Miracle-dz/UniFAR-FTUs huggingface dataset:
FOOT LOADING PATTERNS WITH DIFFERENT UNSTABLE SOLES STRUCTURE

Foot loading patterns can be changed by using different unstable sole structures, detailed quantification of which is of great significance for research and technological development in falling prevention and lower limb disorders rehabilitation. In this study, unstable soles constructions are adjusted through unstable elements in heel and medial, neutral and lateral forefoot and the foot loading patterns are comparatively studied. A total of 22 healthy male subjects participated in this test. Subjects are asked to walk over a 12 m walkway with control shoes and experimental shoes in self-adapted speed. Significant peak pressure, contact area and pressure-time integral differences in middle foot are found between control shoes and experimental shoes. In addition, peak pressure and pressure-time integral are found to increase significantly with unstable elements adding to center forefoot. The results showed that adjusting the unstable elements in coronal plane of forefoot could effectively alter the distribution of plantar pressure, this could potentially offer a mechanism for preventing falling of elderly and rehabilitation of lower extremity malfunctions. This study also demonstrates a novel concept that unstable element could be effectively adjusted in terms of position to meet different functional requirement.
The governance of vulnerable migrants: procedure, resources and affect in asylum reception

ABSTRACT This article explores how vulnerability is understood, appropriated and translated into procedural regulations and actual bureaucratic practices based on two case studies: 1) the reception of asylum seekers in Belgium; and 2) the reception of asylum seekers and provision of aid services in humanitarian operations in Uganda. These two cases demonstrate that ‘vulnerable groups’ and the corresponding procedural and substantial safeguards or protections are often defined flexibly, depending on the resources available to public institutions on the one hand, and specific agency guidelines and definitions of ‘vulnerable’ status on the other. Our ethnographic data show that reception bureaucrats are uncomfortably wedged between their desire to help and their obligation to follow state policies. To reconcile these (sometimes contradictory) obligations, they break administrative guidelines, use their own resources to make up for the shortcomings of their institution, or systematically decline migrants’ requests in the hope of demonstrating the absurdity of current reception policies.
Colors of AGN host galaxies at 0.5

We present the results from a study of the host galaxies of 15 optically selected AGNs with 0.5<z<1.1 from GEMS. GEMS is a Hubble Space Telescope imaging survey of a ~28"x28" contiguous field centered on the Chandra Deep Field South in the F606W and F850LP filter bands. It incorporates the SEDs and redshifts of ~10000 objects, obtained by the COMBO-17 project. We have detected the host galaxies of all 15 AGNs in the F850LP-band (and 13/15 in the F606W-band), recovering their fluxes, morphologies and structural parameters. We find that 80% of the host galaxies have early-type (bulge-dominated) morphologies, while the rest have structures characteristic of late-type (disk-dominated) galaxies. We find that 25% of the early types, and 30% of the late types, exhibit disturbances consistent with galaxy interactions. The hosts show a wide range of colors, from those of red-sequence galaxies to blue colors consistent with ongoing star formation. Roughly 70% of the morphologically early-type hosts have rest-frame blue colors, a much larger fraction than those typical of non-active morphologically early-type galaxies in this redshift and luminosity range. Yet, we find that the early-type hosts are structurally similar to red-sequence ellipticals, inasmuch as they follow an absolute magnitude versus half-light size correlation that are consistent with the mean relation for early-type galaxies at similar redshifts.
A Deficit of Dark Matter from Jeans Modeling of the Ultra-diffuse Galaxy NGC 1052-DF2

