1,331 research outputs found
Constraining the dark fluid
Cosmological observations are normally fit under the assumption that the dark
sector can be decomposed into dark matter and dark energy components. However,
as long as the probes remain purely gravitational, there is no unique
decomposition and observations can only constrain a single dark fluid; this is
known as the dark degeneracy. We use observations to directly constrain this
dark fluid in a model-independent way, demonstrating in particular that the
data cannot be fit by a dark fluid with a single constant equation of state.
Parameterizing the dark fluid equation of state by a variety of polynomials in
the scale factor , we use current kinematical data to constrain the
parameters. While the simplest interpretation of the dark fluid remains that it
is comprised of separate dark matter and cosmological constant contributions,
our results cover other model types including unified dark energy/matter
scenarios.Comment: 5 pages, 5 figures incorporated. Updated to new observational data
including SHOES determination of H0; new citations adde
Unified dark energy and dark matter from a scalar field different from quintessence
We explore unification of dark matter and dark energy in a theory containing
a scalar field of non-Lagrangian type, obtained by direct insertion of a
kinetic term into the energy-momentum tensor. This scalar is different from
quintessence, having an equation of state between -1 and 0 and a zero sound
speed in its rest frame. We solve the equations of motion for an exponential
potential via a rewriting as an autonomous system, and demonstrate the
observational viability of the scenario, for sufficiently small exponential
potential parameter \lambda, by comparison to a compilation of kinematical
cosmological data.Comment: 10 pages RevTeX4 with 5 figures incorporate
Reconstructing thawing quintessence with multiple datasets
In this work we model the quintessence potential in a Taylor series
expansion, up to second order, around the present-day value of the scalar
field. The field is evolved in a thawing regime assuming zero initial velocity.
We use the latest data from the Planck satellite, baryonic acoustic
oscillations observations from the Sloan Digital Sky Survey, and Supernovae
luminosity distance information from Union2.1 to constrain our models
parameters, and also include perturbation growth data from the WiggleZ, BOSS
and the 6dF surveys. The supernova data provide the strongest individual
constraint on the potential parameters. We show that the growth data
performance is competitive with the other datasets in constraining the dark
energy parameters we introduce. We also conclude that the combined constraints
we obtain for our model parameters, when compared to previous works of nearly a
decade ago, have shown only modest improvement, even with new growth of
structure data added to previously-existent types of data.Comment: 9 pages, 4 figures and 1 table. Version 2 with minor changes to match
Physical Review D accepted versio
The WMAP normalization of inflationary cosmologies
We use the three-year WMAP observations to determine the normalization of the
matter power spectrum in inflationary cosmologies. In this context, the
quantity of interest is not the normalization marginalized over all parameters,
but rather the normalization as a function of the inflationary parameters n and
r with marginalization over the remaining cosmological parameters. We compute
this normalization and provide an accurate fitting function. The statistical
uncertainty in the normalization is 3 percent, roughly half that achieved by
COBE. We use the k-l relation for the standard cosmological model to identify
the pivot scale for the WMAP normalization. We also quote the inflationary
energy scale corresponding to the WMAP normalization.Comment: 4 pages RevTex4 with two figure
Diisopropylamide and TMP turbo-grignard reagents : a structural rationale for their contrasting reactivities
A neutral dimeric molecule in crystal form, the diisopropylamido turbo-Grignard reagent "(iPr2N)MgClâ
LiCl" (see structure; blue N, red O, green Mg, yellow Cl, black C) separates into several charged ate species in dynamic exchange with each other in THF solution as determined by a combination of EXSY and DOSY NMR studies
Comment on `Tainted evidence: cosmological model selection versus fitting', by Eric V. Linder and Ramon Miquel (astro-ph/0702542v2)
In astro-ph/0702542v2, Linder and Miquel seek to criticize the use of
Bayesian model selection for data analysis and for survey forecasting and
design. Their discussion is based on three serious misunderstandings of the
conceptual underpinnings and application of model-level Bayesian inference,
which invalidate all their main conclusions. Their paper includes numerous
further inaccuracies, including an erroneous calculation of the Bayesian
Information Criterion. Here we seek to set the record straight.Comment: 6 pages RevTeX
On the prior dependence of constraints on the tensor-to-scalar ratio
We investigate the prior dependence of constraints on cosmic tensor
perturbations. Commonly imposed is the strong prior of the single-field
inflationary consistency equation, relating the tensor spectral index nT to the
tensor-to-scalar ratio r. Dropping it leads to significantly different
constraints on nT, with both positive and negative values allowed with
comparable likelihood, and substantially increases the upper limit on r on
scales k = 0.01 Mpc^-1 to 0.05 Mpc^-1, by a factor of ten or more. Even if the
consistency equation is adopted, a uniform prior on r on one scale does not
correspond to a uniform one on another; constraints therefore depend on the
pivot scale chosen. We assess the size of this effect and determine the optimal
scale for constraining the tensor amplitude, both with and without the
consistency relation.Comment: 14 pages, 6 figures. v2: added references. v3: minor clarifications;
added reference; matches version accepted by JCA
A Nested Sampling Algorithm for Cosmological Model Selection
The abundance of new cosmological data becoming available means that a wider
range of cosmological models are testable than ever before. However, an
important distinction must be made between parameter fitting and model
selection. While parameter fitting simply determines how well a model fits the
data, model selection statistics, such as the Bayesian Evidence, are now
necessary to choose between these different models, and in particular to assess
the need for new parameters. We implement a new evidence algorithm known as
nested sampling, which combines accuracy, generality of application and
computational feasibility, and apply it to some cosmological datasets and
models. We find that a five-parameter model with Harrison-Zel'dovich initial
spectrum is currently preferred.Comment: 4 pages, 3 figures. Minor updates to match version accepted by
Astrophys J Letter
Optimizing future dark energy surveys for model selection goals
We demonstrate a methodology for optimizing the ability of future dark energy
surveys to answer model selection questions, such as `Is acceleration due to a
cosmological constant or a dynamical dark energy model?'. Model selection
Figures of Merit are defined, exploiting the Bayes factor, and surveys
optimized over their design parameter space via a Monte Carlo method. As a
specific example we apply our methods to generic multi-fibre baryon acoustic
oscillation spectroscopic surveys, comparable to that proposed for SuMIRe PFS,
and present implementations based on the Savage-Dickey Density Ratio that are
both accurate and practical for use in optimization. It is shown that whilst
the optimal surveys using model selection agree with those found using the Dark
Energy Task Force (DETF) Figure of Merit, they provide better informed
flexibility of survey configuration and an absolute scale for performance; for
example, we find survey configurations with close to optimal model selection
performance despite their corresponding DETF Figure of Merit being at only 50%
of its maximum. This Bayes factor approach allows us to interpret the survey
configurations that will be good enough for the task at hand, vital especially
when wanting to add extra science goals and in dealing with time restrictions
or multiple probes within the same project.Comment: 12 pages, 16 figure
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