195 research outputs found
Coupled dark energy and dark matter from dilatation anomaly
Cosmological runaway solutions may exhibit an exact dilatation symmetry in
the asymptotic limit of infinite time. In this limit, the massless dilaton or
cosmon could be accompanied by another massless scalar field - the geon. At
finite time, small time-dependent masses for both the cosmon and geon are still
present due to imperfect dilatation symmetry. For a sufficiently large mass the
geon will start oscillating and play the role of dark matter, while the cosmon
is responsible for dark energy. The common origin of the mass of both fields
leads to an effective interaction between dark matter and dark energy.
Realistic cosmologies are possible for a simple form of the effective
cosmon-geon-potential. We find an inverse geon mass of a size where it could
reduce subgalactic structure formation.Comment: 4 pages, 2 figure
Dark Matter & Dark Energy from a single scalar field: CMB spectrum and matter transfer function
The dual axion model (DAM), yielding bot DM and DE form a PQ-like scalar
field solving the strong CP problem, is known to allow a fair fit of CMB data.
Recently, however, it was shown that its transfer function exhibits significant
anomalies, causing difficulties to fit deep galaxy sample data. Here we show
how DAM can be modified to agree with the latter data set. The modification
follows the pattern suggested to reconcile any PQ-like approach with gravity.
Modified DAM allows precise predictions which can be testable against future
CMB and/or deep sample data.Comment: 15 pages, 8 figures, accepted for publication in JCA
Modeling Dynamical Dark Energy
Cosmological models with different types of Dark Energy are becoming viable
alternatives for standard models with the cosmological constant. Yet, such
models are more difficult to analyze and to simulate. We present analytical
approximations and discuss ways of making simulations for two families of
models, which cover a wide range of possibilities and include models with both
slow and fast changing ratio w=p\rho. More specifically, we give analytical
expressions for the evolution of the matter density parameter Omega_m(z) and
the virial density contrast Delta_c at any redshift z. The latter is used to
identify halos and to find their virial masses. We also provide an
approximation for the linear growth factor of linear fluctuations between
redshift z=40 and z=0. This is needed to set the normalization of the spectrum
of fluctuations. Finally, we discuss the expected behavior of the halo mass
function and its time evolution.Comment: 10 pages, 10 figures ApJ submitte
Tracing the Nature of Dark Energy with Galaxy Distribution
Dynamical Dark Energy (DE) is a viable alternative to the cosmological
constant. Yet, constructing tests to discriminate between Lambda and dynamical
DE models is difficult because the differences are not large. In this paper we
explore tests based on the galaxy mass function, the void probability function
(VPF), and the number of galaxy clusters. At high z the number density of
clusters shows large differences between DE models, but geometrical factors
reduce the differences substantially. We find that detecting a model dependence
in the cluster redshift distribution is a hard challenge. We show that the
galaxy redshift distribution is potentially a more sensitive characteristics.
We do so by populating dark matter halos in Nbody simulations with galaxies
using well-tested Halo Occupation Distribution (HOD). We also estimate the Void
Probability Function and find that, in samples with the same angular surface
density of galaxies in different models, the VPF is almost model independent
and cannot be used as a test for DE. Once again, geometry and cosmic evolution
compensate each other. By comparing VPF's for samples with fixed galaxy mass
limits, we find measurable differences.Comment: 12 pages, 11 figures, dependence on mass-luminosity relation
discussed, minor changes to match the accepted version by MNRA
Universe acceleration and fine structure constant variation in BSBM theory
In this work we investigate the utility of using SNe Ia observations in
constraining the cosmological parameters in BSBM theory where a scalar field is
responsible for both fine structure constant variation and late time universe
acceleration. The model is discussed in the presence of an exponential self
potential for the scalar field. Stability and phase space analysis of the
solutions are studied. The model is tested against observational data for
Hubble parameter and quasar absorption spectra. With the best fitted model
parameters, the theory predicts a good match with the experimental results and
exhibits fine structure constant variation. The analysis also shows that for
the equation of state parameter, recent universe acceleration and possible
phantom crossing in future is forecasted.Comment: 14 pages, 10 figures, final version with minor modification accepted
to be published in JCA
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