Miracle-dz/UniFAR-FTUs huggingface dataset:
Stability of optimal-wave-front-sample coupling under sample translation and rotation

The method of wavefront shaping to control optical properties of opaque media is a promising technique for authentication applications. One of the main challenges of this technique is the sensitivity of the wavefront-sample coupling to translation and/or rotation. To better understand how translation and rotation affect the wavefront- sample coupling we perform experiments in which we first optimize reflection from an opaque surface--to obtain an optimal wavefront--and then translate or rotate the surface and measure the new reflected intensity pattern. By using the correlation between the optimized and translated or rotated patterns we determine how sensitive the wavefront-sample coupling is. These experiments are performed for different spatial-light-modulator (SLM) bin sizes, beam-spot sizes, and nanoparticle concentrations. We find that all three parameters affect the different positional changes, implying that an optimization scheme can be used to maximize the stability of the wavefront-sample coupling. We also develop a model to simulate sample translation or rotation and its effect on the coupling stability, with the simulation results being qualitatively consistent with experiment.
The ‘Kim Jong-un Effect’ and the mainstreaming of North Korea coverage in UK Media

This article uses qualitative and quantitative methods to analyse the entire corpus of news articles published about North Korea by six major UK national newspapers from 2000 to 2020. It offers insights on how North Korea evolved from a relatively obscure subject to a mainstay in the world news section, particularly for the tabloids. Coverage grew exponentially, led by not only stories about nuclear development and missile programmes, but also by soft news items like football, and tourism. Notably, the tone of coverage shifted after Kim Jong-un came to power in 2011, leading to an explosion of stories focussed on the young leader and his family. Structural topic modelling reveals 12 key topic areas among elite and tabloid media. While elite media coverage spanned a wider range of subjects, tabloid media largely focussed on three topics: missiles, the Kim family, and football. Each theme was highly compatible with the traditions of tabloid coverage, supplying eye-catching images (missiles and Kim’s eccentric appearance), a ‘royal family’ of sorts, and sports (North Koreans’ feats during World Cup). Furthermore, qualitative analysis demonstrates that while tabloidization and sensationalistic reporting on the Kim family largely drove the increase in coverage, such stories also added colour and depth previously lacking in reportage on the enemy regime, thereby making the portrayal of North Korea more multidimensional.
Potential Nevadensin from Ocimum basilicum as Antibacterial Agent against Streptococcus mutans: In Vitro and In Silico Studies.

BACKGROUND Streptococcus mutans is one of the bacteria which contributes to biofilm formation and causes dental caries. The inhibition of SrtA, gbpC, and Ag I/II is a promising target to be developed as an antibacterial. Ocimum bacilicum is known to have antibacterial activity. AIM AND OBJECTIVE The aim of this study is to evaluate the potential nevadensin as antibacterial against S. mutans. METHODS Antibacterial analysis was carried out by disc diffusion and micro-dilution methods and the in-silico study was performed with ligand-protein docking. RESULTS The result showed that the MIC and MBC values of nevadensin are 900 and 7200 µg/mL, respectively. The binding energy of nevadensin to SrtA, gbpC, and Ag I/II were -4.53, 8.37, -6.12 kcal/mol, respectively. CONCLUSION Nevadensin shows moderate activity as an antibacterial against S. mutans. Meanwhile, in silico studies showed it has the same binding strength as chlorhexidine in inhibiting SrtA, whereas to gbpC and Ag I/II, it has a weaker binding affinity. Therefore, nevadensin has the potential as natural antibacterial against S. mutans by inhibiting SrtA.
Simple parameterization for the ground-state energy of the infinite Hubbard chain incorporating Mott physics, spin-dependent phenomena and spatial inhomogeneity

