Miracle-dz/UniFAR-FTUs huggingface dataset:
The Immunological Role of Milk Fat Globule Membrane

Human milk is the ideal food for newborns until the age of six months. Human milk can be defined as a dynamic living tissue, containing immunological molecules, such as immunoglobulins, supra-molecular structures, such as the milk fat globule membrane (MFGM), and even entire cells, such as the milk microbiota. The milk composition changes throughout lactation to fulfill the infant’s requirements and reflect the healthy/disease status of the lactating mother. Many bioactive milk components are either soluble or bound to the MFGM. In this work, we focus on the peculiar role of the MFGM components, from their structural organization in fat globules to their route into the gastrointestinal tract. Immunometabolic differences between human and bovine MFGM components are reported and the advantages of supplementing infant formula with the MFGM are highlighted.
Two-Body and Three-Body Contacts for Three Bosons in the Unitary Regime: Analytic Expressions and Limiting Forms

The two- and three-body contacts are central to a set of univeral relations between microscopic few-body physics within an ultracold Bose gas and its thermodynamical properties. They may also be defined in trapped few-particle systems, which is the subject of this work. In this work, we focus on the unitary three-body problem in a trap, where interactions are as strong as allowed by quantum mechanics. We derive analytic results for the two- and three-body contacts in this regime and compare them with existing limiting expressions and previous numerical studies.
Evolution of the f-mode instability in neutron stars and gravitational wave detectability

We study the dynamical evolution of the gravitational-wave driven instability of the $f$ mode in rapidly rotating relativistic stars. With an approach based on linear perturbation theory we describe the evolution of the mode amplitude and follow the trajectory of a newborn neutron star through its instability window. The influence on the $f$-mode instability of the magnetic field and the presence of an unstable $r$ mode is also considered. Two different configurations are studied in more detail, an $N=1$ polytrope with a typical mass and radius and a more massive polytropic $N=0.62$ model with gravitational mass $M=1.98{M}_{\ensuremath{\bigodot}}$. We study several evolutions with different initial rotation rates and temperature and determine the gravitational waves radiated during the instability. In more massive models, an unstable $f$ mode with a saturation energy of about ${10}^{\ensuremath{-}6}{M}_{\ensuremath{\bigodot}}{c}^{2}$ may generate a gravitational wave signal which can be detected by the Advanced LIGO/Virgo detector from the Virgo cluster. The magnetic field affects the evolution and then the detectability of the gravitational radiation when its strength is higher than ${10}^{12}\text{ }\text{ }\mathrm{G}$, while the effects of an unstable $r$ mode become dominant when this mode reaches the maximum saturation value allowed by nonlinear mode couplings. However, the relative saturation amplitude of the $f$ and $r$ modes must be known more accurately in order to provide a definitive answer to this issue. From the thermal evolution we find also that the heat generated by shear viscosity during the saturation phase completely balances the neutrinos' cooling and prevents the star from entering the regime of mutual friction. The evolution time of the instability is therefore longer and the star loses significantly larger amounts of angular momentum via gravitational waves.
Short time-scale AGN X-ray variability with EXOSAT: black hole mass and normalized variability amplitude

The old EXOSAT medium energy measurements of high frequency (HF) AGN power spectral normalisation are re-examined in the light of accurate black hole mass determinations which were not available when these data were first published (Green et al 1993). It is found that the normalised variability amplitude (NVA), measured directly from the power spectrum, is proportional to M^{beta} where beta ~ -0.54 +/- 0.08. As NVA is the square root of the power, these observations show that the normalisation of the HF power spectrum for this sample of AGN varies very close to inversely with black hole mass. Almost the same value of $\beta$ is obtained whether the quasar 3C273 is included in the sample or not, suggesting that the same process that drives X-ray variability in Seyfert galaxies applies also to 3C273. These observations support the work of Gierlinski et al (2008) who show that an almost exactly linear anticorrelation is required if the normalisations of the HF power spectra of AGN and X-ray binary systems are to scale similarly. These observations are also consistent with a number of studies showing that the short timescale variance of AGN X-ray lightcurves varies approximately inversely with mass.
On the Goldberg–Sachs theorem in higher dimensions in the non-twisting case