The discovery of the ultra-diffuse galaxy NGC 1052-DF2 and its peculiar population of star clusters has raised new questions about the connections between galaxies and dark matter (DM) halos at the extremes of galaxy formation. In light of debates over the measured velocity dispersion of its star clusters and the associated mass estimate, we constrain mass models of DF2 using its observed kinematics with a range of priors on the halo mass. Models in which the galaxy obeys a standard stellar-halo mass relation are in tension with the data and also require a large central density core. Better fits are obtained when the halo mass is left free, even after accounting for increased model complexity. The dynamical mass-to-light ratio for our model with a weak prior on the halo mass is , consistent with the stellar population estimate for DF2. We use tidal analysis to find that the low-mass models are consistent with the undisturbed isophotes of DF2. Finally, we compare with Local Group dwarf galaxies and demonstrate that DF2 is an outlier in both its spatial extent and its relative DM deficit.
Superradiant and stimulated-superradiant emission of bunched electron beams

Electron beams can generate radiation spanning a wide range of the electromagnetic spectrum. Creating temporal structure in the beam density results in intense radiation emission proportional to the square of the particle number as compared to the linear dependence on particle number from a randomly distributed electron beam. In this article various coherent radiation emission processes are discussed including spontaneous emission, coherent spontaneous superradiance, and stimulated superradiance.
The Circumgalactic Medium of eBOSS Emission Line Galaxies: Signatures of Galactic Outflows in Gas Distribution and Kinematics

We study the distribution and kinematics of the cool circumgalactic medium (CGM) of emission line galaxies (ELGs) traced by metal absorption lines. Using about 200,000 ELGs from SDSS-IV eBOSS and half a million background quasars from SDSS, we measure the median absorption strength of Mg ii and Fe ii lines in quasar spectra for impact parameters ranging from 10 kpc to 1 Mpc. For comparison, we measure the same quantity around luminous red galaxies (LRGs). On scales greater than 100 kpc both ELGs and LRGs exhibit similar absorption profiles. However, metal absorption is 5–10 times stronger around ELGs on smaller scales. The metal absorption strength is anisotropic, with an excess along the minor axis of the galaxies, indicating an outflow origin of the absorbing gas. The ratio between the velocity dispersion of the cool CGM and that of its host dark matter halo is about one for ELGs but about half for LRGs. These results show that the dichotomy of galaxy types is reflected in both the density distribution and kinematics of the CGM traced by metal absorption lines. Our results provide strong evidence that the CGM of ELGs is enriched by gas outflows generated by star formation.
Participation Rates in Physics 12 in BC: Science Teachers’ and Students’ Views

In recent years, participation rates in the British Columbia (BC) provincial physics exams have been low, compared with chemistry and biology. A qualitative study employing questionnaire and interview methods sought the views of teachers and students of senior science courses on why this is the case. Data analysis revealed that students’ decisions about Physics 12 were influenced by their perceptions of the mathematical content of physics, the physics teachers’ personalities and teaching styles, the perceived difficulty of physics, and prior experience of physics. We conclude that enhancing student interest in taking physics at advanced high school levels may necessitate a wider, more articulated exposure to topics in physics, together with more careful attention to mathematical background and skills. RésuméAu cours des dernières années, le taux de participation aux examens provinciaux de physique en Colombie Britannique a été nettement plus bas que celui des examens en chimie et en biologie. Au moyen d’une étude quantitative basée sur des méthodes utilisant des questionnaires et des entrevues, nous avons tenté de cerner l’opinion des enseignants et des étudiants des cours de dernière année en sciences à ce sujet. Une analyse des données révèle que les décisions des étudiants sur la physique de cinquième secondaire sont influencées par leur perception des contenus mathématiques des cours de physique, par la personnalité et le style d’enseignement des professeurs, par la difficulté qu’ils attribuent à cette matière et par leurs expériences passées qui y sont associées. En conclusion, nous estimons que si l’on souhaite favoriser l’intérêt des étudiants pour la physique de niveau avancé au secondaire, il sera peut-être nécessaire d’exposer ces derniers à une plus vaste gamme de sujets dans ce domaine, plus articulés et plus détaillés, et d’accorder une attention plus soignée aux connaissances et aux compétences de base en mathématiques.
G315.1+2.7 : a new galactic supernova remnant from the AAO/UKST Hα survey