Simple analytical parameterizations for the ground-state energy of the one-dimensional repulsive Hubbard model are developed. The charge dependence of energy is parameterized using exact results extracted from the Bethe-ansatz (BA). The resulting parameterization is shown to be in better agreement with highly precise data obtained from a fully numerical solution to the BA equations than previous expressions (Lima et al 2003 Phys. Rev. Lett. 90 146402). Unlike these earlier proposals, the present parameterization correctly predicts a positive Mott gap at half filling for any U > 0. The construction is extended to spin-dependent phenomena by parameterizing the magnetization dependence of the ground-state energy using further exact results and numerical benchmarking. Lastly, the parameterizations developed for the spatially uniform model are extended by means of a simple local-density-type approximation to spatially inhomogeneous models, e.g. in the presence of impurities, external fields or trapping potentials. The results are shown to be in excellent agreement with independent many-body calculations, at a fraction of the computational cost.
PSR J1840−1419: A VERY COOL NEUTRON STAR

We present upper limits on the X-ray emission for three neutron stars. For PSR J1840−1419, with a characteristic age of 16.5 Myr, we calculate a blackbody temperature upper limit (at 99% confidence) of kT∞bb < 24+17−10 eV, making this one of the coolest neutron stars known. PSRs J1814−1744 and J1847−0130 are both high magnetic field pulsars, with inferred surface dipole magnetic field strengths of 5.5 × 1013 and 9.4 × 1013 G, respectively. Our temperature upper limits for these stars are kT∞bb < 123+20−33 eV and kT∞bb < 115+16−33 eV, showing that these high magnetic field pulsars are not significantly hotter than those with lower magnetic fields. Finally, we put these limits into context by summarizing all temperature measurements and limits for rotation-driven neutron stars.
Intervalles d'instabilité pour une équation de Hill à potentiel méromorphe

Dans ce travail nous etudions les intervalles d'instabilite pour une equation de Hill en dimension 1, dont le potentiel est reel-analytique et s'etend en une fonction meromorphe a poles simples dans une bande du plan complexe. Nous obtenons le developpement asymptotique de la largeur du n-ieme intervalle d'instabilite pour n grand a une erreur exponentiellement petite pres. Notre resultat montre en particulier qu'il y a une infinite d'intervalles d'instabilite ouverts pour ce type de potentiel. Nous utilisons la methode wkb complexe exacte pour construire des solutions de l'equation dont nous connaissons le developpement asymptotique en dehors des poles, puis des techniques d'analyse microlocale semiclassique pour etudier les solutions de l'equation dans un voisinage des poles. C’est le recollement de ces deux types de solutions qui donne notre resultat
The equatorial current sheet and other interesting features of the pulsar magnetosphere

We want to understand what drives magnetospheric dissipation in the equatorial current sheet. Numerical simulations have limitations and, unless we have a clear a priori understanding of the physical processes involved, their results can be misleading. We argue that the canonical pulsar magnetosphere is strongly dissipative and that a large fraction (up to 30–40 % in an aligned rotator) of the spindown luminosity is redirected towards the equator where it is dissipated into particle acceleration and emission of radiation. We show that this is due to the failure of the equatorial electric current to cross the Y-point at the tip of the corotating zone.
Evolution of the Universe to the present inert phase

We assume that the current state of the Universe can be described by the inert doublet model, containing two scalar doublets, one of which is responsible for electroweak-symmetry breaking and masses of particles and the second one having no couplings to fermions and being responsible for dark matter. We consider possible evolutions of the Universe to this state during cooling down of the Universe after inflation. We found that in the past the Universe could pass through phase states having no dark matter candidate. In the evolution via such states, in addition to a possible electroweak-symmetry breaking phase transition (second order), the Universe sustained one first-order phase transition or two phase transitions of the second order.
Frequency response function identification using fused filament fabrication-3D-printed embedded ArUco markers

The assessment of modal components is a fundamental step in structural dynamics. While experimental investigations are generally performed through full-contact techniques, using accelerometers or modal hammers, this research proposes a non-contact Frequency Response Function identification measurement technique based on ArUco markers displacement detection. The proposed method is presented using a harmonically excited FFF 3D-printed flexible structure, equipped with multiple embedded-printed markers, whose displacement is measured with an industrial camera. Comparison with numerical simulation and an established experimental approach is finally provided for the results validation.
Effect of Interfacial Interaction on the Demolding Deformation of Injection Molded Microfluidic Chips

