Miracle-dz/UniFAR-FTUs huggingface dataset:
Market food diversity mitigates the effect of environment on women’s dietary diversity in the Agriculture to Nutrition (ATONU) study, Ethiopia

Abstract Objective In Ethiopia, women’s dietary diversity is low, primarily due to poor food availability and access, both at home and market level. The present study aimed to describe market access using a new definition called market food diversity (MFD) and estimate the impact of MFD, crop and livestock diversity on dietary diversity among women enrolled in the Agriculture to Nutrition (ATONU) trial. Design Baseline cross-sectional data collected from November 2016 to January 2017 were used for the analysis. Availability of foods in markets was assessed at the village level and categorized into nine food groups similar to the dietary diversity index for women. Bivariate and multivariate mixed-effects regression analyses were conducted, adjusted for clustering at the village level. Setting Chicken-producing farmers in rural Ethiopia. Participants Women (n 2117) aged 15–49 years. Results Overall, less than 6 % of women met the minimum dietary diversity (≥5 food groups) and the most commonly consumed food groups were staples and legumes. Median MFD was 4 food groups (interquartile range: 2–8). Multivariate models indicated that women’s dietary diversity differed by livestock diversity, food crop diversity and agroecology, with significant interaction effects between agroecology and MFD. Conclusions Women’s dietary diversity is poor in Ethiopia. Local markets are variable in food availability across seasons and agroecological zones. The MFD indicator captures this variability, and women who have access to higher MFD in the highland agroecological zone have better dietary diversity. Thus, MFD has the potential to mitigate the effects of environment on women’s dietary diversity.
Nebular Continuum and Line Emission in Stellar Population Synthesis Models

Accounting for nebular emission when modeling galaxy spectral energy distributions (SEDs) is important, as both line and continuum emissions can contribute significantly to the total observed flux. In this work, we present a new nebular emission model integrated within the Flexible Stellar Population Synthesis code that computes the line and continuum emission for complex stellar populations using the photoionization code Cloudy. The self-consistent coupling of the nebular emission to the matched ionizing spectrum produces emission line intensities that correctly scale with the stellar population as a function of age and metallicity. This more complete model of galaxy SEDs will improve estimates of global gas properties derived with diagnostic diagrams, star formation rates based on Hα, and physical properties derived from broadband photometry. Our models agree well with results from other photoionization models and are able to reproduce observed emission from H ii regions and star-forming galaxies. Our models show improved agreement with the observed H ii regions in the Ne iii/O ii plane and show satisfactory agreement with He ii emission from z = 2 galaxies, when including rotating stellar models. Models including post-asymptotic giant branch stars are able to reproduce line ratios consistent with low-ionization emission regions. The models are integrated into current versions of FSPS and include self-consistent nebular emission predictions for MIST and Padova+Geneva evolutionary tracks.
Renormalization group approach to scalar quantum electrodynamics on de Sitter

We consider the quantum loop effects in scalar electrodynamics on de Sitter space by making use of the functional renormalization group approach. We first integrate out the photon field, which can be done exactly to leading (zeroth) order in the gradients of the scalar field, thereby making this method suitable for investigating the dynamics of the infrared sector of the theory. Assuming that the scalar remains light we then apply the functional renormalization group methods to the resulting effective scalar theory and focus on investigating the effective potential, which is the leading order contribution in the gradient expansion of the effective action. We find symmetry restoration at a critical renormalization scale $\kappa=\kappa_{\rm cr}$ much below the Hubble scale $H$. When compared with the results of Serreau and Guilleux [arXiv:1306.3846 [hep-th], arXiv:1506.06183 [hep-th]] we find that the photon facilitates symmetry restoration such that it occurs at an RG scale $\kappa_{\rm cr}$ that is higher than in the case of a pure scalar theory. The true effective potential is recovered when $\kappa\rightarrow 0$ and in that limit one obtains the results that agree with those of stochastic inflation, provided one interprets it in the sense as advocated by Lazzari and Prokopec [arXiv:1304.0404 [hep-th]].
Periodontitis as the risk factor of chronic kidney disease: Mediation analysis

