Cosmological implications of the MAXIMA-I high resolution Cosmic Microwave Background anisotropy measurement

TL;DR

This paper analyzes high-resolution MAXIMA-I CMB measurements to test inflationary predictions and to search for a third acoustic peak. It reports a statistically significant excess power near $\ell \sim 860$, consistent with a third peak, and uses a seven-parameter inflationary model grid with COBE-DMR data to derive cosmological constraints. The results indicate a near-flat or mildly curved universe with $\Omega \approx 0.9$, $\Omega_b h^2 \approx 0.033$, and $\Omega_{cdm} h^2 \approx 0.17$, with a degeneracy between $\tau_c$ and $n_s$. Overall, the findings reinforce inflationary coherent perturbations, constrain non-standard models, and align with independent SN Ia measurements of the matter and vacuum-energy densities.

Abstract

We discuss the cosmological implications of the new constraints on the power spectrum of the Cosmic Microwave Background Anisotropy derived from a new high resolution analysis of the MAXIMA-1 measurement (Lee et al. 2001). The power spectrum shows excess power at $\ell \sim 860$ over the average level of power at $411 \le\ell \le 785.$ This excess is statistically significant on the 95% confidence level. Such a feature is consistent with the presence of a third acoustic peak, which is a generic prediction of inflation-based models. The height and the position of the excess power match the predictions of a family of inflationary models with cosmological parameters that are fixed to fit the CMB data previously provided by BOOMERANG-LDB and MAXIMA-1 experiments (e.g., Jaffe et al.2001). Our results, therefore, lend support for inflationary models and more generally for the dominance of coherent perturbations in the structure formation of the Universe. At the same time, they seem to disfavor a large variety of the non-standard (but still inflation-based) models that have been proposed to improve the quality of fits to the CMB data and consistency with other cosmological observables. Within standard inflationary models, our results combined with the COBE-DMR data give best fit values and 95% confidence limits for the baryon density, $Ω_b h^2\simeq 0.033{\pm 0.013}$, and the total density, $Ω=0.9{+0.18\atop -0.16}$. The primordial spectrum slope ($n_s$) and the optical depth to the last scattering surface ($τ_c$) are found to be degenerate and to obey the relation $n_s \simeq 0.46 τ_c + (0.99 \pm 0.14)$, for $τ_c \le 0.5$ (all 95% c.l.).