| WMAP |
| Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation |
|
|
|
| (6 March 2008) |
CMBR Temperature
:
|
[COBE-FIRAS,PDG]
|
Hubble Constant
:
|
[HST]
|
Total Energy Density
:
|
[WMAP]
-
[SDSS]
|
Matter Energy Density
(for
):
|
[SCP-SN98]
-
[SST-SN03]
-
[2dFGRS]
[SNLS]
|
Dark Energy Eq.
of State
:
|
[SNLS]
-
(68% CL) [CFHTLS]
|
| [WMAP03] | [SDSS03] | [SDSS04B] | [2dFGRS05] | [B05] | |
Spectral Index
|
|
|
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Baryon Energy Density
|
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Matter Energy Density
|
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Vacuum Energy Density
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Age of Universe
|
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|
| A direct empirical proof of the existence of dark matter |
| (21 August 2006) |
| NASA News, SLAC News |
Flat Lambda-CDM Model
(WMAP data only)
|
WMAP +
SNLS
+
|
WMAP +
SNLS
+
|
WMAP +
HST
|
WMAP + LLS +SNIa
|
(WMAP)
(WMAP +
SDSS)
(WMAP +
2dFGRS)
(CMB + LLS +SNIa)
|
(WMAP +
SDSS)
(WMAP +
2dFGRS)
(CMB + LLS +SNIa)
|
|
|
|
|
|
| The Fourth Data Release of the Sloan Digital Sky Survey |
| (1 August 2005) |
| Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies |
|
| (10 January 2005) |
| Press Release: The Cosmic Yardstick |
| The Third Data Release of the Sloan Digital Sky Survey |
| (8 October 2004) |
| The Second Data Release of the Sloan Digital Sky Survey |
| (16 March 2004) |
| Type Ia Supernova Discoveries at z>1 From the Hubble Space Telescope: Evidence for Past Deceleration and Constraints on Dark Energy Evolution |
| > 99% confidence level for a transition from deceleration to acceleration |
the transition between the two epochs is constrained to be at
|
|
(
at 95% confidence level)
|
| (24 February 2004) |
|
VIRGO,
Simulating the Universe
Living Reviews in Relativity
CMB:
CAMB
(Code for Anisotropies in the Microwave Background),
CosmoMC
(Cosmological MonteCarlo),
CMB Resources,
The Physics of Microwave Background Anisotropies,
CMB Experiments,
LAMBDA
(Legacy Archive for Microwave Background Data Analysis)
CMBFAST:
CMBFAST,
CMBFast Web Interface Form,
CMBEASY,
Modeling the CMB Power Spectrum with CMBFAST
Large Scale Structures:
Probes Of Large Scale Structure,
Large-scale structure,
theory and statistics
Lyman-α
Forest:
Lyman alpha systems and cosmology
Maps:
An Atlas of the Universe,
Logarithmic Maps of the Universe
Further Reading
Yellow Book on Dark Energy
Cosmology links for non-cosmologists
Cosmology Books and Links
Level 5
N.
Kaiser,
Elements of Astrophysics
M.
Hudson,
Cosmology
High-Z SN Search
Quantum Universe
A Review of the Universe - Structures,
Evolutions,
Observations,
and Theories
Ned Wright's Cosmology Tutorial
Links to Cosmology and Cosmic Structure Evolution
APS Neutrino Study
First Principles of Cosmology
by Eric V.
Linder
Cosmology: A Research Briefing
PArthENoPE
(Public Algorithm Evaluating the Nucleosinthesis of Primordial Elements)
ESA-ESO WG on Fundamental Cosmology
The Astrophysics Spectator
1 - Books
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56 - Data Analysis
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59 - History
.
,
and the effective number of neutrino species,
,
which benefit from better determinations of the third peak and
.
model....
We detect no convincing deviations from the minimal model....
,...,
,
,
,...
and
....
,
which is free from the uncertainty in the normalization of the large-scale structure data.
The number of relativistic degrees of freedom,
expressed in units of the effective number of neutrino species,
is constrained as
(68%),
consistent with the standard value of 3.04.
old.
Decoupling was
after the Big Bang at a redshift of
.
The thickness of the decoupling surface was
.
The matter density of the universe is
,
the baryon density is
,
and the total mass-energy of the universe is
....
This flat universe model is composed of 4.4% baryons,
22% dark matter and 73% dark energy....
Inflation theory is supported with
,
,
Gaussian random phases of the CMB anisotropy,
and superhorizon fluctuations implied by the TE anticorrelations at decoupling.
,
the source redshift distribution and systematics,
we constrain
,
the amplitude of the matter power spectrum.
At a fiducial matter density
we find
.
This estimate is in excellent agreement with previous studies.
Combination of our results with those from the Deep component of the CFHTLS enables us to place a constraint on a constant equation of state for the dark energy,
based on cosmic shear data alone.
We find that
at 68% confidence.
.
spectrum,
and negligible neutrino mass,
the preferred parameters are
and a baryon fraction
(1
errors).