New narrow-band Hα imaging and subsequent optical spectra confirm G315.1+2.7, a previously identified candidate supernova remnant (SNR), as a bona fide Galactic SNR. Present observations are based on independent discovery of filamentary optical emission nebulosity on images of the Anglo-Australian Observatory/United Kingdom Schmidt Telescope Hα survey of the southern Galactic plane which were found to coincide with existing multifrequency radio detections. Separate medium- and high-dispersion spectra were taken across two locations of this 11-arcmin north–south (NS) aligned optical filament. The resulting spectral signatures were found to strongly confirm the SNR identification based on standard emission-line ratio discriminators which characterize emission from shock-heated gas. The average observed ratios of S ii/Hα= 1.13, N ii/Hα= 1.43 and S ii 6717/6731 = 1.46, together with the simultaneous detection of [O ii] 3727, [O iii] 5007 and [O i] 6300 A, all point to a SNR origin of the observed optical emission. There is also an excellent positional coincidence between the new Hα filament and the north-east radio arc of G315.1+2.7 seen at several frequencies. Careful scrutiny of the low-resolution but high-sensitivity Southern Hα Sky Survey Atlas also revealed a low-level but distinct optical emission arc. This arc precisely correlates with the large, 2.5°, NS angular extent of the proposed new SNR also seen as a fractured structure in the extant radio data. G315.1+2.7 was detected previously at 2400 and 4800 MHz and at 408 and 1420 MHz. We also identified associated radio emission at 843 MHz from the now publicly available Sydney University Molonglo Sky Survey. On the basis of optical imaging and spectra and radio observations at five frequencies, we identify G315.1+2.7 as a new Galactic SNR. The large projected angular extent of the new remnant, together with the distance estimate of ∼1.7 kpc and diameter of ∼80 pc, make G315.1+2.7 one of the largest remnants known.
IN-SYNC. V. Stellar Kinematics and Dynamics in the Orion A Molecular Cloud

The kinematics and dynamics of young stellar populations enable us to test theories of star formation. With this aim, we continue our analysis of the SDSS-III/APOGEE IN-SYNC survey, a high-resolution near-infrared spectroscopic survey of young clusters. We focus on the Orion A star-forming region, for which IN-SYNC obtained spectra of ∼2700 stars. In Paper IV we used these data to study the young stellar population. Here we study the kinematic properties through radial velocities (vr). The young stellar population remains kinematically associated with the molecular gas, following a gradient along the filament. However, near the center of the region, the vr distribution is slightly blueshifted and asymmetric; we suggest that this population, which is older, is slightly in the foreground. We find evidence for kinematic subclustering, detecting statistically significant groupings of colocated stars with coherent motions. These are mostly in the lower-density regions of the cloud, while the ONC radial velocities are smoothly distributed, consistent with it being an older, more dynamically evolved cluster. The velocity dispersion varies along the filament. The ONC appears virialized, or just slightly supervirial, consistent with an old dynamical age. Here there is also some evidence for ongoing expansion, from a vr-extinction correlation. In the southern filament, is ∼2–3 times larger than virial in the L1641N region, where we infer a superposition along the line of sight of stellar subpopulations, detached from the gas. In contrast, decreases toward L1641S, where the population is again in agreement with a virial state.
Nanobubble induced formation of quantum emitters in monolayer semiconductors

The recent discovery of exciton quantum emitters in transition metal dichalcogenides (TMDCs) has triggered renewed interest of localized excitons in low-dimensional systems. Open questions remain about the microscopic origin previously attributed to dopants and/or defects as well as strain potentials. Here we show that the quantum emitters can be deliberately induced by nanobubble formation in WSe2 and BN/WSe2 heterostructures. Correlations of atomic-force microscope and hyperspectral photoluminescence images reveal that the origin of quantum emitters and trion disorder is extrinsic and related to 10 nm tall nanobubbles and 70 nm tall wrinkles, respectively. We further demonstrate that ‘hot stamping’ results in the absence of 0D quantum emitters and trion disorder. The demonstrated technique is useful for advances in nanolasers and deterministic formation of cavity-QED systems in monolayer materials.
Recent Findings on Platelet Activation, vWF Multimers and Other Thrombotic Biomarkers Associated with Critical COVID-19

