2,665 research outputs found
A Taste of Cosmology
This is the summary of two lectures that aim to give an overview of
cosmology. I will not try to be too rigorous in derivations, nor to give a full
historical overview. The idea is to provide a "taste" of cosmology and some of
the interesting topics it covers. The standard cosmological model is presented
and I highlight the successes of cosmology over the past decade or so. Keys to
the development of the standard cosmological model are observations of the
cosmic microwave background and of large-scale structure, which are introduced.
Inflation and dark energy and the outlook for the future are also discussed.
Slides from the lectures are available from the school website:
physicschool.web.cern.ch/PhysicSchool/CLASHEP/CLASHEP2011/.Comment: 16 pages, contribution to the 2011 CERN-Latin-American School of
High-Energy Physics, Natal, Brazil, 23 March-5 April 2011, edited by C.
Grojean, M. Mulders and M. Spiropul
Large-scale bias in the Universe: bispectrum method
Evidence that the Universe may be close to the critical density, required for
its expansion eventually to be halted, comes principally from dynamical studies
of large-scale structure. These studies either use the observed peculiar
velocity field of galaxies directly, or indirectly by quantifying its
anisotropic effect on galaxy clustering in redshift surveys. A potential
difficulty with both such approaches is that the density parameter
is obtained only in the combination , if linear
perturbation theory is used. The determination of the density parameter
is therefore compromised by the lack of a good measurement of the
bias parameter , which relates the clustering of sample galaxies to the
clustering of mass.
In this paper, we develop an idea of Fry (1994), using second-order
perturbation theory to investigate how to measure the bias parameter on large
scales. The use of higher-order statistics allows the degeneracy between
and to be lifted, and an unambiguous determination of
then becomes possible. We apply a likelihood approach to the bispectrum, the
three-point function in Fourier space. This paper is the first step in turning
the idea into a practical proposition for redshift surveys, and is principally
concerned with noise properties of the bispectrum, which are non-trivial. The
calculation of the required bispectrum covariances involves the six-point
function, including many noise terms, for which we have developed a generating
functional approach which will be of value in calculating high-order statistics
in general.Comment: 12 pages, latex, 7 postscript figures included. Accepted by MNRAS.
(Minor numerical typesetting errors corrected: results unchanged
The nonlinear redshift-space power spectrum of galaxies
We study the power spectrum of galaxies in redshift space, with third order
perturbation theory to include corrections that are absent in linear theory. We
assume a local bias for the galaxies: i.e. the galaxy density is sampled from
some local function of the underlying mass distribution. We find that the
effect of the nonlinear bias in real space is to introduce two new features:
first, there is a contribution to the power which is constant with wavenumber,
whose nature we reveal as essentially a shot-noise term. In principle this
contribution can mask the primordial power spectrum, and could limit the
accuracy with which the latter might be measured on very large scales.
Secondly, the effect of second- and third-order bias is to modify the effective
bias (defined as the square root of the ratio of galaxy power spectrum to
matter power spectrum). The effective bias is almost scale-independent over a
wide range of scales. These general conclusions also hold in redshift space. In
addition, we have investigated the distortion of the power spectrum by peculiar
velocities, which may be used to constrain the density of the Universe. We look
at the quadrupole-to-monopole ratio, and find that higher-order terms can mimic
linear theory bias, but the bias implied is neither the linear bias, nor the
effective bias referred to above. We test the theory with biased N-body
simulations, and find excellent agreement in both real and redshift space,
providing the local biasing is applied on a scale whose fractional r.m.s.
density fluctuations are .Comment: 13 pages, 7 figures. Accepted by MNRA
Tests for primordial non-Gaussianity
We investigate the relative sensitivities of several tests for deviations
from Gaussianity in the primordial distribution of density perturbations. We
consider models for non-Gaussianity that mimic that which comes from inflation
as well as that which comes from topological defects. The tests we consider
involve the cosmic microwave background (CMB), large-scale structure (LSS),
high-redshift galaxies, and the abundances and properties of clusters. We find
that the CMB is superior at finding non-Gaussianity in the primordial
gravitational potential (as inflation would produce), while observations of
high-redshift galaxies are much better suited to find non-Gaussianity that
resembles that expected from topological defects. We derive a simple expression
that relates the abundance of high-redshift objects in non-Gaussian models to
the primordial skewness.Comment: 6 pages, 2 figures, MNRAS in press (minor changes to match the
accepted version
Reducing sample variance: halo biasing, non-linearity and stochasticity
Comparing clustering of differently biased tracers of the dark matter
distribution offers the opportunity to reduce the cosmic variance error in the
measurement of certain cosmological parameters. We develop a formalism that
includes bias non-linearities and stochasticity. Our formalism is general
enough that can be used to optimise survey design and tracers selection and
optimally split (or combine) tracers to minimise the error on the
cosmologically interesting quantities. Our approach generalises the one
presented by McDonald & Seljak (2009) of circumventing sample variance in the
measurement of . We analyse how the bias, the noise,
the non-linearity and stochasticity affect the measurements of and explore
in which signal-to-noise regime it is significantly advantageous to split a
galaxy sample in two differently-biased tracers. We use N-body simulations to
find realistic values for the parameters describing the bias properties of dark
matter haloes of different masses and their number density.
We find that, even if dark matter haloes could be used as tracers and
selected in an idealised way, for realistic haloes, the sample variance limit
can be reduced only by up to a factor .