...
This analysis therefore implies a density significantly below the standard
: in combination with CMB data from WMAP,
we infer
.
,
,
,
.
separation that is an excellent match to the predicted shape and location of the imprint of the recombination-epoch acoustic oscillations on the low-redshift clustering of matter.
This detection demonstrates the linear growth of structure by gravitational instability between
and the present and confirms a firm prediction of the standard cosmological theory.
The acoustic peak provides a standard ruler by which we can measure the ratio of the distances to
and
to 4% fractional accuracy and the absolute distance to
to 5% accuracy.
From the overall shape of the correlation function,
we measure the matter density
to 8% and find agreement with the value from cosmic microwave background (CMB) anisotropies.
Independent of the constraints provided by the CMB acoustic scale,
we find
.
Including the CMB acoustic scale,
we find that the spatial curvature is
if the dark energy is a cosmological constant.
) cosmology and a
cosmology
function to convert from redshift into comoving distance,
we find best fit values of
and
.
,
and
from the First Year Data Set,
P. Astier et al.
(SNLS),
Astron. Astrophys. 447 (2006) 31,
arXiv:astro-ph/0510447.
,
with all distance measurements involving at least two bands....
Cosmological fits to this first year SNLS Hubble diagram give the following results:
for a flat
model;
and
for a flat cosmology with constant equation of state
when combined with the constraint from the recent Sloan Digital Sky Survey measurement of baryon acoustic oscillations.
,
Nobili, Serena et al.
(Supernova Cosmology Project),
arXiv:astro-ph/0504139, 2005.
.
.
(
),
and are inconsistent with a simple model of evolution or dust as an alternative to dark energy.
(equivalently,
).
When combined with external flat-Universe constraints including the cosmic microwave background and large-scale structure,
we find
(and
at the 95% confidence level) for an assumed static equation of state of dark energy,
.
expected for a cosmological constant (i.e.,
,
),
and are inconsistent with very rapid evolution of dark energy.
,
Brian J. Barris et al.,
Astrophys. J. 602 (2004) 571,
arXiv:astro-ph/0310843.
,
doubling the published number of objects at these redshifts,
and indicates that the evidence for acceleration of the universe is not due to a systematic effect proportional to redshift.
In combination with the recent compilation of
Tonry and others (2003),
we calculate cosmological parameter density contours which are consistent with the flat universe indicated by the CMB [26-87].
Adopting the constraint that
,
we obtain best-fit values of (
,
)=(0.33,
0.67) using 22 SNe from this survey augmented by the literature compilation.
,
,
and
from an Independent Set of Eleven High-Redshift Supernovae Observed with HST,
Knop, Robert A. et al.
(The Supernova Cosmology Project),
Astrophys. J. 598 (2003) 102,
arXiv:astro-ph/0309368.
,
,
and
from eleven supernovae at
-
with high-quality lightcurves measured using WFPC2 on the HST.
This is an independent set of high-redshift supernovae that confirms previous supernova evidence for an accelerating Universe.
The high-quality lightcurves available from photometry on \wfpc\ make it possible for these eleven supernovae alone to provide measurements of the cosmological parameters comparable in statistical weight to the previous results.
Combined with earlier Supernova Cosmology Project data,
the new supernovae yield a measurement of the mass density
(statistical)
(identified systematics),
or equivalently,
a cosmological constant of
(statistical)
(identified systematics),
under the assumptions of a flat universe and that the dark energy equation of state parameter has a constant value
.
When the supernova results are combined with independent flat-universe measurements of
from CMB and galaxy redshift distortion data,
they provide a measurement of
(statistical)
(identified systematic),
if
is assumed to be constant in time.
...
dark energy is required with
.
Supernova Search Team has discovered and observed 8 new supernovae in the redshift interval
.
These independent observations,
analyzed by similar but distinct methods,
confirm the result of Riess and others (1998a) and Perlmutter and others (1999) that supernova luminosity distances imply an accelerating universe.
More importantly,
they extend the redshift range of consistently observed SN Ia to
,
where the signature of cosmological effects has the opposite sign of some plausible systematic effects....
if the equation of state parameter of the dark energy is
,
then
,
and
.
Including the constraint of a flat Universe,
we find
,
independent of any large-scale structure measurements.
Adopting a prior based on the 2dF redshift survey constraint on
and assuming a flat universe,
we find that the equation of state parameter of the dark energy lies in the range
at 95% confidence.
If we further assume that
,
we obtain
at 95% confidence.
in the region of interest (
).
For a flat (
) cosmology we find
(1
statistical)
(identified systematics).
The data are strongly inconsistent with a
flat cosmology,
the simplest inflationary universe model.
An open,
cosmology also does not fit the data well: the data indicate that the cosmological constant is non-zero and positive,
with a confidence of
%,
including the identified systematic uncertainties.
The best-fit age of the universe relative to the Hubble time is
Gyr for a flat cosmology.