60,774 research outputs found
Local Self-Energy Approach For Electronic Structure Calculations
Using a novel self-consistent implementation of Hedin's GW perturbation
theory we calculate space and energy dependent self-energy for a number of
materials. We find it to be local in real space and rapidly convergent on
second-- to third-- nearest neighbors. Corrections beyond GW are evaluated and
shown to be completely localized within a single unit cell. This can be viewed
as a fully self consistent implementation of the dynamical mean field theory
for electronic structure calculations of real solids using a perturbative
impurity solver.Comment: 5 pages, 2 figure
AGB Stars in the Fornax Dwarf Spheroidal Galaxy
We report on a multi-epoch study of the Fornax dwarf spheroidal galaxy, made
with the Infrared Survey Facility, over an area of about 42'x42'. The
colour-magnitude diagram shows a broad well-populated giant branch with a tip
that slopes down-wards from red to blue, as might be expected given Fornax's
known range of age and metallicity. The extensive AGB includes seven Mira
variables and ten periodic semi-regular variables. Five of the seven Miras are
known to be carbon rich. Their pulsation periods range from 215 to 470 days,
indicating a range of initial masses. Three of the Fornax Miras are redder than
typical LMC Miras of similar period, probably indicating particularly heavy
mass-loss rates. Many, but not all, of the characteristics of the AGB are
reproduced by isochrones from Marigo et al. for a 2 Gyr population with a
metallicity of Z=0.0025.
An application of the Mira period-luminosity relation to these stars yields a
distance modulus for Fornax of 20.69+/-0.04 (internal), +/-0.08 (total) (on a
scale that puts the LMC at 18.39 mag) in good agreement with other
determinations. Various estimates of the distance to Fornax are reviewed.Comment: 15 pages, 13 figures, accepted for publication in MNRA
Fast Predictive Simple Geodesic Regression
Deformable image registration and regression are important tasks in medical
image analysis. However, they are computationally expensive, especially when
analyzing large-scale datasets that contain thousands of images. Hence, cluster
computing is typically used, making the approaches dependent on such
computational infrastructure. Even larger computational resources are required
as study sizes increase. This limits the use of deformable image registration
and regression for clinical applications and as component algorithms for other
image analysis approaches. We therefore propose using a fast predictive
approach to perform image registrations. In particular, we employ these fast
registration predictions to approximate a simplified geodesic regression model
to capture longitudinal brain changes. The resulting method is orders of
magnitude faster than the standard optimization-based regression model and
hence facilitates large-scale analysis on a single graphics processing unit
(GPU). We evaluate our results on 3D brain magnetic resonance images (MRI) from
the ADNI datasets.Comment: 19 pages, 10 figures, 13 table
Statistical Physics of Irregular Low-Density Parity-Check Codes
Low-density parity-check codes with irregular constructions have been
recently shown to outperform the most advanced error-correcting codes to date.
In this paper we apply methods of statistical physics to study the typical
properties of simple irregular codes.
We use the replica method to find a phase transition which coincides with
Shannon's coding bound when appropriate parameters are chosen.
The decoding by belief propagation is also studied using statistical physics
arguments; the theoretical solutions obtained are in good agreement with
simulations. We compare the performance of irregular with that of regular codes
and discuss the factors that contribute to the improvement in performance.Comment: 20 pages, 9 figures, revised version submitted to JP
The Zeta Herculis binary system revisited. Calibration and seismology
We have revisited the calibration of the visual binary system Zeta Herculis
with the goal to give the seismological properties of the G0 IV sub-giant Zeta
Her A. We have used the most recent physical and observational data. For the
age we have obtained 3387 Myr, for the masses respectively 1.45 and 0.98 solar
mass, for the initial helium mass fraction 0.243, for the initial mass ratio of
heavy elements to hydrogen 0.0269 and for the mixing-length parameters
respectively 0.92 and 0.90 using the Canuto & Mazitelli (1991, 1992) convection
theory. Our results do not exclude that Zeta Her A is itself a binary
sub-system; the mass of the hypothetical unseen companion would be smaller than
0.05 solar mass. The adiabatic oscillation spectrum of Zeta Her A is found to
be a complicated superposition of acoustic and gravity modes; some of them have
a dual character. This greatly complicates the classification of the non-radial
modes. The echelle diagram used by the observers to extract the frequencies
will work for ell=0, 2, 3. The large difference is found to be of the order of
42 mu Hz, in agreement with the Martic et al. (2001) seismic observations.Comment: 12 pages, A&A in pres
Solution of the Skyrme-Hartree-Fock-Bogolyubov equations in the Cartesian deformed harmonic-oscillator basis. (VII) HFODD (v2.49t): a new version of the program
