60 research outputs found
Median Statistics, H_0, and the Accelerating Universe
(Abridged) We develop median statistics that provide powerful alternatives to
chi-squared likelihood methods and require fewer assumptions about the data.
Applying median statistics to Huchra's compilation of nearly all estimates of
the Hubble constant, we find a median value H_0=67 km/s/Mpc. Median statistics
assume only that the measurements are independent and free of systematic
errors. This estimate is arguably the best summary of current knowledge because
it uses all available data and, unlike other estimates, makes no assumption
about the distribution of measurement errors. The 95% range of purely
statistical errors is +/- 2 km/s/Mpc. The statistical precision of this result
leads us to analyze the range of possible systematic errors in the median,
which we estimate to be roughly +/- 5 km/s/Mpc (95% limits), dominating over
the statistical errors. A Bayesian median statistics treatment of high-redshift
Type Ia supernovae (SNe Ia) apparent magnitude versus redshift data from Riess
et al. yields a posterior probability that the cosmological constant Lambda > 0
of 70 or 89%, depending on the prior information used. The posterior
probability of an open universe is about 47%. Analysis of the Perlmutter et al.
high-redshift SNe Ia data show the best-fit flat-Lambda model favored over the
best-fit Lambda = 0 open model by odds of 366:1; corresponding Riess et al.
odds are 3:1 (assuming prior odds of 1:1).Median statistics analyses of the SNe
Ia data do not rule out a time-variable Lambda model, and may even favor it
over a time-independent Lambda and a Lambda = 0 open model.Comment: Significant revisions include discussion of systematic errors in the
median of H_0. Accepted for publication in The Astrophysical Journal, v548,
February 20, 2001 issue. 47 pages incl. figures and table
Cosmological Parameter Determination from Counts of Galaxies
We study constraints that anticipated DEEP survey galaxy counts versus
redshift data will place on cosmological model parameters in models with and
without a constant or time-variable cosmological constant . This data
will result in fairly tight constraints on these parameters. For example, if
all other parameters of a spatially-flat model with a constant are
known, the galaxy counts data should constrain the nonrelativistic matter
density parameter to about 5% (10%, 1.5%) at 1 with neutral
(worst case, best case) assumptions about data quality.Comment: 15 pages, 6 figure
Supernovae Ia Constraints on a Time-Variable Cosmological "Constant"
The energy density of a scalar field with potential , , behaves like a time-variable cosmological
constant that could contribute significantly to the present energy density.
Predictions of this spatially-flat model are compared to recent Type Ia
supernovae apparent magnitude versus redshift data. A large region of model
parameter space is consistent with current observations. (These constraints are
based on the exact scalar field model equations of motion, not on the widely
used time-independent equation of state fluid approximation equations of
motion.) We examine the consequences of also incorporating constraints from
recent measurements of the Hubble parameter and the age of the universe in the
constant and time-variable cosmological constant models. We also study the
effect of using a non-informative prior for the density parameter.Comment: Accepted for publication in Ap
On the Degeneracy Inherent in Observational Determination of the Dark Energy Equation of State
Using a specific model for the expansion rate of the Universe as a function
of scale factor, it is demonstrated that the equation of state of the dark
energy cannot be determined uniquely from observations at redshifts
unless the fraction of the mass density of the Universe
in nonrelativistic particles, , somehow can be found independently. A
phenomenological model is employed to discuss the utility of additional
constraints from the formation of large scale structure and the positions of
CMB peaks in breaking the degeneracy among models for the dark energy.Comment: 12 pages, 3 figures. Several references adde
A new cosmological tracker solution for Quintessence
In this paper we propose a quintessence model with the potential , which
asymptotic behavior corresponds to an inverse power-law potential at early
times and to an exponential one at late times. We demonstrate that this is a
tracker solution and that it could have driven the Universe into its current
inflationary stage. The exact solutions and the description for a complete
evolution of the Universe are also given. We compare such model with the
current cosmological observations.Comment: 13 pages REVTeX, 5 eps color figure
Cosmological Studies with Radio Galaxies and Supernovae
Physical sizes of extended radio galaxies can be employed as a cosmological
"standard ruler", using a previously developed method. Eleven new radio
