15,770 research outputs found
A Profile Likelihood Analysis of the Constrained MSSM with Genetic Algorithms
The Constrained Minimal Supersymmetric Standard Model (CMSSM) is one of the
simplest and most widely-studied supersymmetric extensions to the standard
model of particle physics. Nevertheless, current data do not sufficiently
constrain the model parameters in a way completely independent of priors,
statistical measures and scanning techniques. We present a new technique for
scanning supersymmetric parameter spaces, optimised for frequentist profile
likelihood analyses and based on Genetic Algorithms. We apply this technique to
the CMSSM, taking into account existing collider and cosmological data in our
global fit. We compare our method to the MultiNest algorithm, an efficient
Bayesian technique, paying particular attention to the best-fit points and
implications for particle masses at the LHC and dark matter searches. Our
global best-fit point lies in the focus point region. We find many
high-likelihood points in both the stau co-annihilation and focus point
regions, including a previously neglected section of the co-annihilation region
at large m_0. We show that there are many high-likelihood points in the CMSSM
parameter space commonly missed by existing scanning techniques, especially at
high masses. This has a significant influence on the derived confidence regions
for parameters and observables, and can dramatically change the entire
statistical inference of such scans.Comment: 47 pages, 8 figures; Fig. 8, Table 7 and more discussions added to
Sec. 3.4.2 in response to referee's comments; accepted for publication in
JHE
The Tilt of the Local Velocity Ellipsoid as Seen by Gaia
The Gaia Radial Velocity Spectrometer (RVS) provides a sample of 7,224,631
stars with full six-dimensional phase space information. Bayesian distances of
these stars are available from the catalogue of Sch\"onrich et al. (2019). We
exploit this to map out the behaviour of the velocity ellipsoid within 5 kpc of
the Sun. We find that the tilt of the disc-dominated RVS sample is accurately
described by the relation , where
() are cylindrical polar coordinates. This corresponds to velocity
ellipsoids close to spherical alignment (for which the normalising constant
would be unity) and pointing towards the Galactic centre. Flattening of the
tilt of the velocity ellipsoids is enhanced close to the plane and Galactic
centre, whilst at high elevations far from the Galactic center the population
is consistent with exact spherical alignment. Using the LAMOST catalogue
cross-matched with Gaia DR2, we construct thin disc and halo samples of
reasonable purity based on metallicity. We find that the tilt of thin disc
stars straddles , and of halo stars
straddles . We caution against the use
of reciprocal parallax for distances in studies of the tilt, as this can lead
to serious artefacts.Comment: MNRAS, revised version contains additional checks on the integrity of
the distance
Online Tool Condition Monitoring Based on Parsimonious Ensemble+
Accurate diagnosis of tool wear in metal turning process remains an open
challenge for both scientists and industrial practitioners because of
inhomogeneities in workpiece material, nonstationary machining settings to suit
production requirements, and nonlinear relations between measured variables and
tool wear. Common methodologies for tool condition monitoring still rely on
batch approaches which cannot cope with a fast sampling rate of metal cutting
process. Furthermore they require a retraining process to be completed from
scratch when dealing with a new set of machining parameters. This paper
presents an online tool condition monitoring approach based on Parsimonious
Ensemble+, pENsemble+. The unique feature of pENsemble+ lies in its highly
flexible principle where both ensemble structure and base-classifier structure
can automatically grow and shrink on the fly based on the characteristics of
data streams. Moreover, the online feature selection scenario is integrated to
actively sample relevant input attributes. The paper presents advancement of a
newly developed ensemble learning algorithm, pENsemble+, where online active
learning scenario is incorporated to reduce operator labelling effort. The
ensemble merging scenario is proposed which allows reduction of ensemble
complexity while retaining its diversity. Experimental studies utilising
real-world manufacturing data streams and comparisons with well known
algorithms were carried out. Furthermore, the efficacy of pENsemble was
examined using benchmark concept drift data streams. It has been found that
pENsemble+ incurs low structural complexity and results in a significant
reduction of operator labelling effort.Comment: this paper has been published by IEEE Transactions on Cybernetic
