CMB Observations

TL;DR

Results from BOOMERANG-98 and MAXIMA-1 provide consistent and high signal-to-noise measurements of the cosmic microwave background power spectrum at spherical harmonic multipole bands over 2<l less similar to 800, implying the existence of both nonbaryonic dark matter and dark energy in the Universe.

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 . Analysis of the combined data yields 68% (95%) confidence limits on the total density, , the baryon density, , and the scalar spectral tilt, . 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.

Paper Structure

This paper contains 3 sections, 2 figures, 1 table.

Table of Contents

  1. Comparison & Calibration.
  2. Cosmological Parameters.
  3. Conclusions.

Figures (2)

  • Figure 1: CMB power spectra, $\mathcal{C}_\ell = \ell(\ell+1)C_\ell/2\pi$. Top: MAXIMA-1, B98 and COBE-DMR. Bottom: maximum-likelihood fit to the power in bands for the three spectra, marginalized over beam and calibration uncertainty. In both panels the curves show the best fit model in the joint parameter estimation with weak priors and the best fit with $\Omega_{\rm {tot}}=1$. These models have {$\Omega_{\rm {tot}}$, $\Omega_\Lambda$, $\Omega_b h^2$, $\Omega_c h^2$,$n_s$,$\tau_C$}$=${1.2, 0.5, 0.03, 0.12, 0.95, 0}, {1, 0.7, 0.03, 0.17, 0.975, 0}. They remain the best fits when the large scale structure prior LSS is added, and when the SN prior SNIa is added the $\Omega_{\rm {tot}}=1$ model becomes the best fit in both cases.
  • Figure 2: Likelihood functions calculated using the weak prior. Top: likelihoods from DMR+B98, DMR+MAXIMA-1 (M-1) apj2diffs, DMR+MAXIMA-1+B98 and DMR+MAXIMA-1+B98+LSS (LSS is the large-scale structure prior LSS). Bottom: the likelihood in ($\Omega_m, \Omega_\Lambda$). Shaded contours nearly parallel to $\Omega_m+\Omega_\Lambda=1$ are one-, two-, and three-sigma limits, defined as the equivalent likelihood ratio for a two-dimensional Gaussian distribution, from DMR+B98+MAXIMA-1 with weak priors (left) and DMR+B98+MAXIMA-1+LSS (right). Contours labeled "SNIa" are from high-redshift supernovae observations SNIa, and the final heavy set of contours are constraints from the product of the two distributions.