853 research outputs found
Single-field inflation constraints from CMB and SDSS data
We present constraints on canonical single-field inflation derived from WMAP
five year, ACBAR, QUAD, BICEP data combined with the halo power spectrum from
SDSS LRG7. Models with a non-scale-invariant spectrum and a red tilt n_s < 1
are now preferred over the Harrison-Zel'dovich model (n_s = 1, tensor-to-scalar
ratio r = 0) at high significance. Assuming no running of the spectral indices,
we derive constraints on the parameters (n_s, r) and compare our results with
the predictions of simple inflationary models. The marginalised credible
intervals read n_s = 0.962^{+0.028}_{-0.026} and r < 0.17 (at 95% confidence
level). Interestingly, the 68% c.l. contours favour mainly models with a convex
potential in the observable region, but the quadratic potential model remains
inside the 95% c.l. contours. We demonstrate that these results are robust to
changes in the datasets considered and in the theoretical assumptions made. We
then consider a non-vanishing running of the spectral indices by employing
different methods, non-parametric but approximate, or parametric but exact.
With our combination of CMB and LSS data, running models are preferred over
power-law models only by a Delta chi^2 ~ 5.8, allowing inflationary stages
producing a sizable negative running -0.063^{+0.061}_{-0.049} and larger
tensor-scalar ratio r < 0.33 at the 95% c.l. This requires large values of the
third derivative of the inflaton potential within the observable range. We
derive bounds on this derivative under the assumption that the inflaton
potential can be approximated as a third order polynomial within the observable
range.Comment: 32 pages, 7 figures. v2: additional references, some typos corrected,
passed to JCAP style. v3: minor changes, matches published versio
Cosmological Parameters Degeneracies and Non-Gaussian Halo Bias
We study the impact of the cosmological parameters uncertainties on the
measurements of primordial non-Gaussianity through the large-scale non-Gaussian
halo bias effect. While this is not expected to be an issue for the standard
LCDM model, it may not be the case for more general models that modify the
large-scale shape of the power spectrum. We consider the so-called local
non-Gaussianity model and forecasts from planned surveys, alone and combined
with a Planck CMB prior. In particular, we consider EUCLID- and LSST-like
surveys and forecast the correlations among and the running of the
spectral index , the dark energy equation of state , the effective
sound speed of dark energy perturbations , the total mass of massive
neutrinos , and the number of extra relativistic degrees of
freedom . Neglecting CMB information on and scales /Mpc, we find that, if is assumed to be known, the
uncertainty on cosmological parameters increases the error on by
10 to 30% depending on the survey. Thus the constraint is
remarkable robust to cosmological model uncertainties. On the other hand, if
is simultaneously constrained from the data, the
error increases by . Finally, future surveys which provide a large
sample of galaxies or galaxy clusters over a volume comparable to the Hubble
volume can measure primordial non-Gaussianity of the local form with a
marginalized 1-- error of the order , after
combination with CMB priors for the remaining cosmological parameters. These
results are competitive with CMB bispectrum constraints achievable with an
ideal CMB experiment.Comment: 17 pages, 1 figure added, typos corrected, comments added, matches
the published versio
The sensitivity of BAO Dark Energy Constraints to General Isocurvature Perturbations
Baryon Acoustic Oscillation (BAO) surveys will be a leading method for
addressing the dark energy challenge in the next decade. We explore in detail
the effect of allowing for small amplitude admixtures of general isocurvature
perturbations in addition to the dominant adiabatic mode. We find that
non-adiabatic initial conditions leave the sound speed unchanged but instead
excite different harmonics. These harmonics couple differently to Silk damping,
altering the form and evolution of acoustic waves in the baryon-photon fluid
prior to decoupling. This modifies not only the scale on which the sound waves
imprint onto the baryon distribution, which is used as the standard ruler in
BAO surveys, but also the shape, width and height of the BAO peak. We discuss
these effects in detail and show how more general initial conditions impact our
interpretation of cosmological data in dark energy studies. We find that the
inclusion of these additional isocurvature modes leads to an increase in the
Dark Energy Task Force Figure of merit by 140% and 60% for the BOSS and ADEPT
experiments respectively when considered in conjunction with Planck data. We
also show that the incorrect assumption of adiabaticity has the potential to
