Miracle-dz/UniFAR-FTUs huggingface dataset:
Paternal Diet before Conception and Its Social Determinants in the Elfe Cohort

This study aimed to characterize paternal diet during the peri-conception period and its associated characteristics. These cross-sectional analyses were based on 998 fathers from the French nationwide ELFE birth cohort recruited in 2011. Fathers’ diet before mothers’ pregnancies was assessed by a 46-item food frequency questionnaire. Six exploratory dietary patterns were identified by principal component analysis: “Diverse diet”, “Balanced”, “Alcohol”, “Snacking”, “Bread and cheese”, and “Processed products”. Older age was related to higher scores for the “Balanced”, “Alcohol”, and “Snacking” patterns, and high education level with high scores on the “Balanced” pattern and low scores on the “Processed products” pattern. Unemployment and having a first child were related to high scores on the “Alcohol” pattern. Smoking was positively related to “Alcohol” and “Processed products” patterns. A restrictive diet was associated with high scores on the “Balanced” and “Processed products” patterns and low scores on “Alcohol”, “Snacking”, and “Bread and cheese” patterns. Maternal dietary patterns, identified in a previous analysis, were moderately and positively related to the similar patterns among fathers. These findings are important for screening fathers at risk of a suboptimal diet and for accounting for this factor in future studies to examine the specific influence of paternal diet on a child’s health and development.
Sir Maurice Kendall (1907–1983)

Maurice George Kendall was an extraordinarily versatile and influential leader in statistics. He distinguished himself as a prolific and effective expositor of statistical theory, and also made important contributions to nonparametric statistics, time series, symmetric functions, and the history of statistics. An innovative organizer, he launched a Dictionary of Statistical Terms and a Bibliography of the Statistical Literature, and served as Director of the World Fertility Survey.
THE TWO PHASES OF GALAXY FORMATION

Cosmological simulations of galaxy formation appear to show a “two-phase” character with a rapid early phase at z ≳ 2 during which “in situ” stars are formed within the galaxy from infalling cold gas followed by an extended phase since z ≲ 3 during which “ex situ” stars are primarily accreted. In the latter phase, massive systems grow considerably in mass and radius by accretion of smaller satellite stellar systems formed at quite early times (z>3) outside of the virial radius of the forming central galaxy. These tentative conclusions are obtained from high-resolution re-simulations of 39 individual galaxies in a full cosmological context with present-day virial halo masses ranging from 7 × 1011 M☉ h−1 ≲Mvir ≲ 2.7 × 1013 M☉ h−1 (h = 0.72) and central galaxy masses between 4.5 × 1010 M☉ h−1 ≲ M* ≲ 3.6 × 1011 M☉ h−1. The simulations include the effects of a uniform UV background, radiative cooling, star formation, and energetic feedback from Type II supernova. The importance of stellar accretion increases with galaxy mass and toward lower redshift. In our simulations, lower mass galaxies (M* ≲ 9 × 1010 M☉ h−1) accrete about 60% of their present-day stellar mass. High-mass galaxy (M* ≳ 1.7 × 1011 M☉ h−1) assembly is dominated by accretion and merging with about 80% of the stars added by the present day. In general the simulated galaxies approximately double their mass since z = 1. For massive systems this mass growth is not accompanied by significant star formation. The majority of the in situ created stars are formed at z>2, primarily out of cold gas flows. We recover the observational result of “archaeological downsizing,” where the most massive galaxies harbor the oldest stars. We find that this is not in contradiction with hierarchical structure formation. Most stars in the massive galaxies are formed early on in smaller structures; the galaxies themselves are assembled late.
Effect of Fe on the Hydrogen Production Properties of Al-Bi-Sn Composite Powders

Fe additives may play an important role in the preparation of aluminum-based hydrolysis hydrogen powder, with high hydrogen yield, low cost, and good oxidation resistance. Therefore, it is necessary to ascertain the effect of Fe on the hydrogen production performance of Al-Bi-Sn composite powders. According to the calculated vertical cross-section of the Al-10Bi-7Sn-(0~6)Fe (wt.%) quasi-binary system, Al-10Bi-7Sn-xFe (x = 0, 0.5, 1.5, 3) wt. % composite powders for hydrogen production were prepared by the gas-atomization method. The results showed that the Al-10Bi-7Sn-1.5Fe (wt.%) powder exhibited an extremely fast hydrogen generation rate at 50 °C, which reached 1105 mL·g−1 in 27 min in distilled water, 1086 mL·g−1 in 15 min in 0.1 mol·L−1 NaCl solution, and 1086 mL·g−1 in 15 min in 0.1 mol·L−1 CaCl2 solution. In addition, the antioxidant properties of these powders were also investigated. The results showed that the hydrogen production performance of the Al-10Bi-7Sn-1.5Fe (wt.%) powder could retain 91% of its hydrogen production activity, even though the powder was exposed to 25 °C and 60 RH% for 72 h. The addition of Fe not only promoted the hydrogen generation rate of the Al-Bi-Sn composite powders, but also improved their oxidation resistance. The Al-10Bi-7Sn-1.5Fe (wt.%) composite powder shows great potential for mobile hydrogen source scenarios with rapid hydrogen production.
ORIGIN OF MULTIPLE NUCLEI IN ULTRALUMINOUS INFRARED GALAXIES