Abstract Aim To determine sequences and magnitude of causality among periodontitis, diabetes and chronic kidney disease (CKD) by mediation analysis. Methods Ten‐year‐data were retrieved from the Electric Generation Authority of Thailand (EGAT) study. A cohort of 2,635 subjects was identified with no CKD at baseline. The interested outcome was CKD incidence defined as glomerular filtration rate <60 ml/min/1.73 m2. The percentage of proximal sites with clinical attachment loss ≥5 mm was used to represent periodontitis. Mediation analysis with 1,000‐replication bootstrapping was applied to two causal diagrams, diagram A (Periodontitis → Diabetes → CKD) and diagram B (Diabetes → Periodontitis → CKD). Results The cumulative incidence of CKD was 10.3 cases per 100 persons during 10‐year period. In diagram A, each increasing percentage of proximal sites with severe periodontitis increased the adjusted odds ratio of CKD 1.010 (95% CI: 1.005, 1.015) and 1.007 (95% CI: 1.004, 1.013), by direct and indirect effect through diabetes, respectively. In diagram B, diabetes increased the odds of CKD twofold, with 6.5% of this effect mediated via periodontitis. Conclusions Periodontitis had significant direct effect, and indirect effect through diabetes, on the incidence of CKD. Awareness about systemic morbidities from periodontitis should be emphasized.
New effective interactions in relativistic mean field theory with nonlinear terms and density-dependent meson-nucleon coupling

New parameter sets for the Lagrangian density in the relativistic mean field (RMF) theory, PK1 with nonlinear sigma- and omega-meson self-coupling, PK1R with nonlinear sigma-, omega-, and rho-meson self-coupling, and PKDD with the density-dependent meson-nucleon coupling are proposed. They are able to provide an excellent description not only for the properties of nuclear matter but also for the nuclei in and far from the valley of beta stability. For the first time in the parametrization of the RMF Lagrangian density, the center-of-mass correction is treated by a microscopic way, which is essential to unify the description of nuclei from light to heavy regions with one effective interaction.
Generalized Factorization in Hardy Spaces and the Commutant of Toeplitz Operators

Abstract Every classical inner function $\varphi$ in the unit disk gives rise to a certain factorization of functions in Hardy spaces. This factorization, which we call the generalized Riesz factorization, coincides with the classical Riesz factorization when $\varphi (z)\,=\,z$ . In this paper we prove several results about the generalized Riesz factorization, and we apply this factorization theory to obtain a new description of the commutant of analytic Toeplitz operators with inner symbols on a Hardy space. We also discuss several related issues in the context of the Bergman space.
Application of Levenberg-Marquardt Based Back Propagation Neurointelligence Algorithm in Studying the Cutting Parameters Effect on Thrust Force & Hole Diameteral Accuracy in Drilling of Aluminum Alloys

In this paper, the effect of the cutting speed, feed rate and the point angle, mechanical properties of aluminium alloys on diametric error and thrust force were investigated and estimated by assistance of a neural network using Levenberg-Marquardt Based Back Propagation Algorithm. Three types of commercial aluminium alloys were selected as the work piece materials for experiments. The neural network analysis were employed to analyze the effect of drilling parameters and predict the response of diametral error and the thrust force toward the drilling parameters changes. The results of network sensitivity and relative importance analysis indicated that feed rate and cutting speed minimize significantly both the diametral error and the thrust force.
Classical/quantum integrability in AdS/CFT

We discuss the AdS/CFT duality from the perspective of integrable systems and establish a direct relationship between the dimension of single trace local operators composed of two types of scalar ﬁelds in N = 4 super Yang-Mills and the energy of their dual semiclassical string states in AdS 5 × S 5 . The anomalous dimensions can be computed using a set of Bethe equations, which for “long” operators reduces to a Riemann-Hilbert problem. We develop a uniﬁed approach to the long wavelength Bethe equations, the classical ferromagnet and the classical string solutions in the SU (2) sector and present a general solution, governed by complex curves endowed with meromorphic diﬀerentials with integer periods. Using this solution we compute the anomalous dimensions of these long operators up to two loops and demonstrate that they agree with string-theory predictions.
Star-forming galaxies in intermediate-redshift clusters: stellar versus dynamical masses of luminous compact blue galaxies