We study a generalization of the ‘shearfree part’ of the Goldberg–Sachs theorem for Einstein spacetimes admitting a non-twisting multiple Weyl aligned null direction (WAND) ℓ in n ⩾ 6 spacetime dimensions. The form of the corresponding optical matrix ρ is restricted by the algebraically special property in terms of the degeneracy of its eigenvalues. In particular, there necessarily exists at least one multiple eigenvalue, and further constraints arise in various special cases. For example, when ρ is non-degenerate and certain (boost weight zero) Weyl components do not vanish, all eigenvalues of ρ coincide and such spacetimes thus correspond to the Robinson–Trautman class. On the other hand, in certain degenerate cases all non-zero eigenvalues can be distinct. We also present explicit examples of Einstein spacetimes admitting some of the permitted forms of ρ, including examples violating the ‘optical constraint’. The obtained restrictions on ρ are, however, in general not sufficient for ℓ to be a multiple WAND, as demonstrated by a few ‘counterexamples’. We also discuss the geometrical meaning of these restrictions in terms of integrability properties of certain totally null distributions. Finally, we specialize our analysis to the six-dimensional case, where all the permitted forms of ρ are given in terms of just two parameters. In the appendices, some examples are given and certain results pertaining to (possibly) twisting multiple WANDs of Einstein spacetimes are presented.
Linkage to HIV care and hypertension and diabetes control in rural South Africa: Results from the population-based Vukuzazi Study

Non-communicable diseases (NCDs) account for half of all deaths in South Africa, partly reflecting unmet NCDs healthcare needs. Leveraging existing HIV infrastructure is touted as a strategy to alleviate this chronic care gap. We evaluated whether HIV care platforms are associated with improved NCDs care. We conducted a community-based screening of adults in rural KwaZulu-Natal, collecting BP, HbA1c, and health services utilization data. Care cascade indicators for hypertension and diabetes mellitus were defined as: 1) aware, if previously diagnosed, 2) in care, if seeing a provider within last 6 months; 3) treated, if reporting medication use within preceding 2 weeks; and 4) controlled, if BP<140/90mmHg or HbA1c<6.5%. We fit multivariable adjusted logistic regression models to compare successful completion of each step of the care cascade for hypertension and diabetes between people with virally suppressed HIV and HIV-negative comparators. Inverse probability sampling weights were applied to derive population-level estimates. The analytic sample included 4,933 individuals [mean age 58.4 years; 77% female]. Compared to being HIV-negative, having suppressed HIV was associated with lower adjusted prevalence of being aware (-6.0% [95% CI: -11.0, -1.1%]), in care (-5.7% [-10.6, -0.8%]), and in treatment (-4.8% [-9.7, 0.1%]) for diabetes; but higher adjusted prevalence of controlled diabetes (3.2% [0.2–6.2%]). In contrast, having suppressed HIV was associated with higher adjusted prevalence of being aware (7.4% [5.3–9.6%]), in care (8.0% [5.9–10.2%]), in treatment (8.4% [6.1–10.6%]) and controlled (9.0% [6.2–11.8%]), for hypertension. Overall, disease control was achieved for 40.0% (38.6–40.8%) and 6.8% (5.9–7.8%) of individuals with hypertension and diabetes, respectively. Engagement in HIV care in rural KwaZulu-Natal was generally associated with worse diabetes care and improved hypertension care. While further work should explore how success of HIV programs can be translated to NCD care, strengthening of primary healthcare will also be needed to respond to the growing NCDs epidemic.
Fast Antenna Characterization With Numerical Expansion Functions Built With Partial Knowledge of the Antenna and Accelerated Asymptotic Methods