Reconstruction and Particle Identification for a DIRC System
We study the reconstruction and particle identification (PID) problem for
Ring Imaging devices providing a good knowledge of the direction of the
Cerenkov photons, as the DIRC system, on which we specialize. We advocate first
the use of the stereographic projection as a tool allowing a suitable
representation of the photon data, as it allows to represent the Cerenkov cone
always as a circle. We set up an algorithm able to perform reliably a fit of
circle arcs of small angular opening, by minimising a true Chi2 expression. The
system we develop for PID relies on this algorithm and on a procedure able to
remove background photons with a high efficiency. We thus show that, even when
the background is large, it is possible to perform an efficient PID by means of
a fit algorithm which finally provides all the circle parameters; these are
connected with the charged track direction and its Cerenkov angle. It is shown
that background effects can be dealt without spoiling significantly the
reconstruction probability distributions.Comment: 67 pages, 23 figure
Filling in CMB map missing data using constrained Gaussian realizations
For analyzing maps of the cosmic microwave background sky, it is necessary to
mask out the region around the galactic equator where the parasitic foreground
emission is strongest as well as the brightest compact sources. Since many of
the analyses of the data, particularly those searching for non-Gaussianity of a
primordial origin, are most straightforwardly carried out on full-sky maps, it
is of great interest to develop efficient algorithms for filling in the missing
information in a plausible way. We explore practical algorithms for filling in
based on constrained Gaussian realizations. Although carrying out such
realizations is in principle straightforward, for finely pixelized maps as will
be required for the Planck analysis a direct brute force method is not
numerically tractable. We present some concrete solutions to this problem, both
on a spatially flat sky with periodic boundary conditions and on the pixelized
sphere. One approach is to solve the linear system with an appropriately
preconditioned conjugate gradient method. While this approach was successfully
implemented on a rectangular domain with periodic boundary conditions and
worked even for very wide masked regions, we found that the method failed on
the pixelized sphere for reasons that we explain here. We present an approach
that works for full-sky pixelized maps on the sphere involving a kernel-based
multi-resolution Laplace solver followed by a series of conjugate gradient
corrections near the boundary of the mask.Comment: 22 pages, 14 figures, minor changes, a few missing references adde
Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Bayesian Estimation of CMB Polarization Maps
We describe a sampling method to estimate the polarized CMB signal from
observed maps of the sky. We use a Metropolis-within-Gibbs algorithm to
estimate the polarized CMB map, containing Q and U Stokes parameters at each
pixel, and its covariance matrix. These can be used as inputs for cosmological
analyses. The polarized sky signal is parameterized as the sum of three
components: CMB, synchrotron emission, and thermal dust emission. The polarized
Galactic components are modeled with spatially varying power law spectral
indices for the synchrotron, and a fixed power law for the dust, and their
component maps are estimated as by-products. We apply the method to simulated
low resolution maps with pixels of side 7.2 degrees, using diagonal and full
noise realizations drawn from the WMAP noise matrices. The CMB maps are
recovered with goodness of fit consistent with errors. Computing the likelihood
of the E-mode power in the maps as a function of optical depth to reionization,
tau, for fixed temperature anisotropy power, we recover tau=0.091+-0.019 for a
simulation with input tau=0.1, and mean tau=0.098 averaged over 10 simulations.
A `null' simulation with no polarized CMB signal has maximum likelihood
consistent with tau=0. The method is applied to the five-year WMAP data, using
the K, Ka, Q and V channels. We find tau=0.090+-0.019, compared to
tau=0.086+-0.016 from the template-cleaned maps used in the primary WMAP
analysis. The synchrotron spectral index, beta, averaged over high
signal-to-noise pixels with standard deviation sigma(beta)<0.25, but excluding
~6% of the sky masked in the Galactic plane, is -3.03+-0.04. This estimate does
not vary significantly with Galactic latitude, although includes an informative
prior.Comment: 11 pages, 9 figures, matches version accepted by Ap
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