During the demolding process, the interfacial interaction between the polymer and the metal mold insert will lead to the deformation of the micro-structure, which will directly affect the molding quality and performance of injection molded microfluidic chips. In this study, the demolding quality of micro-channels and micro-mixing structures of polycarbonate (PC), polymethyl methacrylate (PMMA), cyclic olefin copolymer (COC), and polystyrene (PS) microfluidic chips for heavy metal detection were investigated by molding experiments. The experimental results showed that the structures of microfluidic chips could be completely replicated. However, tensile deformation and fracture defects were observed at the edges of the micro-structures after demolding. Compared to the Ni mold insert, the calculation of the relative deviation percentages showed that the width of the micro-channel became larger and the depth became smaller, while the dimensions of the micro-mixing structure changes in the opposite direction. Subsequently, a molecular dynamics (MD) simulation model of polymer/nickel (Ni) mold insert for injection molding was established. The changes of adhesion work, demolding resistance and potential energy during demolding were analyzed. The simulation results showed that the polymer structures had some deformations such as necking, molecular chain stretching and voids under the action of adhesion work and demolding resistance. The difference in the contact area with the mold insert directly brought different interfacial interactions. In addition, the potential energy change of the polymer system could be used to quantitatively characterize the demolding deformation of the structure. Overall, the MD method is able to effectively explain the internal mechanisms of interfacial interactions, leading to the demolding deformation of polymer structures from the molecular/atomic scale.
The Fermi Large Area Telescope On Orbit: Event Classification, Instrument Response Functions, and Calibration

The Fermi Large Area Telescope (Fermi -LAT, hereafter LAT), the primary instrument on the Fermi Gamma-ray Space Telescope (Fermi) mission, is an imaging, wide field-of-view, high-energy γ-ray telescope, covering the energy range from 20 MeV to more than 300 GeV. During the first years of the mission the LAT team has gained considerable insight into the in-flight performance of the instrument. Accordingly, we have updated the analysis used to reduce LAT data for public release as well as the Instrument Response Functions (IRFs), the description of the instrument performance provided for data analysis. In this paper we describe the effects that motivated these updates. Furthermore, we discuss how we originally derived IRFs from Monte Carlo simulations and later corrected those IRFs for discrepancies observed between flight and simulated data. We also give details of the validations performed using flight data and quantify the residual uncertainties in the IRFs. Finally, we describe techniques the LAT team has developed to propagate those uncertainties into estimates of the systematic errors on common measurements such as fluxes and spectra of astrophysical sources. Subject headings: instrumentation: detectors – instrumentation: miscellaneous – methods: data analysis – methods: observational – telescopes
COLD MOLECULAR GAS IN MASSIVE, STAR-FORMING DISK GALAXIES AT z = 1.5

We report the detection of the CO J = 1–0 emission line in three near-infrared selected star-forming galaxies at z ∼ 1.5 with the Very Large Array and the Green Bank Telescope. These observations directly trace the bulk of molecular gas in these galaxies. We find H2 gas masses of 8.3 ± 1.9 × 1010 M☉, 5.6 ± 1.4 × 1010 M☉, and 1.23 ± 0.34 × 1011 M☉ for BzK-4171, BzK-21000, and BzK-16000, respectively, assuming a conversion αCO = 3.6 M☉ (K km s−1 pc2)−1. We combined our observations with previous CO 2–1 detections of these galaxies to study the properties of their molecular gas. We find brightness temperature ratios between the CO 2–1 and CO 1–0 emission lines of 0.80+0.35−0.22, 1.22+0.61−0.36, and 0.41+0.23−0.13 for BzK-4171, BzK-21000, and BzK-16000, respectively. At the depth of our observations it is not possible to discern between thermodynamic equilibrium or sub-thermal excitation of the molecular gas at J = 2. However, the low temperature ratio found for BzK-16000 suggests sub-thermal excitation of CO already at J = 2. For BzK-21000, a large velocity gradient model of its CO emission confirms previous results of the low excitation of the molecular gas at J = 3. From a stacked map of the CO 1–0 images, we measure a CO 2–1 to CO 1–0 brightness temperature ratio of 0.92+0.28−0.19. This suggests that, on average, the gas in these galaxies is thermalized up to J = 2, has star formation efficiencies of ∼100 L☉ (K km s−1 pc2)−1, and gas consumption timescales of ∼0.4 Gyr, unlike submillimeter galaxies and quasi-stellar objects at high redshifts.
The dust content of galaxies from z = 0 to z = 9

