List of plots shown in Prof. S.
Bonometto's lectures:
Title of the lectures
The polarization tensor for cosmic
radiation, as e.g. CBR
Angular spectra for CBR defined
Spectra and correlation functions.
The Gaussian distribution.
Still on Gaussian/non--Gaussian
distribution.
The COBE data
WMAP data 1
WMAP data 2
Anisotropy spectrum for a SCDM
model
Anisotropy and polarization
spectra for a SCDM model
with different values of cosmic opacity to CMB photons
(due to cosmic reionization)
Behavior of rel./non-rel.
component densities up to z=5
Horizon and Jeans scale.
The oscillatory regime.
The Jeans' scale: definition
The sound speed around
recombination.
The yellow region represents the last-scattering-band
Angular amplitude of the horizon
scale at recombination
CBR spectra for large tau,
including the expected B-mode
of polarization, for primeval
spectral index n=0.99 and 0.95
B-mode due to
primeval GW and B-mode originated by lensing
of E-mode
Cosmic variance (yellow
bands)
Effects of change of
Omega_m. Different colors correspond
to different Omega_m. In the
small squares we zoom on the
regions of the first and second
peak. The shifts have the same
direction on the first and second
peaks.
Effects of change of Omega_b.
Different colors correspond
to different Omega_b. In the small
squares we zoom on the
regions of the first and second peak.
The shifts have opposite
directions on the first and second
peaks.
A model with dynamical DE
(SUGRA potential) compared with
LCDM
A model with dynamical DE
(SUGRA potential) coupled with DM,
compared with LCDM. \beta yields the coupling
intensity.
A model with dynamical DE (SUGRA
potential) coupled with DM,
with a time-dependent
coupling, compared with LCDM
Varying tau and spectral index may
compensate
in the
anisotropy spectrum
Minimal reionization redshift to
have given tau values
for a set
of models.