bias our estimates of the dark energy parameters by () for a
single correlated isocurvature mode, and up to () for three
correlated isocurvature modes in the case of the BOSS (ADEPT) experiment. We
find that the use of the large scale structure data in conjunction with CMB
data improves our ability to measure the contributions of different modes to
the initial conditions by as much as 100% for certain modes in the fully
correlated case.Comment: 20 pages, 17 figure
Probing the primordial power spectra with inflationary priors
We investigate constraints on power spectra of the primordial curvature and
tensor perturbations with priors based on single-field slow-roll inflation
models. We stochastically draw the Hubble slow-roll parameters and generate the
primordial power spectra using the inflationary flow equations. Using data from
recent observations of CMB and several measurements of geometrical distances in
the late Universe, Bayesian parameter estimation and model selection are
performed for models that have separate priors on the slow-roll parameters. The
same analysis is also performed adopting the standard parameterization of the
primordial power spectra. We confirmed that the scale-invariant
Harrison-Zel'dovich spectrum is disfavored with increased significance from
previous studies. While current observations appear to be optimally modeled
with some simple models of single-field slow-roll inflation, data is not enough
constraining to distinguish these models.Comment: 23 pages, 3 figures, 7 tables, accepted for publication in JCA
Inter-rater reliability of the EPUAP pressure ulcer classification system using photographs
Background. Many classification systems for grading pressure ulcers are discussed in the literature. Correct identification and classification of a pressure ulcer is important for accurate reporting of the magnitude of the problem, and for timely prevention. The reliability of pressure ulcer classification systems has rarely been tested. Aims and objectives. The purpose of this paper is to examine the inter-rater reliability of classifying pressure ulcers according to the European Pressure Ulcer Advisory Panel classification system when using pressure ulcer photographs.Design. Survey was among pressure ulcer experts.Methods. Fifty-six photographs were presented to 44 pressure ulcer experts. The experts classified the lesions as normal skin, blanchable erythema, pressure ulcer (four grades) or incontinence lesion. Inter-rater reliability was calculated.Results. The multirater-Kappa for the entire group of experts was 0.80 (P < 0.001).Various groups of experts obtained comparable results. Differences in classifications are mainly limited to 1 degree of difference. Incontinence lesions are most often confused with grade 2 (blisters) and grade 3 pressure ulcers (superficial pressure ulcers).Conclusions. The inter-rater reliability of the European Pressure Ulcer Advisory Panel classification appears to be good for the assessment of photographs by experts. The difference between an incontinence lesion and a blister or a superficial pressure ulcer does not always seem clear.Relevance to clinical practice. The ability to determine correctly whether a lesion is a pressure ulcer lesion is important to assess the effectiveness of preventive measures. In addition, the ability to make a correct distinction between pressure ulcers and incontinence lesions is important as they require different preventive measures. A faulty classification leads to mistaken measures and negative results. Photographs can be used as a practice instrument to learn to discern pressure ulcers from incontinence lesions and to get to know the different grades of pressure ulcers. The Pressure Ulcer Classification software package has been developed to facilitate learning
The dark side of curvature
Geometrical tests such as the combination of the Hubble parameter H(z) and
the angular diameter distance d_A(z) can, in principle, break the degeneracy
between the dark energy equation of state parameter w(z), and the spatial
curvature Omega_k in a direct, model-independent way. In practice, constraints
on these quantities achievable from realistic experiments, such as those to be
provided by Baryon Acoustic Oscillation (BAO) galaxy surveys in combination
with CMB data, can resolve the cosmic confusion between the dark energy
equation of state parameter and curvature only statistically and within a
parameterized model for w(z). Combining measurements of both H(z) and d_A(z) up
to sufficiently high redshifts around z = 2 and employing a parameterization of
the redshift evolution of the dark energy equation of state are the keys to
resolve the w(z)-Omega_k degeneracy.Comment: 18 pages, 9 figures. Minor changes, matches version accepted in JCA
Neutrinos in Non-linear Structure Formation - The Effect on Halo Properties
We use N-body simulations to find the effect of neutrino masses on halo