We describe a method to use numerical simulations concurrently with measurements (near-field data) to characterize the radiation properties of an antenna (far-field) with a strongly reduced number of samples. Both the simulations and experimental data are dealt with as sources of information toward obtaining the desired characterization. Simulations compensate for data scarceness, allowing to obtain an accurate characterization with fewer data than with measurements only, and the few measured data allow the comprehensive numerical proxy to get tuned to the true antenna under test (AUT). The method uses partial knowledge of the antenna and leverages accelerated asymptotic numerical methods to perform the numerical simulations needed by the algorithm. We report experimental tests of performance, both in terms of accuracy and speed-up with respect to the classical methods, with reflector antennas up to 27 wavelength. It is important to note that good results are obtained both when samples are taken on irregular optimized grids and on regular grids usually resulting from the conventional measurement rigs.
Analysis of Science Learning Module Development Needs PBL-Based (Problem Based Learning) to Improve HOTS

This study aims to examine the needs of students in MTs Negeri 2 Ngawi, especially Class VII, for PBL-based science learning modules to improve HOTS. This development research method is R&D (Research and Development), which is adapted from the development of a 4-D model (Define, Design, Develop and Disseminate). However, this research is limited to the Define stage, which is carried out by analyzing learning procedures. The subjects of this study were MTsN 2 Ngawi science teachers and class VII students who had studied temperature and heat material. Based on the questionnaire from students, it can be concluded that 90% of students believe in the need to develop teaching materials. While the questionnaire given to teachers found the result that learning in the classroom seemed to be monotonous so that it did not support the ability of students to think at a high level, it was necessary to have teaching materials or modules as support because the books provided by the government were inadequate. In conclusion from the results of the questionnaire of students and teachers, as well as the cognitive learning outcomes of students, it is necessary to develop modules related to Temperature and Heat. The development of problem-based learning modules (PBL) is a method for teachers to improve the learning process of students, especially in terms of fostering higher-order thinking skills (HOTS).
The remnant radio galaxy associated with NGC 1534

Abstract We present new observations of the large-scale radio emission surrounding the lenticular galaxy NGC 1534 with the Australia Telescope Compact Array and Murchison Widefield Array. We find no significant compact emission from the nucleus of NGC 1534 to suggest an active core, and instead find low-power radio emission tracing its star-formation history with a radio-derived star-formation rate of 0.38±0.03 M⊙ yr−1. The spectral energy distribution of the extended emission is well-fit by a continuous injection model with an ‘off’ component, consistent with dead radio galaxies. We find the spectral age of the emission to be 203 Myr, having been active for 44 Myr. Polarimetric analysis points to both a large-scale magneto-ionic Galactic foreground at +33 rad m−2 and a component associated with the northern lobe of the radio emission at -153 rad m−2. The magnetic field of the northern lobe shows an unusual circular pattern of unknown origin. While such remnant sources are rare, combined low- and high-frequency radio surveys with high surface-brightness sensitivities are expected to greatly increase their numbers in the coming decade, and combined with new optical and infrared surveys should provide a wealth of information on the hosts of the emission.
On nonlinear Alfvén-cyclotron waves in multi-species plasma

Abstract Large-amplitude Alfvén waves are ubiquitous in space plasmas and a main component of magnetohydrodynamic (MHD) turbulence in the heliosphere. As pump waves, they are prone to parametric instability by which they can generate cyclotron and acoustic daughter waves. Here, we revisit a related process within the framework of the multi-fluid equations for a plasma consisting of many species. The nonlinear coupling of the Alfvén wave to acoustic waves is studied, and a set of compressive and coupled-wave equations for the transverse magnetic field and longitudinal electric field is derived for waves propagating along the mean-field direction. It turns out that slightly compressive Alfvén waves exert, through induced gyro-radius and kinetic-energy modulations, an electromotive force on the particles in association with a longitudinal electric field, which has a potential that is given by the gradient of the transverse kinetic energy of the particles gyrating about the mean field. This in turn drives electric fluctuations (sound and ion-acoustic waves) along the mean magnetic field, which can nonlinearly react back on the transverse magnetic field. Mutually coupled Alfvén-cyclotron--acoustic waves are thus excited, a nonlinear process that can drive a cascade of wave energy in the plasma, and may generate compressive microturbulence. These driven electric fluctuations might have consequences for the dissipation of an MHD turbulence and, thus, for the heating and acceleration of particles in the solar wind.
A Survey on Efficient Methods for Adversarial Robustness