Ultraluminous infrared galaxies (ULIRGs) with multiple (⩾3) nuclei are frequently observed. It has been suggested that these nuclei are produced by multiple major mergers of galaxies. The expected rate of such mergers is, however, too low to reproduce the observed number of ULIRGs with multiple nuclei. We have performed high-resolution simulations of the merging of two gas-rich disk galaxies. We found that extremely massive and compact star clusters form from the strongly disturbed gas disks after the first or second encounter between the galaxies. The mass of such clusters reaches ∼108 M☉ and their half-mass radii are 20–30 pc. Since these clusters consist of young stars, they appear as several bright cores in the galactic central region (∼kpc). The peak luminosity of these clusters reaches ∼10% of the total luminosity of the merging galaxy. These massive and compact clusters are consistent with the characteristics of the observed multiple nuclei in ULIRGs. Multiple mergers are not necessary to explain multiple nuclei in ULIRGs.
Motion of spinning test bodies in Kerr spacetime

Extreme mass ratios in astrophysical situations, for example as found in the galactic center, allow for an approximate analytic description of the motion in certain parameter regimes. The steadily improving observational situation of the galactic center [1–3] may soon enable us to test different competing theoretical approaches to model the motion of astrophysical objects in the theory of General Relativity. In this work we study the motion of extended spinning test bodies in a Kerr background. Our starting point is an explicit velocity formula based on the multipolar description [4–8] of pole-dipole test bodies, with the help of which we classify the orbital motion in the equatorial plane of a Kerr black hole for aligned and anti-aligned test body spin. An exact expression for the periastron shift is given and compared with corresponding post-Newtonian results. We provide an estimate of the test body spin corrections for orbits around the black hole in the galactic center. The structure of the paper is as follows. In section II we provide the equations of motion for spinning test bodies and derive a general formula which relates the momentum and the velocity of the test body. The motion of spinning test bodies is then studied in a Kerr background in section III. These equations of motion are of a mathematical structure which allows for an analytic solution [9, 10] and a systematic classification of different orbit types in section IV. In section V a general formula for the periastron shift is given and compared to corresponding post-Newtonian results. Our conclusions are drawn in section VI. In the appendices A and B we pro
A new step‐up DC‐DC converter with high gain for photovoltaic applications

Using interfacing converters with a high boost factor and high efficiency is essential for utilizing the solar cells energy since these energy sources produce low voltage levels. Although employing a high‐frequency transformer or coupled inductors in such converters results in high gain, these elements increase the weight, volume, and cost and affect the efficiency. This article presents a new topology for DC‐DC converter with a high voltage gain to overcome the mentioned problems. The converter provides a higher voltage gain than conventional structures while it includes only one power switch. The switch is connected to the ground; thus, a simple control circuit is required. Besides, the proposed structure has a low output voltage ripple. In this paper, the operating modes of the proposed topology, the influence of parasitic elements on the boost factor, and the efficiency have been described in detail. These item has been examined by experimental verifications. A 500‐W laboratory prototype confirms the proposed topology. Results demonstrate that the topology produces high efficiency and voltage gain.
Current Understanding of the Neural Stem Cell Niches

Neural stem cells (NSCs) are self-renewing, multipotent cells which give rise to all components of the central nervous system (CNS) during embryogenesis, but also activate in response to injury and disease and maintain a certain level of neurogenic activity throughout adulthood. This activity takes place in specialized regions of the brain, the neurovascular niches, whose main role is to control the behaviour of the CNS. In adult mammals, two main “canonical” niches have been described: The subventricular zone (SVZ) of the lateral ventricles and the subgranular zone (SGZ) of the dentate gyrus. This review discusses our current understanding of the neural stem cells and their canonical niches, as well as their structure, behaviours, and role in neural disease.
Effect of sugar replacement with stevia on quality of vanilla flavoured cow milk
set yoghurt