We investigate the stellar masses of the class of star-forming objects known as Luminous Compact Blue Galaxies (LCBGs) by studying a sample of galaxies in the distant cluster MS$~$0451.6-0305 at $z\approx0.54$ with ground-based multicolor imaging and spectroscopy. For a sample of 16 spectroscopically-confirmed cluster LCBGs (colour $B-V < 0.5$, surface brightness $\mu_B < 21$ mag arcsec$^{-2}$, and magnitude $M_B < -18.5$), we measure stellar masses by fitting spectral energy distribution (SED) models to multiband photometry, and compare with dynamical masses (determined from velocity dispersion between 10 $<$ $\sigma_v (\rm km~ s^{-1})$ $<$ 80), we previously obtained from their emission-line spectra. We compare two different stellar population models that measure stellar mass in star-bursting galaxies, indicating correlations between the stellar age, extinction, and stellar mass derived from the two different SED models. The stellar masses of cluster LCBGs are distributed similarly to those of field LCBGs, but the cluster LCBGs show lower dynamical-to-stellar mass ratios ($\rm M_{dyn}/M_{\ast} = 2.6$) than their field LCBG counterparts ($\rm M_{dyn}/M_{\ast}=4.8$), echoing trends noted previously in low-redshift dwarf elliptical galaxies. Within this limited sample, the specific star formation rate declines steeply with increasing mass, suggesting that these cluster LCBGs have undergone vigorous star formation.
K2 Study of the Magnetic Precataclysmic Variable V1082 Sagittarius

We present a long-term light curve of the precataclysmic variable (CV) V1082 Sgr obtained by the K2 mission over the course of 81 days. We analyze the entire complex light curve as well as explore several sections in detail with a sliding periodogram. The long data set allows the first detection of the orbital period in the light curve, as well as the confirmation of cyclical variability on a longer timescale of about a month. A portion of the light curve in deep minimum reveals a clean, near-sinusoidal variability attributed to the rotation of the spotted surface of the donor star. We model that portion of the light curve assuming that the donor star grossly under-fills its Roche lobe, has cool spots similar to a chromospherically active, slightly evolved early K-star, and might be irradiated by the X-ray beam from the magnetically accreting white dwarf. The fast variability of the object in the active phases resembles the light curves of magnetic CVs (polars).
On improving the effectiveness of periodic solutions of the NLS and DNLS equations

A method for improving the effectiveness of one-phase periodic solutions of integrable equations is suggested, which is based on the explicit determination of the locus of the auxiliary spectrum point. The method is applied to the nonlinear Schrodinger equation and the derivative nonlinear Schrodinger equation. It is shown that the relations between polynomial P( lambda ), defining the solution in the inverse transform method, and its algebraic resolvents play an important role in the theory.
The hypersingular boundary element method revisited

This is the sequel of a paper presented at the BEM/MRM Conference four years ago, in which the conventional, collocation boundary element method was reformulated by proposing a simple, however consistent derivation on the basis of the weighted-residuals statement. It was shown that the single-layer potential matrix G should be in general rectangular and satisfy some spectral properties (orthogonality to the space of unbalanced boundary traction forces) in the same way as the double-layer potential matrix H is orthogonal to rigid-body displacements, when modelling a finite elastic body. Moreover, a “subtle” improvement was proposed for the interpolation of traction forces, in the case of curved boundaries, which was meant to just simplify the numerical implementation. In the present paper, it is concluded that the proposed improvement is in fact a necessary one if strict consistency of the formulation is required and more emphatically if a consistent hypersingular formulation is to be implemented. It is also shown that the correct hypersingular formulation requires that the discontinuous parts (two free terms) of the matrix H be obtained independently from the matrix G. Motivation of the present developments was the application of the hybrid boundary element method to strain gradient elasticity, which only makes use of the matrix H together with its hypersingular counterpart. Although this paper is of a rather theoretical nature, a simple numerical example is shown to illustrate the necessity of the proposed improvements.
The role of volume and surface spontaneous parametric down-conversion in the generation of photon pairs in layered media