Deep learning has revolutionized computer vision with phenomenal success and widespread applications. Despite impressive results in complex problems, neural networks are susceptible to adversarial attacks: small and imperceptible changes in input space that lead these models to incorrect outputs. Adversarial attacks have raised serious concerns, and robustness to these attacks has become a vital issue. Adversarial training, a min-max optimization approach, has shown promise against these attacks. The computational cost of adversarial training, however, makes it prohibitively difficult to scale as well as to be useful in practice. Recently, several works have explored different approaches to make adversarial training computationally more affordable. This paper presents a comprehensive survey on efficient adversarial robustness methods with an aim to present a holistic outlook to make future exploration more systematic and exhaustive. We start by mathematically defining fundamental ideas in adversarially robust learning. We then divide these approaches into two categories based on underlying mechanisms: methods that modify initial adversarial training and techniques that leverage transfer learning to improve efficiency. Finally, based on this overview, we analyze and present an outlook of future directions.
THE DISCOVERY OF A NEW INSTABILITY IN A HYPERACCRETION FLOW AND ITS IMPLICATION FOR GAMMA-RAY BURSTS

A hyperaccretion flow around a stellar mass black hole is thought to be the most plausible engine that powers gamma-ray bursts (GRBs). The flow efficiently cools via neutrino emission at ≳ 0.003–0.01 M☉ s−1 (corresponding to a luminosity of ∼1050 erg s−1), while neither neutrino nor photon emission is efficient below this rate, so the flow should be advection-dominated. We carefully solve how a transition occurs from the advection-dominated to the neutrino-dominated branches, and find that the slope of the thermal equilibrium curve is negative in the surface density–accretion rate (Σ–) plane, a condition for viscous instability, at radii smaller than ∼12 Rg (with Rg being the gravitational radius). We also confirm that the flow is thermally stable. The consequence of this instability is the formation of a clumpy structure in the flow. This is because the larger (respectively smaller) surface density is, the smaller (respectively larger) the mass accretion rate from the region in question becomes, leading to growth of the density contrast. The timescale for clump formation is estimated to be shorter than 0.1 s. The observational implication is discussed in the context of GRBs. We suggest that this might explain the origin of the large variability observed in the prompt emission of GRBs.
ForwArd Search ExpeRiment at the LHC

New physics has traditionally been expected in the high-$p_T$ region at high-energy collider experiments. If new particles are light and weakly-coupled, however, this focus may be completely misguided: light particles are typically highly concentrated within a few mrad of the beam line, allowing sensitive searches with small detectors, and even extremely weakly-coupled particles may be produced in large numbers there. We propose a new experiment, ForwArd Search ExpeRiment, or FASER, which would be placed downstream of the ATLAS or CMS interaction point (IP) in the very forward region and operated concurrently there. Two representative on-axis locations are studied: a far location, $400~\text{m}$ from the IP and just off the beam tunnel, and a near location, just $150~\text{m}$ from the IP and right behind the TAN neutral particle absorber. For each location, we examine leading neutrino- and beam-induced backgrounds. As a concrete example of light, weakly-coupled particles, we consider dark photons produced through light meson decay and proton bremsstrahlung. We find that even a relatively small and inexpensive cylindrical detector, with a radius of $\sim 10~\text{cm}$ and length of $5-10~\text{m}$, depending on the location, can discover dark photons in a large and unprobed region of parameter space with dark photon mass $m_{A'} \sim 10 - 500~\text{MeV}$ and kinetic mixing parameter $\epsilon \sim 10^{-6} - 10^{-3}$. FASER will clearly also be sensitive to many other forms of new physics. We conclude with a discussion of topics for further study that will be essential for understanding FASER's feasibility, optimizing its design, and realizing its discovery potential.
Comment on "High-Pressure Behavior of Hydrogen and Deuterium at Low Temperatures".