We describe the new version (v2.49t) of the code HFODD which solves the
nuclear Skyrme Hartree-Fock (HF) or Skyrme Hartree-Fock-Bogolyubov (HFB)
problem by using the Cartesian deformed harmonic-oscillator basis. In the new
version, we have implemented the following physics features: (i) the isospin
mixing and projection, (ii) the finite temperature formalism for the HFB and
HF+BCS methods, (iii) the Lipkin translational energy correction method, (iv)
the calculation of the shell correction. A number of specific numerical methods
have also been implemented in order to deal with large-scale multi-constraint
calculations and hardware limitations: (i) the two-basis method for the HFB
method, (ii) the Augmented Lagrangian Method (ALM) for multi-constraint
calculations, (iii) the linear constraint method based on the approximation of
the RPA matrix for multi-constraint calculations, (iv) an interface with the
axial and parity-conserving Skyrme-HFB code HFBTHO, (v) the mixing of the HF or
HFB matrix elements instead of the HF fields. Special care has been paid to
using the code on massively parallel leadership class computers. For this
purpose, the following features are now available with this version: (i) the
Message Passing Interface (MPI) framework, (ii) scalable input data routines,
(iii) multi-threading via OpenMP pragmas, (iv) parallel diagonalization of the
HFB matrix in the simplex breaking case using the ScaLAPACK library. Finally,
several little significant errors of the previous published version were
corrected.Comment: Accepted for publication to Computer Physics Communications. Program
files re-submitted to Comp. Phys. Comm. Program Library after correction of
several minor bug
XMM-Newton observation of the relaxed cluster A478: gas and dark matter distribution from 0.01 R_200 to 0.5 R_200
We present an \xmm mosaic observation of the hot ( keV) and nearby
() relaxed cluster of galaxies A478. We derive precise gas density,
gas temperature, gas mass and total mass profiles up to 12\arcmin (about half
of the virial radius ). The gas density profile is highly peaked
towards the center and the surface brightness profile is well fitted by a sum
of three --models. The derived gas density profile is in excellent
agreement, both in shape and in normalization, with the published Chandra
density profile (measured within 5\arcmin of the center). Projection and PSF
effects on the temperature profile determination are thoroughly investigated.
The derived radial temperature structure is as expected for a cluster hosting a
cooling core, with a strong negative gradient at the cluster center. The
temperature rises from keV up to a plateau of keV beyond 2'
(i.e. , Mpc being the virial radius).
From the temperature profile and the density profile and under the hypothesis
of hydrostatic equilibrium, we derived the total mass profile of A478 down to
0.01 and up to 0.5 the virial radius. We tested different dark matter models
against the observed mass profile. The Navarro, Frenk & White
(\cite{navarro97}) model is significantly preferred to other models. It leads
to a total mass of M for a concentration
parameter of . The gas mass fraction slightly increases with
radius. The gas mass fraction at a density contrast of is
\fgas=0.13\pm0.02, consistent with previous results on similar hot and
massive clusters. We confirm the excess of absorption in the direction of
A478.[abridged]Comment: 15 pages, 11 figures, accepted for publication in A&A, corrected
typo
The XMM-Newton serendipitous ultraviolet source survey catalogue
The XMM-Newton Serendipitous Ultraviolet Source Survey (XMM-SUSS) is a
catalogue of ultraviolet (UV) sources detected serendipitously by the Optical
Monitor (XMM-OM) on-board the XMM-Newton observatory. The catalogue contains
ultraviolet-detected sources collected from 2,417 XMM-OM observations in 1-6
broad band UV and optical filters, made between 24 February 2000 and 29 March
2007. The primary contents of the catalogue are source positions, magnitudes
and fluxes in 1 to 6 passbands, and these are accompanied by profile
diagnostics and variability statistics. The XMM-SUSS is populated by 753,578 UV
source detections above a 3 sigma signal-to-noise threshold limit which relate
to 624,049 unique objects. Taking account of substantial overlaps between
observations, the net sky area covered is 29-54 square degrees, depending on UV
filter. The magnitude distributions peak at 20.2, 20.9 and 21.2 in UVW2, UVM2
and UVW1 respectively. More than 10 per cent of sources have been visited more
than once using the same filter during XMM-Newton operation, and > 20 per cent
of sources are observed more than once per filter during an individual visit.
Consequently, the scope for science based on temporal source variability on
timescales of hours to years is broad. By comparison with other astrophysical
catalogues we test the accuracy of the source measurements and define the
nature of the serendipitous UV XMM-OM source sample. The distributions of
source colours in the UV and optical filters are shown together with the
expected loci of stars and galaxies, and indicate that sources which are
detected in multiple UV bands are predominantly star-forming galaxies and stars
of type G or earlier.Comment: Accepted for publication in MNRA
- …