A rigorous description of volume and surface spontaneous parametric down-conversion in 1D nonlinear layered structures is developed considering exact continuity relations for the fields' amplitudes at the boundaries. The nonlinear process is described by the quantum momentum operator that provides the Heisenberg equations which solution is continuous at the boundaries. The transfer-matrix formalism is applied. The volume and surface contributions are clearly identified. Numerical analysis of a structure composed of 20 alternating GaN/AlN layers is given as an example.
Recovering galaxy cluster gas density profiles with XMM-Newton and Chandra

We examine the reconstruction of galaxy cluster radial density profiles obtained from Chandra and XMM X-ray observations, using high quality data for a sample of twelve objects covering a range of morphologies and redshifts. By comparing the results obtained from the two observatories and by varying key aspects of the analysis procedure, we examine the impact of instrumental effects and of differences in the methodology used in the recovery of the density profiles. We find that the final density profile shape is particularly robust. We adapt the photon weighting vignetting correction method developed for XMM for use with Chandra data, and confirm that the resulting Chandra profiles are consistent with those corrected a posteriori for vignetting effects. Profiles obtained from direct deprojection and those derived using parametric models are consistent at the 1% level. At radii larger than $\sim$6", the agreement between Chandra and XMM is better than 1%, confirming an excellent understanding of the XMM PSF. We find no significant energy dependence. The impact of the well-known offset between Chandra and XMM gas temperature determinations on the density profiles is found to be negligible. However, we find an overall normalisation offset in density profiles of the order of $\sim$2.5%, which is linked to absolute flux cross-calibration issues. As a final result, the weighted ratios of Chandra to XMM gas masses computed at R2500 and R500 are r=1.03$\pm$0.01 and r=1.03$\pm$0.03, respectively. Our study confirms that the radial density profiles are robustly recovered, and that any differences between Chandra and XMM can be constrained to the $\sim$ 2.5% level, regardless of the exact data analysis details. These encouraging results open the way for the true combination of X-ray observations of galaxy clusters, fully leveraging the high resolution of Chandra and the high throughput of XMM.
Elasto-plastic models of the yielding transition with stress-dependent transition rates

Elasto-plastic models are among the most successful ways to study the critical properties of the plastic yielding transition of amorphous solids. Typically these models are studied under a condition of constant transition rates from one plastic configuration to another, and in this form they predict the existence of well defined critical exponents that display universality, in the same sense that in standard equilibrium phase transitions. I show however that very naturally the transition rates must not be taken as a constant, but dependent of the local stress excess above the critical value. This modification in the model is seen to affect the values of some of the exponents of the transition, concretely, of the dynamical exponents that are related to the speed at which the system is driven. I argue about the reason for this dependence, claiming that it is due to the quasi-mean field nature of the plastic yielding transition originated in the fact that elastic interactions are long range.
THE LANDAU PROBLEM AND NONCOMMUTATIVE QUANTUM MECHANICS

We explore the conditions under which noncommutative quantum mechanics and the Landau problem are equivalent theories. If the potential in noncommutative quantum mechanics is chosen as V=Ωℵ with ℵ defined in the text, then for the value $\tilde\theta=0.22\times 10^{-11}~{\rm cm}^2$ (which measures the noncommutative effects of the space), the Landau problem and noncommutative quantum mechanics are equivalent theories in the lowest Landau level. For other systems one can find different values for $\tilde\theta$ and, therefore, the possible bounds for $\tilde\theta$ should be searched in a physical independent scenario. This last fact could explain the different bounds for $\tilde\theta$ found in the literature.
Some remarks on Dirac's hole theory versus quantum field theory

Dirac's hole theory and quantum field theory are generally considered to be equivalent to each other. However, it has been recently shown that this is not necessarily the case. In this article, we will discuss the reason for this lack of equivalence and suggest a possible solution.PACS Nos.: 03.65. w, 11.10. z
On stability of non-inflectional elastica

This study considers the stability of a non-inflectional elastica under a conservative end force subject to the Dirichlet, mixed, and Neumann boundary conditions. It is demonstrated that the non-inflectional elastica subject to the Dirichlet boundary conditions is unconditionally stable, while for the other two boundary conditions, sufficient criteria for stability depend on the signs of the second derivatives of the tangent angle at the endpoints.
The accreted stellar halo as a window on halo assembly in L* galaxies