galaxies are added to our previous sample of nineteen sources, forming a sample
of thirty objects with redshifts between 0 and 1.8. This sample of radio
galaxies are used to obtain the best fit cosmological parameters in a
quintessence model in a spatially flat universe, a cosmological constant model
that allows for non-zero space curvature, and a rolling scalar field model in a
spatially flat universe. Results obtained with radio galaxies are compared with
those obtained with different supernova samples, and with combined radio galaxy
and supernova samples. Results obtained with different samples are consistent,
suggesting that neither method is seriously affected by systematic errors. Best
fit radio galaxy and supernovae model parameters determined in the different
cosmological models are nearly identical, and are used to determine
dimensionless coordinate distances to supernovae and radio galaxies, and
distance moduli to the radio galaxies. The distance moduli to the radio
galaxies can be combined with supernovae samples to increase the number of
sources, particularly high-redshift sources, in the samples. The constraints
obtained here with the combined radio galaxy plus supernovae data set in the
rolling scalar field model are quite strong. The best fit parameter values
suggest a value of omega is less than about 0.35, and the model parameter alpha
is close to zero; that is, a cosmological constant provides a good description
of the data. We also obtain new constraints on the physics of engines that
power the large-scale radio emission.Comment: 32 pages. Accepted for publication in the Astrophysical Journa
Limitations in using luminosity distance to determine the equation of state of the universe
Supernova searches have been been suggested as a method for determining
precisely the current value and time variation of the equation of state, ,
of the dark energy component responsible for the accelerated expansion of the
Universe. We show that the method is fundamentally limited by the fact that
luminosity dista nce depends on through a multiple integral relation that
smears out information about and its time variatio n. The effect degrades
the resolution of that can be obtained from current d ata.Comment: 4 pages, 2 figures; corrected figure 1 (compared to preprint and
published versions) and minor changes to tex
Unified dark energy models : a phenomenological approach
A phenomenological approach is proposed to the problem of universe
accelerated expansion and of the dark energy nature. A general class of models
is introduced whose energy density depends on the redshift in such a way
that a smooth transition among the three main phases of the universe evolution
(radiation era, matter domination, asymptotical de Sitter state) is naturally
achieved. We use the estimated age of the universe, the Hubble diagram of Type
Ia Supernovae and the angular size - redshift relation for compact and
ultracompact radio structures to test whether the model is in agreement with
astrophysical observation and to constrain its main parameters. Although
phenomenologically motivated, the model may be straightforwardly interpreted as
a two fluids scenario in which the quintessence is generated by a suitably
chosen scalar field potential. On the other hand, the same model may also be
read in the context of unified dark energy models or in the framework of
modified Friedmann equation theories.Comment: 12 pages, 10 figures, accepted for publication on Physical Review
Unified phantom cosmology: inflation, dark energy and dark matter under the same standard
Phantom cosmology allows to account for dynamics and matter content of the
universe tracing back the evolution to the inflationary epoch, considering the
transition to the non-phantom standard cosmology (radiation/matter dominated
eras) and recovering the today observed dark energy epoch. We develop the
unified phantom cosmology where the same scalar plays the role of early time
(phantom) inflaton and late-time Dark Energy. The recent transition from
decelerating to accelerating phase is described too by the same scalar field.
The (dark) matter may be embedded in this scheme, giving the natural solution
of the coincidence problem. It is explained how the proposed unified phantom
cosmology can be fitted against the observations which opens the way to define
all the important parameters of the model.Comment: LaTeX file, 9 pages, no figure, version to appear in PL
Quintessence models in Supergravity
Scalar field models of quintessence typically require that the expectation
value of the field today is of order the Planck mass, if we want them to
explain the observed acceleration of the Universe. This suggests that we should
be considering models in the context of supergravity. We discuss a particular
class of supergravity models and analyze their behavior under different choices
of the Kahler metric.Comment: 6 pages, revised version to appear in PR
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