Mortality rate in patients with COVID-19 increases in those admitted to the ICU. Activation of the coagulation system is associated with the worse disease outcomes. The aim of this study was to evaluate platelet activation and thrombotic biomarkers in hospitalized patients with COVID-19 during the second and third infection waves of the pandemic during 2021, following a previous report that included patients from the first wave. Sixty five patients were recruited and classified according to disease outcome; 10 healthy donors were included as a control group. Among prothrombotic biomarkers, t-PA concentrations (p < .0001), PAI-1 (0.0032) and D dimer (p = .0011) were higher in patients who developed critical COVID-19. We also found platelet activation via αIIbβIII expression (p < .0001) and higher presence of vWF-HMWM in severe COVID-19 (p < .0001). Several prothrombotic biomarkers are found to be increased since hospital admission in patients which lately present a worse disease outcome (ICU admission/death), among these, platelet activation, vWF increased plasma concentration and presence of HMWM seem to be of special interest. New studies regarding the predictive value of thrombotic biomarkers are needed as SARS-CoV-2 variants continue to emerge.
Effects of Planetesimal Accretion on the Thermal and Structural Evolution of Sub-Neptunes

A remarkable discovery of NASA’s Kepler mission is the wide diversity in the average densities of planets of similar mass. After gas disk dissipation, fully formed planets could interact with nearby planetesimals from a remnant planetesimal disk. These interactions would often lead to planetesimal accretion due to the relatively high ratio between the planet size and the hill radius for typical planets. We present calculations using the open-source stellar evolution toolkit mesa (Modules for Experiments in Stellar Astrophysics) modified to include the deposition of planetesimals into the H/He envelopes of sub-Neptunes (∼1–20 M⊕). We show that planetesimal accretion can alter the mass–radius isochrones for these planets. The same initial planet, as a result of the same total accreted planetesimal mass, can have up to ≈5% difference in mean densities approximately several gigayears after the last accretion due to the inherent stochasticity of the accretion process. During the phase of rapid accretion, these differences are more dramatic. The additional energy deposition from the accreted planetesimals increase the ratio between the planet’s radius to that of the core during rapid accretion, which in turn leads to enhanced loss of atmospheric mass. As a result, the same initial planet can end up with very different envelope mass fractions. These differences manifest as differences in mean densities long after accretion stops. These effects are particularly important for planets that are initially less massive than ∼10 M⊕ and with envelope mass fractions less than ∼10%, thought to be the most common type of planets discovered by Kepler.
The Fragmentation Criteria in Local Vertically Stratified Self-gravitating Disk Simulations

Massive circumstellar disks are prone to gravitational instabilities, which trigger the formation of spiral arms that can fragment into bound clumps under the right conditions. Two-dimensional simulations of self-gravitating disks are useful starting points for studying fragmentation because they allow high-resolution simulations of thin disks. However, convergence issues can arise in 2D from various sources. One of these sources is the 2D approximation of self-gravity, which exaggerates the effect of self-gravity on small scales when the potential is not smoothed to account for the assumed vertical extent of the disk. This effect is enhanced by increased resolution, resulting in fragmentation at longer cooling timescales β. If true, it suggests that the 3D simulations of disk fragmentation may not have the same convergence problem and could be used to examine the nature of fragmentation without smoothing self-gravity on scales similar to the disk scale height. To that end, we have carried out local 3D self-gravitating disk simulations with simple β cooling with fixed background irradiation to determine if 3D is necessary to properly describe disk fragmentation. Above a resolution of ∼40 grid cells per scale height, we find that our simulations converge with respect to the cooling timescale. This result converges in agreement with analytic expectations which place a fragmentation boundary at βcrit = 3.
Synthesis of Wideband Thinned Eisenstein Fractile Antenna Arrays With Adaptive Beamforming Capability and Reduced Side-Lobes