Theory and observations agree that the properties of the accreted stellar halo (ASH) of Milky Way-like galaxies display significant scatter. Here, I take advantage of this stochasticity, and explore on inverting the link between halo assembly history (HAH) and ASH. I use tens of thousands of mock ASHs, corresponding to 750 $\Lambda$CDM HAHs sharing the same final virial mass. Hosts with poor/rich ASHs assemble following systematically different HAHs, according to orthogonal patterns of growth. Chiefly, hosts with rich ASHs experience accretion events (AEs) with high virial mass ratios (HVMRs, $M_s/M_h\gtrsim 0.1$) at intermediate times, $0.5\lesssim z_{infall}\lesssim1.5$, in a phase of fast growth. This maximises the accreted stellar mass under the condition these satellites are disrupted by $z=0$. At similar times, hosts with poor ASHs grow more slowly through minor mergers alone: HVMR AEs take place more recently, at $z_{infall}\lesssim0.5$, resulting in a distinctive population of surviving massive satellites (stellar mass $\log M_{s,*}/M_\odot\gtrsim 9$). Within these two fundamental modes of growth, hosts with ASHs of comparable richness but concentrated/extended profiles display systematic differences in the length and intensity of the different growth phases. Intriguingly, several properties of the Milky Way are in agreement with the predictions of this framework for hosts with poor and concentrated ASHs, including: i) the recent infall of Sagittarius and Magellanic Clouds, ii) the likely higher-than-average concentration of its dark halo, iii) the signatures of fast chemical enrichment of a sizeable fraction of its halo stellar populations.
Where does galactic dust come from

Here we investigate the origin of the dust mass (Mdust) observed in the Milky Way (MW) and of dust scaling relations found in a sample of local galaxies from the DGS and KINGFISH surveys. To this aim, we model dust production from Asymptotic Giant Branch (AGB) stars and supernovae (SNe) in simulated galaxies forming along the assembly of a Milky Way-like halo in a well resolved cosmic volume of 4cMpc using the GAMESH pipeline. We explore the impact of different sets of metallicity and mass-dependent AGB and SN dust yields on the predicted Mdust. Our results show that models accounting for grain destruction by the SN reverse shock predict a total dust mass in the MW that is a factor of ~4 lower than observed, and can not reproduce the observed galaxy-scale relations between dust and stellar masses, and dust-to-gas ratios and metallicity, with a smaller discrepancy in galaxies with low metallicity (12 + log(O/H) < 7.5) and low stellar masses (Mstar < 10^7 Msun). In agreement with previous studies, we suggest that competing processes in the interstellar medium must be at play to explain the observed trends. Our result reinforces this conclusion by showing that it holds independently of the adopted AGB and SN dust yields.
Near-Infrared Adaptive Optics Spectroscopy of Binary Brown Dwarfs HD 130948B and HD 130948C

We present near-infrared spectroscopy of low-mass companions in a nearby triple system HD 130948 (Gliese 564, HR 5534). Adaptive optics on the Subaru Telescope allowed spectroscopy of the individual components of the 0. ″13 binary system. Based on a direct comparison with a series of template spectra, we determined the spectral types of HD 130948B and C to be L4 ± 1. If we take the young age of the primary star into account (0.3-0.8 Gyr), HD 130948B and 130948C most likely are a binary brown dwarf system.
Structure formation with a long-range scalar dark matter interaction

Numerical simulations show that a long-range scalar interaction in a single species of massive dark matter particles causes voids between the concentrations of large galaxies to be more nearly empty, suppresses accretion of intergalactic matter onto galaxies at low redshift, and produces an early generation of dense dark matter halos. These three effects, in moderation, seem to be improvements over the {lambda}CDM model predictions for cosmic structure formation. Because the scalar interaction in this model has negligible effect on laboratory physics and the classical cosmological tests, it offers an observationally attractive example of cosmology with complicated physics in the dark sector, notably a large violation of the weak equivalence principle.