62 research outputs found
Computation of the Halo Mass Function Using Physical Collapse Parameters: Application to Non-Standard Cosmologies
In this article we compare the halo mass function predicted by the excursion
set theory with a drifting diffusive barrier against the results of N-body
simulations for several cosmological models. This includes the standard LCDM
case for a large range of halo masses, models with different types of
primordial non-Gaussianity, and the Ratra-Peebles quintessence model of Dark
Energy. We show that in all those cosmological scenarios, the abundance of dark
matter halos can be described by a drifting diffusive barrier, where the two
parameters describing the barrier have physical content. In the case of the
Gaussian LCDM, the statistics are precise enough to actually predict those
parameters at different redshifts from the initial conditions. Furthermore, we
found that the stochasticity in the barrier is nonnegligible making the simple
deterministic spherical collapse model a bad approximation even at very high
halo masses. We also show that using the standard excursion set approach with a
barrier inspired by peak patches leads to inconsistent predictions of the halo
mass function.Comment: 25 pages, 12 figure
Self-consistency of the Excursion Set Approach
The excursion set approach provides a framework for predicting how the
abundance of dark matter halos depends on the initial conditions. A key
ingredient of this formalism comes from the physics of halo formation: the
specification of a critical overdensity threshold (barrier) which protohalos
must exceed if they are to form bound virialized halos at a later time. Another
ingredient is statistical, as it requires the specification of the appropriate
statistical ensemble over which to average when making predictions. The
excursion set approach explicitly averages over all initial positions, thus
implicitly assuming that the appropriate ensemble is that associated with
randomly chosen positions in space, rather than special positions such as peaks
of the initial density field. Since halos are known to collapse around special
positions, it is not clear that the physical and statistical assumptions which
underlie the excursion set approach are self-consistent. We argue that they are
at least for low mass halos, and illustrate by comparing our excursion set
predictions with numerical data from the DEUS simulations.Comment: 5 pages, 2 figure
Oral health and nutritional characteristics of adults with morbid obesity: a multivariate analysis.
The relationship between oral health and nutritional aspects are complex, especially in individuals with chronic diseases and comorbidities, such as morbid obesity. Thus, the aim of the present study was to identify oral health and nutritional-related patterns in 113 individuals, aged 19–68 years (92 females), seeking treatment for morbid obesity. Sociodemographic variables and medical records were examined, in addition to the consumption of fruit, vegetables, candies, and processed foods. Measures of body mass index, neck, waist and hip, caries experience (DMFT index), Community Periodontal Index (CPI index), and salivary physicochemical aspects were gathered. Aspects of oral health-related quality of life and symptoms of dry mouth were evaluated by means of Oral Health Impact Profile (OHIP-14) and Xerostomia Inventory-XI questionnaires. K-means cluster analysis and, subsequently, comparisons between clusters (one-way ANOVA) were performed (α = 5%). Three clusters were generated: Cluster 1 (labeled “Young”; n = 77) was characterized by younger participants with higher BMI, who reported the use of distractors while eating, the smallest number of meals/day, and who consumed sweetened drinks and processed food the day before. Cluster 2 (labeled “Diabetic individuals”; n = 12) was characterized by older participants with the highest proportion of diabetic participants (100% were diabetic; 73% insulin users), lower BMI, higher DMFT index and OHIP-14 and xerostomia scores, and who reported having consumed fruit and vegetables the day before. Finally, Cluster 3 (labeled “Poor periodontal health”; n = 24) was characterized by participants with the worse periodontal condition (higher CPI), and lower salivary flow, pH, and buffer capacity. Cluster 1 and 2 were the groups that showed higher demand for nutritional and dietetic counseling, because of the poor eating behavior and higher serum glucose levels, respectively. On the other hand, Cluster 2 and 3 showed the higher demand for oral rehabilitation and dental treatment because of the loss of teeth and worse periodontal condition, respectively, besides the need for dietetic counseling. This sample of individuals with morbid obesity showed very unique oral-health and nutritional characteristics and special needs patterns that should be identified to adjust or change unhealthy habits, thus improving the assistance of this condition
Cosmological MHD simulations of cluster formation with anisotropic thermal conduction
(abridged) The ICM has been suggested to be buoyantly unstable in the
presence of magnetic field and anisotropic thermal conduction. We perform first
cosmological simulations of galaxy cluster formation that simultaneously
include magnetic fields, radiative cooling and anisotropic thermal conduction.
