Bibcode
López-Corredoira, M.
Bibliographical reference
International Journal of Modern Physics D, Volume 22, Issue 7, id. 1350032
Advertised on:
6
2013
Citations
10
Refereed citations
9
Description
In a previous paper (part I), the mathematical properties of the cosmic
microwave background radiation (CMBR) power spectrum which presents
oscillations were discussed. Here, we discuss the physical
interpretation: a power spectrum with oscillations is a rather normal
characteristic expected from any fluid with clouds of overdensities that
emit/absorb radiation or interact gravitationally with the photons, and
with a finite range of sizes and distances for those clouds. The
standard cosmological interpretation of "acoustic" peaks is just a
particular case; peaks in the power spectrum might be generated in
scenarios within some alternative cosmological model that have nothing
to do with oscillations due to gravitational compression in a fluid.
We also calculate the angular correlation function of the anisotropies
from the Wilkinson Microwave Anisotropy Probe (WMAP)-7 yr and ACT data,
in an attempt to derive the minimum number of parameters a polynomial
function should have to fit it: a set of polynomial functions with a
total of ≈ 6 free parameters, apart from the amplitude, is enough to
reproduce the first two peaks. However, the standard model with six
tunable free parameters also reproduces higher-order peaks, giving the
standard model a higher confidence. At present, while no simple function
with six free parameters is found to give a fit as good as the one given
by the standard cosmological model, we may consider the predictive power
of the standard model beyond an instrumentalist approach (such as the
Ptolemaic astronomy model of the orbits of the planets).
Related projects
Cosmology with Large Scale Structure Probes
The Cosmic Microwave Background (CMB) contains the statistical information about the early seeds of the structure formation in our Universe. Its natural counterpart in the local universe is the distribution of galaxies that arises as a result of gravitational growth of those primordial and small density fluctuations. The characterization of the
FRANCISCO SHU
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