This would still correspond to the gain from a three times larger survey volume
if the two tracers were not to be split. Before any practical application one
should bear in mind that these findings apply to dark matter haloes as tracers,
while realistic surveys would select galaxies: the galaxy-host halo relation is
likely to introduce extra stochasticity, which may reduce the gain further.Comment: 21 pages, 13 figures. Published version in MNRA
Exploring data and model poisoning attacks to deep learning-based NLP systems
Natural Language Processing (NLP) is being recently explored also to its application in supporting malicious activities and objects detection. Furthermore, NLP and Deep Learning have become targets of malicious attacks too. Very recent researches evidenced that adversarial attacks are able to affect also NLP tasks, in addition to the more popular adversarial attacks on deep learning systems for image processing tasks. More precisely, while small perturbations applied to the data set adopted for training typical NLP tasks (e.g., Part-of-Speech Tagging, Named Entity Recognition, etc..) could be easily recognized, models poisoning, performed by the means of altered data models, typically provided in the transfer learning phase to a deep neural networks (e.g., poisoning attacks by word embeddings), are harder to be detected. In this work, we preliminary explore the effectiveness of a poisoned word embeddings attack aimed at a deep neural network trained to accomplish a Named Entity Recognition (NER) task. By adopting the NER case study, we aimed to analyze the severity of such a kind of attack to accuracy in recognizing the right classes for the given entities. Finally, this study represents a preliminary step to assess the impact and the vulnerabilities of some NLP systems we adopt in our research activities, and further investigating some potential mitigation strategies, in order to make these systems more resilient to data and models poisoning attacks
Assessment and validation of wildfire susceptibility and hazard in Portugal
A comprehensive methodology to assess forest fire susceptibility, that uses variables of strong spatial correlation, is presented and applied for the Portuguese mainland. Our study is based on a thirty-year chronological series of burnt areas. The first twenty years (1975â1994) are used for statistical modelling, and the last ten (1995â2004) are used for the independent validation of results. The wildfire affected areas are crossed with a set of independent layers that are assumed to be relevant wildfire conditioning factors: elevation, slope, land cover, rainfall and temperature. Moreover, the wildfire recurring pattern is also considered, as a proxy variable expressing the influence of human action in wildfire occurrence. A sensitivity analysis is performed to evaluate the weight of each individual theme within the susceptibility model. Validation of the wildfire susceptibility models is made through the computation of success rate and prediction rate curves. The results show that it is possible to have a good compromise between the number of variables within the model and the model predictive power. Additionally, it is shown that integration of climatic variables does not produce any relevant increase in the prediction capacity of wildfire susceptibility models. Finally, the prediction rate curves produced by the independent cross validation are used to assess the probabilistic wildfire hazard at a scenario basis, for the complete mainland Portuguese territory
La dermatitis alérgica a la picadura de pulga : estudio de factores epidemiológicos en el årea urbana de Zaragoza. :
Se estudiaron 101 casos seleccionados de entre los que llegaron a la consulta de dermatologia a lo largo de un año y se analizaron los resultados de un cuestionario epidemiologico que se aplico a cada uno de los casos. Despues de aplicar el tratamiento estadistico a los datos, se encontraron cuatro factores significativos (p<0, 05)que interfieren en la presentacion de la enfermedad. Tres de estos factores se consideran factores de riesgo: edad de presentacion de los primeros signos clinicos, estacion en la qeu se manifiesta el prurito e infestacion por pulgas. El control de las pulgas se manifesto como un factor de proteccion
Evolution of the decay mechanisms in central collisions of + from = 8 to 29
Collisions of Xe+Sn at beam energies of = 8 to 29 and leading to
fusion-like heavy residues are studied using the INDRA multidetector.
The fusion cross section was measured and shows a maximum at = 18-20
. A decomposition into four exit-channels consisting of the number of
heavy fragments produced in central collisions has been made. Their relative
yields are measured as a function of the incident beam energy. The energy
spectra of light charged particles (LCP) in coincidence with the fragments of
each exit-channel have been analyzed. They reveal that a composite system is
formed, it is highly excited and first decays by emitting light particles and
then may breakup into 2- or many- fragments or survives as an evaporative
residue. A quantitative estimation of this primary emission is given and
compared to the secondary decay of the fragments. These analyses indicate that
most of the evaporative LCP precede not only fission but also breakup into
several fragments.Comment: Invited Talk given at the 11th International Conference on
Nucleus-Nucleus Collisions (NN2012), San Antonio, Texas, USA, May 27-June 1,
2012. To appear in the NN2012 Proceedings in Journal of Physics: Conference
Series (JPCS
Constraints on the equation of state of dark energy and the Hubble constant from stellar ages and the CMB
We place tight constraints on the redshift-averaged, effective value of the
equation of state of dark energy, w, using only the absolute ages of Galactic
stars and the observed position of the first peak in the angular power spectrum
of the CMB. We find w<-0.8 at the 68% confidence level. If we further consider
that w > -1, this finding suggests that within our uncertainties, dark energy
is indistinguishable from a classical vacuum energy term.
We detect a correlation between the ages of the oldest galaxies and their
redshift. This opens up the possibility of measuring w(z) by computing the
relative ages of the oldest galaxies in the universe as a function of redshift,
dz/dt. We show that this is a realistic possibility by computing dz/dt at z~0
from SDSS galaxies and obtain an independent estimate for the Hubble constant,
H_0 = 69 \pm 12 km s-1 Mpc-1. The small number of galaxies considered at z>0.2
does not yield, currently, a precise determination of w(z), but shows that the
age--redshift relation is consistent with a Standard LCDM universe with .Comment: Submitted to Ap
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