A modern design of fractal antenna arrays, called fractile array, which exhibits a fractal boundary contour within a tiled plane, is explored for enhanced array performance. In this paper, the Eisenstein fractile array is introduced to exploit the unique geometrical features of fractiles that allow multiband and wideband operation and avoid grating lobes in the radiation pattern even, in some cases, when the array elements’ spacing is greater than the half wavelength. To alleviate the large number of elements and the high Side-Lobe Level (SLL) occurred at large scales, the Genetic Algorithm (GA) optimization technique is considered for thinning the proposed antenna array by estimating the optimal set of “on” and “off” elements corresponding to the minimum SLL without degrading the directivity of the radiation pattern. Also, the proposed array configuration is designed with adaptive beamforming capability using the Least Mean Square (LMS) technique. The effectiveness of the proposed GA-LMS approach is investigated by performing several MATLAB simulations under various set of array configurations. Results reveal that the suggested thinned Eisenstein fractile antenna array using GA-LMS approach is superior in terms of multiband and wideband performance, array element reduction, SLL reduction, grating lobe elimination, and beamforming capability. This elucidates the robustness of the suggested thinned Eisenstein fractile array as a promising design for multiband, wideband, compact, inexpensive, and adaptive smart antennas in modern wireless systems.
The DECam minute cadence survey – II. 49 variables but no planetary transits of a white dwarf

We present minute cadence photometry of 31 732 point sources observed in one 3 $\rm deg^{2}$ DECam pointing centred at RA = 09:03:02 and Dec. = −04:35:00 over eight consecutive half-nights. We use these data to search for eclipse-like events consistent with a planetary transit of a white dwarf and other sources of stellar variability within the field. We do not find any significant evidence for minute-long transits around our targets, hence we rule out planetary transits around ∼370 white dwarfs that should be present in this field. Additionally, we identify 49 variables, including 40 new systems. These include 23 detached or contact stellar binaries, one eclipsing white dwarf + M dwarf binary, 16 δ Scuti, three RR Lyrae, and two ZZ Ceti pulsators. Results from the remaining two fields in our survey will allow us to place more stringent constraints on the frequency of planets orbiting white dwarfs in the habitable zone.
COMPUTATIONS OF SPHEROIDAL HARMONICS WITH COMPLEX ARGUMENTS : A REVIEW WITH AN ALGORITHM

mn , the prolate and oblate radial spheroidal functions of the second kind, and their first-order derivatives, as obtained by Flammer @Spheroidal Wave Functions~Stanford University Press, Stanford, CA, 1987! #, are found to be inaccurate, although these tabulated data have been considered as exact referenced results for about half a century. The algorithm developed here for evaluating the spheroidal harmonics with the MATHEMATICA program is also found to be simple, fast, and numerically efficient, and of a much better accuracy than the other results tabulated by Flammer and others, being able to produce results of 100 significant digits or more. @S1063-651X~98! 05511-1# PACS number~s! : 02.70. Rw
Implementing an Adaptive Thrust Distribution Algorithm on the Robust Control System for Serial Split-Hull Underwater Vehicles

This paper discusses designing and implementing an adaptive thrust distribution algorithm on the already robust control system for serial split-hull underwater vehicles to maximise operational efficiency. Split-hull underwater vehicles are gaining popularity in subsea operations due to their flexible hyper-redundant design and enhanced manoeuvrability. These features facilitate them to replace conventional solutions, including torpedo-shaped Autonomous Underwater Vehicles (AUVs) and Remotely Operated Vehicles (ROVs). The field of research is currently undergoing a considerable transition toward operations on subsea activities that are more economical and efficient. Thus, implementing a robust and energy-efficient control system is of utmost importance. The robust Super Twisting Algorithm (STA) based control system is used on the vehicle, and an adaptive thrust distribution algorithm is proposed and implemented to optimise the energy efficiency further. The work involves modelling the vehicle, fluid forces, torque effects, and thruster configuration matrix and implementing the adaptive weight distribution on the STA-based control system. With the help of simulations, the improvements in the control system are proved.