We study the dust content of galaxies from $z=0$ to $z=9$ in semi-analytic models of galaxy formation that include new recipes to track the production and destruction of dust. We include condensation of dust in stellar ejecta, the growth of dust in the interstellar medium (ISM), the destruction of dust by supernovae and in the hot halo, and dusty winds and inflows. The rate of dust growth in the ISM depends on the metallicity and density of molecular clouds. Our fiducial model reproduces the relation between dust mass and stellar mass from $z=0$ to $z=7$, the number density of galaxies with dust masses less than $10^{8.3}\,\rm{M}_\odot$, and the cosmic density of dust at $z=0$. The model accounts for the double power-law trend between dust-to-gas (DTG) ratio and gas-phase metallicity of local galaxies and the relation between DTG ratio and stellar mass. The dominant mode of dust formation is dust growth in the ISM, except for galaxies with $M_*<10^7\,\rm{M}_\odot$, where condensation of dust in supernova ejecta dominates. The dust-to-metal ratio of galaxies depends on the gas-phase metallicity, unlike what is typically assumed in cosmological simulations. Model variants including higher condensation efficiencies, a fixed timescale for dust growth in the ISM, or no growth at all reproduce some of the observed constraints, but fail to simultaneously reproduce the shape of dust scaling relations and the dust mass of high-redshift galaxies.
Accuracy of Generalized Gradient Approximation functionals for density functional perturbation theory calculations

We assess the validity of various exchange-correlation functionals for computing the structural, vibrational, dielectric, and thermodynamical properties of materials in the framework of density-functional perturbation theory (DFPT). We consider five generalized-gradient approximation (GGA) functionals (PBE, PBEsol, WC, AM05, and HTBS) as well as the local density approximation (LDA) functional. We investigate a wide variety of materials including a semiconductor (silicon), a metal (copper), and various insulators (SiO2 α-quartz and stishovite, ZrSiO4 zircon, and MgO periclase). For the structural properties, we find that PBEsol and WC are the closest to the experiments and AM05 performs only slightly worse. All three functionals actually improve over LDA and PBE in contrast with HTBS, which is shown to fail dramatically for α-quartz. For the vibrational and thermodynamical properties, LDA performs surprisingly very well. In the majority of the test cases, it outperforms PBE significantly and also the WC, PBEsol and AM05 functionals though by a smaller margin (and to the detriment of structural parameters). On the other hand, HTBS performs also poorly for vibrational quantities. For the dielectric properties, none of the functionals can be put forward. They all (i) fail to reproduce the electronic dielectric constant due to the well-known band gap problem and (ii) tend to overestimate the oscillator strengths (and hence the static dielectric constant).
Nanotechnology and the application in the food industry

The application of nanotechnology in the food industry enables prioritization of consumers’ needs. Nanotechnology has the ability to provide new forms of control on food structure; therefore, this technology has higher industrial value. This paper briefly introduces the main concepts of nanotechnology and its correlation with size reduction performance. This paper also introduces the main nanobjects and their potential applications in food, and summarizes various studies and their applications in food industry.
Conformal Transformation Analysis of Capacitive Wireless Charging

This paper studies the capacitive coupling in a capacitive power transfer (CPT) system designed for charging applications. It proposes mathematical models using the conformal transformation for calculating air-gapped and underwater capacitance and verifies the proposed models using COMSOL multiphysics and measurements. The measured results show that we can achieve nano-farad capacitance ranges if we submerge the capacitor in seawater. The seawater’s capacitance slightly changes when we increase the gap distance or the operating frequency. As the under seawater CPT system can be an attractive option for loosely-coupled charging applications, we further examine the system by focusing on the cross-coupling effects. The results show that the cross-coupling between the plate degrades the system’s power transfer capability and efficiency. With negligible cross-coupling effects, the system gives 129 W output power at an efficiency of 81.2%.
The Evolution of Cooling Flows: Self-similar Cooling Waves