properties, and investigate how the density profiles of both the neutrino and
the dark matter components change as a function of the neutrino mass. We
compare our neutrino density profiles with results from the N-one-body method
and find good agreement. We also show and explain why the Tremaine-Gunn bound
for the neutrinos is not saturated. Finally we study how the halo mass function
changes as a function of the neutrino mass and compare our results with the
Sheth-Tormen semi-analytic formulae. Our results are important for surveys
which aim at probing cosmological parameters using clusters, as well as future
experiments aiming at measuring the cosmic neutrino background directly.Comment: 20 pages, 8 figure
Distribution function approach to redshift space distortions. Part IV: perturbation theory applied to dark matter
We develop a perturbative approach to redshift space distortions (RSD) using
the phase space distribution function approach and apply it to the dark matter
redshift space power spectrum and its moments. RSD can be written as a sum over
density weighted velocity moments correlators, with the lowest order being
density, momentum density and stress energy density. We use standard and
extended perturbation theory (PT) to determine their auto and cross
correlators, comparing them to N-body simulations. We show which of the terms
can be modeled well with the standard PT and which need additional terms that
include higher order corrections which cannot be modeled in PT. Most of these
additional terms are related to the small scale velocity dispersion effects,
the so called finger of god (FoG) effects, which affect some, but not all, of
the terms in this expansion, and which can be approximately modeled using a
simple physically motivated ansatz such as the halo model. We point out that
there are several velocity dispersions that enter into the detailed RSD
analysis with very different amplitudes, which can be approximately predicted
by the halo model. In contrast to previous models our approach systematically
includes all of the terms at a given order in PT and provides a physical
interpretation for the small scale dispersion values. We investigate RSD power
spectrum as a function of \mu, the cosine of the angle between the Fourier mode
and line of sight, focusing on the lowest order powers of \mu and multipole
moments which dominate the observable RSD power spectrum. Overall we find
considerable success in modeling many, but not all, of the terms in this
expansion.Comment: 37 pages, 13 figures, published in JCA
Distribution function approach to redshift space distortions
We develop a phase space distribution function approach to redshift space
distortions (RSD), in which the redshift space density can be written as a sum
over velocity moments of the distribution function. These moments are density
weighted and their lowest orders are density, momentum density, and stress
energy density. The series expansion is convergent on large scales. We perform
an expansion of these velocity moments into helicity modes, which are
eigenmodes under rotation around the axis of Fourier mode direction,
generalizing the scalar, vector, tensor decomposition of perturbations to an
arbitrary order. We show that only equal helicity moments correlate and derive
the angular dependence of the individual contributions to the redshift space
power spectrum in terms of angle mu between wave vector and line of sight. We
show that the dominant term of mu^2 dependence on large scales is the
cross-correlation between the density and scalar part of momentum density,
which can be related to the time derivative of the matter power spectrum.
Additional terms contributing and dominating on small scales are the vector
part of momentum density-momentum density correlations, the energy
density-density correlations, and the scalar part of anisotropic stress
density-density correlations. Similarly, we identify 7 terms contributing to
mu^4 dependence. Some of the advantages of the distribution function approach
are that the series expansion converges on large scales and remains valid in
multi-stream situations. We finish with a brief discussion of implications for
RSD in galaxies relative to dark matter, highlighting the issue of scale
dependent bias of velocity moments correlators.Comment: 12 page
Security of quantum cryptography using balanced homodyne detection
In this paper we investigate the security of a quantum cryptographic scheme
which utilizes balanced homodyne detection and weak coherent pulse (WCP). The
performance of the system is mainly characterized by the intensity of the WCP
and postselected threshold. Two of the simplest intercept/resend eavesdropping
attacks are analyzed. The secure key gain for a given loss is also discussed in
terms of the pulse intensity and threshold.Comment: RevTeX4, 8pages, 7 figure
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