X. -D. Liu et al. [Phys. Rev. Lett. 119, 065301 (2017)PRLTAO0031-900710.1103/PhysRevLett.119. 065301] report on the existence of a new unique solid phase of D_{2}, which makes the high-pressure low-temperature behavior distinct from H_{2}. Here, based on the analysis of their Raman data and phase transition theory, we show that the presented data do not support this claim.
Absence of linear polarization in H$\alpha$ emission of solar flares

High sensitivity observations of Ha polarization of 30 flares of different sizes and disk positions are reported. Both filter and spectrographic techniques have been used. The ZIMPOL system eliminates spurious polarizations due to seeing and flat-field effects. We didn't find any clear linear polarization signature above our sensitivity level which was usually better than 0.1%. The observations include an X17.1 flare with gamma-ray lines reported by the RHESSI satellite. These results cast serious doubts on previous claims of linear polarization at the one percent level and more, attributed to impact polarization. The absence of linear polarization limits the anisotropy of energetic protons in the Ha emitting region. The likely causes are isotropization by collisions with neutrals in the chromosphere and defocusing by the converging magnetic field.
DETERMINATION OF THE CRITICAL PERIOD OF WEED CONTROL (CPWC) TO INCREASE THE YIELD OF BARLEY (HORDEUM VULGARE L.) CROP IN EGYPT

The purpose of this study was to determine the effect of different weed competition periods on the growth and yield of an Egyptian barley crop under field conditions, as well as to estimate the critical period of weed control (CPWC) in barley. The treatments were arranged in a randomized complete block design with three replications (i.e., plots 4 × 4 m each) and consisted of a quantitative series of both increasing duration of weed interference and length of weed-free periods. The measured morphological parameters of barley plants were greater in non-weedy barley fields than in weedy barley fields. The shoot height of non-weedy barley plants was significantly ( P < 0.05 ) higher than that of weedy plants. After 75 DAE (Days After Emergence) of weed infestation, the maximum height and plant density were obtained. The biomass of barley plants and their associated weeds was gradually increased until 45 DAE, when barley biomass continued to increase, while weed biomass decreased. The maximum barley yield in the weed-free plots was 3.2 t ha -1 after 90 DAE, while it was 2.2 t ha -1 in the weed-infested plots after 75 DAE. Based on a 10% yield loss, the CPWC fell between 63 and 79 DAE, while a 5% yield loss fell between 41 and 102 DAE. Weed presence prior to and after the CPWC is not expected to reduce crop yield. As a result, weed removal at the CPWC is critical to allow plants to grow to their full potential without being hampered by competition and, hence, crop yield loss.
Supersolar Metallicity in the NLS1 Galaxy Markarian 1044

We present measurements of the metallicity of the circumnuclear gas in the narrow-line Seyfert 1 (NLS1) galaxy Markarian 1044 using O VI column density measurements from the Far Ultraviolet Spectroscopic Explorer (FUSE) together with C IV, N V, and H I measurements from the Hubble Space Telescope (HST). From the absorption lines we find that the circumnuclear gas in Mrk 1044 has a metallicity of at least 5 times solar, consistent with the expectation from previous emission-line studies that NLS1s have a high metallicity, similar to that found in high-redshift quasars. More surprisingly, we find that the absorbing material requires a near-solar mixture of elements in which the N/C ratio is consistent with the solar ratio and does not scale with the metallicity. This suggests that the chemical enrichment scenario for this active galactic nucleus (and thus possibly others) may be different from the traditional model of galactic metal enrichment, at least in the high-metallicity regime.
A parametric physical model for the intracluster medium and its use in joint SZ/X-ray analyses of galaxy clusters

We present a parametrized model of the intracluster medium that is suitable for jointly analysing pointed observations of the Sunyaev-Zel'dovich (SZ) effect and X-ray emission in galaxy clusters. The model is based on assumptions of hydrostatic equilibrium, the Navarro, Frenk and White model for the dark matter and a softened power-law profile for the gas entropy. We test this entropy-based model against high and low signal-to-noise ratio ratio mock observations of a relaxed and recently merged cluster from N-body/hydrodynamic simulations, using Bayesian hyperparameters to optimize the relative statistical weighting of the mock SZ and X-ray data. We find that it accurately reproduces both the global values of the cluster temperature, total mass and gas mass fraction (f gas ), and the radial dependencies of these quantities outside the core (r > 100 kpc). For reference, we also provide a comparison with results from the single isothermal β model. We confirm previous results that the single isothermal β model can result in significant biases in derived cluster properties.