In isolated and idealized cluster models, the magnetothermal instability (MTI)
tends to reorient the magnetic fields radially. Using cosmological simulations
of the Santa Barbara cluster we detect radial bias in the velocity and magnetic
fields. Such radial bias is consistent with either the inhomogeneous radial gas
flows due to substructures or residual MTI-driven field rearangements that are
expected even in the presence of turbulence. Although disentangling the two
scenarios is challenging, we do not detect excess bias in the runs that include
anisotropic thermal conduction. The anisotropy effect is potentially detectable
via radio polarization measurements with LOFAR and SKA and future X-ray
spectroscopic studies with the IXO. We demonstrate that radiative cooling
boosts the amplification of the magnetic field by about two orders of magnitude
beyond what is expected in the non-radiative cases. At z=0 the field is
amplified by a factor of about 10^6 compared to the uniform magnetic field
evolved due to the universal expansion alone. Interestingly, the runs that
include both radiative cooling and anisotropic thermal conduction exhibit
stronger magnetic field amplification than purely radiative runs at the
off-center locations. In these runs, shallow temperature gradients away from
the cluster center make the ICM neutrally buoyant. The ICM is more easily mixed
in these regions and the winding up of the frozen-in magnetic field is more
efficient resulting in stronger magnetic field amplification.Comment: submitted to ApJ, higher resolution figures available at:
http://www.astro.lsa.umich.edu/~mateuszr
Antiferromagnet-ferromagnet phase transition in lightly doped manganites
Magnetic and structural phase diagrams of the La₀.₈₈MnOx, La₁₋xSrx(Mn₁₋x/₂Nbx/₂)O₃,
Nd₁₋xCaxMnO₃, and Bi₁₋xCaxMnO₃ series constructed on the basis of x-ray, neutron powder diffraction,
Young’s modulus, magnetization and resistivity measurements are presented. It is shown
that the main factor controlling the antiferromagnet–ferromagnet phase transition in the manganites
is a type of an orbital state. The results are discussed in the framework of structurally driven
magnetic phase separation model
Haloes gone MAD: The Halo-Finder Comparison Project
[abridged] We present a detailed comparison of fundamental dark matter halo
properties retrieved by a substantial number of different halo finders. These
codes span a wide range of techniques including friends-of-friends (FOF),
spherical-overdensity (SO) and phase-space based algorithms. We further
introduce a robust (and publicly available) suite of test scenarios that allows
halo finder developers to compare the performance of their codes against those
presented here. This set includes mock haloes containing various levels and
distributions of substructure at a range of resolutions as well as a
cosmological simulation of the large-scale structure of the universe. All the
halo finding codes tested could successfully recover the spatial location of
our mock haloes. They further returned lists of particles (potentially)
belonging to the object that led to coinciding values for the maximum of the
circular velocity profile and the radius where it is reached. All the finders
based in configuration space struggled to recover substructure that was located
close to the centre of the host halo and the radial dependence of the mass
recovered varies from finder to finder. Those finders based in phase space
could resolve central substructure although they found difficulties in
accurately recovering its properties. Via a resolution study we found that most
of the finders could not reliably recover substructure containing fewer than
30-40 particles. However, also here the phase space finders excelled by
resolving substructure down to 10-20 particles. By comparing the halo finders
using a high resolution cosmological volume we found that they agree remarkably
well on fundamental properties of astrophysical significance (e.g. mass,
position, velocity, and peak of the rotation curve).Comment: 27 interesting pages, 20 beautiful figures, and 4 informative tables
accepted for publication in MNRAS. The high-resolution version of the paper
as well as all the test cases and analysis can be found at the web site
http://popia.ft.uam.es/HaloesGoingMA
Haloes gone MAD: The Halo-Finder Comparison Project
We present a detailed comparison of fundamental dark matter halo properties retrieved by a substantial number of different halo finders. These codes span a wide range of techniques including friends-of-friends, spherical-overdensity and phase-space-based algorithms. We further introduce a robust (and publicly available) suite of test scenarios that allow halo finder developers to compare the performance of their codes against those presented here. This set includes mock haloes containing various levels and distributions of substructure at a range of resolutions as well as a cosmological simulation of the large-scale structure of the universe. All the halo-finding codes tested could successfully recover the spatial location of our mock haloes. They further returned lists of particles (potentially) belonging to the object that led to coinciding values for the maximum of the circular velocity profile and the radius where it is reached. All the finders based in configuration space struggled to recover substructure that was located close to the centre of the host halo, and the radial dependence of the mass recovered varies from finder to finder. Those finders based in phase space could resolve central substructure although they found difficulties in accurately recovering its properties. Through a resolution study we found that most of the finders could not reliably recover substructure containing fewer than 30-40 particles. However, also here the phase-space finders excelled by resolving substructure down to 10-20 particles. By comparing the halo finders using a high-resolution cosmological volume, we found that they agree remarkably well on fundamental properties of astrophysical significance (e.g. mass, position, velocity and peak of the rotation curve). We further suggest to utilize the peak of the rotation curve, vmax, as a proxy for mass, given the arbitrariness in defining a proper halo edg
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