Similarity solutions are presented for the time-dependent evolution of cooling flows. A cooling flow expands when the cooling time computed from the initial gas distribution increases with radius. If certain simplifying conditions are met, the evolution of the resulting cooling wave becomes self-similar. The similarity solutions obtained here assumed subsonic flow, which is valid in the outer parts of observed cooling flows; they are matched to transonic accretion solutions valid in the central parts. The models are applied to the cooling flow onto M87, with unsatisfactory agreement at small radius. A local linear stability analysis shows that the similarity solution suffers isobaric thermal instability, suggesting that the neglect of star formation may be responsible for the poor agreement. The similarity solution suggests that the cooling flow around M87 was more vigorous in the past. 41 refs.
Joint constraints on galaxy bias and σ8 through the N-pdf of the galaxy number density

We present a full description of the N-probability density function of the galaxy number density fluctuations. This N-pdf is given in terms, on the one hand, of the cold dark matter correlations and, on the other hand, of the galaxy bias parameter. The method relies on the assumption commonly adopted that the dark matter density fluctuations follow a local non-linear transformation of the initial energy density perturbations. The N-pdf of the galaxy number density fluctuations allows for an optimal estimation of the bias parameter (e.g., via maximum-likelihood estimation, or Bayesian inference if there exists any a priori information on the bias parameter), and of those parameters defining the dark matter correlations, in particular its amplitude (σ8). It also provides the proper framework to perform model selection between two competitive hypotheses. The parameters estimation capabilities of the N-pdf are proved by SDSS-like simulations (both, ideal log-normal simulations and mocks obtained from Las Damas simulations), showing that our estimator is unbiased. We apply our formalism to the 7th release of the SDSS main sample (for a volume-limited subset with absolute magnitudes Mr ⩽ −20). We obtain b̂ = 1.193 ± 0.074 and σ̂8 = 0.862 ± 0.080, for galaxy number density fluctuations in cells of the size of 30h−1Mpc. Different model selection criteria show that galaxy biasing is clearly favoured.
THREE-DIMENSIONAL HYDRODYNAMIC SIMULATIONS OF MULTIPHASE GALACTIC DISKS WITH STAR FORMATION FEEDBACK. II. SYNTHETIC H i 21 cm LINE OBSERVATIONS

We use three-dimensional numerical hydrodynamic simulations of the turbulent, multiphase atomic interstellar medium (ISM) to construct and analyze synthetic H i 21 cm emission and absorption lines. Our analysis provides detailed tests of 21 cm observables as physical diagnostics of the atomic ISM. In particular, we construct (1) the “observed” spin temperature, , and its optical-depth weighted mean Ts, obs; (2) the absorption-corrected “observed” column density, ; and (3) the “observed” fraction of cold neutral medium (CNM), fc, obs ≡ Tc/Ts, obs for Tc the CNM temperature; we compare each observed parameter with true values obtained from line-of-sight (LOS) averages in the simulation. Within individual velocity channels, Ts, obs(vch) is within a factor 1.5 of the true value up to τ(vch) ∼ 10. As a consequence, NH, obs and Ts, obs are, respectively, within 5% and 12% of the true values for 90% and 99% of LOSs. The optically thin approximation significantly underestimates NH for τ > 1. Provided that Tc is constrained, an accurate observational estimate of the CNM mass fraction can be obtained down to 20%. We show that Ts, obs cannot be used to distinguish the relative proportions of warm and thermally unstable atomic gas, although the presence of thermally unstable gas can be discerned from 21 cm lines with 200 K ≲ Ts, obs(vch) ≲ 1000 K. Our mock observations successfully reproduce and explain the observed distribution of the brightness temperature, optical depth, and spin temperature in Roy et al. The threshold column density for CNM seen in observations is also reproduced by our mock observations. We explain this observed threshold behavior in terms of vertical equilibrium in the local Milky Way's ISM disk.
Directional emission of single photons from small atomic samples

We provide a formalism to describe deterministic emission of single photons with tailored spatial and temporal profiles from a regular array of multi-level atoms. We assume that a single collective excitation is initially shared by all the atoms in a metastable atomic state, and that this state is coupled by a classical laser field to an optically excited state which rapidly decays to the ground atomic state. Our model accounts for the different field polarization components via re-absorption and emission of light by the Zeeman manifold of optically excited states.