Stevia extracted from the leaf of Stevia rebaudiana Bertoni plant is a natural alternative sweetener that has the potential to be used as a sugar replacer in sweetened dairy products. The current study aimed to investigate the effect of sugar replacement with stevia extract on the quality of vanilla flavoured cow milk set yoghurt. Cow milk was standardized to 3% fat and 12% milk solids non-fat. Commercially available pure stevia extract was used to replace the sugar (maintained at 8% in the control) at the rate of 0 (control), 25% (T1), 50% (T2), 75% (T3) and 100% (T4) in cow milk set yoghurt. Yoghurt mixtures were separately heat treated (85°C/30 mins), cooled to inoculation temperature (42°C), inoculated with commercial yoghurt culture containing Streptococcus thermophilus and Lactobacillus delbruekii subsp. bulgaricus (1:1 ratio) and incubated till the pH reaches nearly 4.6. Set yoghurt samples were tested for chemical composition, organoleptic attributes, physicochemical and physical properties using standard procedures. Total calorie content was calculated per 100 g of yoghurt. Milk fermentation characteristics, water holding capacity and instrumental colour of yoghurt were not affected (p>0.05) by the sugar replacement with stevia. Carbohydrate content showed a decrease while protein and ash showed an increasing trend with an increasing level of sugar replacement in yoghurt. A 100% sugar replacement with stevia resulted in a 16.83% reduction in the calorie content of yoghurt. Control, as well as 100% sugar replaced yoghurt, obtained higher sensory scores while in the other treatments a decreasing trend in the sensory score was observed with the increasing level of sugar replacement suggesting possible interaction of stevia compounds with sucrose. It can be concluded that the replacement of 100% sugar is possible with the commercially available stevia extract used in the current study for the production of vanilla flavoured set yoghurt.
Sport policy in Finland

ABSTRACT The aim of this paper is to provide a description and create an understanding of public sport policy, the key actors within the sports system, and the political sphere in Finnish sport. The development of sport policy in Finland has been characterised by a relatively long-lasting, polarised, and highly politicised sports sector and a series of structural reforms. The contemporary sports system in Finland represents a mixed model, in which the state has a strong role in directing sport policy (especially through resource steering), while the role of sports organisations is implementation. Further, municipalities play a central role in creating conditions for sport and physical activity, and all sport policy actors have high autonomy in their operations. In particular, the population’s increasing physical inactivity and lack of elite sport success in Finland have driven the central government to seek new solutions, such as centralisation, a cross-administrative approach, and evidence-informed policy-making practices. Sport policy is also impacted by international trends and agreements, such as sustainable development, in which Finland’s ambitious goals affect the sports sector. In the future, the unclear roles of different actors and a lack of leadership could cause further challenges to the adoption of effective sport policies.
Cosmic ray backgrounds for dark matter indirect detection

The identification of the relic particles which presumably constitute cold dark matter is a key challenge for astroparticle physics. Indirect methods for their detection using high energy astro- physical probes such as cosmic rays have been much discussed. In particular, recent ‘excesses’ in cosmic ray electron and positron fluxes, as well as in microwave sky maps, have been claimed to be due to the annihilation or decay of dark matter. In this thesis, we argue however that these signals are plagued by irreducible astrophysical backgrounds and show how plausible con- ventional physics can mimic the alleged dark matter signals. In chapter 1, we review evidence of, and possible particle candidates for, cold dark matter, as well as our current understanding of galactic cosmic rays and the state-of-the-art in indirect detection. All other chapters contain original work, mainly based on the author’s journal publications. In particular, in chapter 2, we consider the possibility that the rise in the positron fraction observed by the PAMELA satellite is due to the production through (hadronic) cosmic ray spallation and subsequent acceleration of positrons, in the same sources as the primary cosmic rays. We present a new (unpublished) analytical estimate of the range of possible fluctuations in the high energy electron flux due to the discreteness of plausible cosmic ray sources such as supernova remnants. Fitting our result for the total electron-positron flux measured by the Fermi satellite allows us to fix the only free parameter of the model and make an independent prediction for the positron fraction. Our explanation relies on a large number of supernova remnants nearby which are accelerating hadronic cosmic rays. Turning the argument around, we find encouraging prospects for the observation of neutrinos from such sources in km^3-scale detectors such as IceCube. Chapter 3 presents a test of this model by considering similar effects expected for nuclear secondary-to-primary ratios such as B/C. A rise predicted above O(100)GeV/n would be an unique confirmation of our explanation for a rising positron fraction and rule out the dark matter explanation. In chapter 4, we review the assumptions made in the extraction of the `WMAP haze' which has also been claimed to be due to electrons and positrons from dark matter annihilation in the Galactic centre region. We argue that the energy-dependence of their diffusion means that the extraction of the haze through fitting to templates of low frequency diffuse galactic radio emission is unreliable. The systematic effects introduced by this can, under specific circumstances, reproduce the residual, suggesting that the ‘haze’ may be just an artefact of the template subtraction. We present a summary and thoughts about further work in the epilogue.
DO BARS TRIGGER ACTIVITY IN GALACTIC NUCLEI?

We investigate the connection between the presence of bars and active galactic nucleus (AGN) activity, using a volume-limited sample of ∼9000 late-type galaxies with axis ratio b/a > 0.6 and Mr < −19.5 + 5 log h at low redshift (0.02 ⩽ z ≲ 0.055), selected from Sloan Digital Sky Survey Data Release 7. We find that the bar fraction in AGN-host galaxies (42.6%) is ∼2.5 times higher than in non-AGN galaxies (15.6%), and that the AGN fraction is a factor of two higher in strong-barred galaxies (34.5%) than in non-barred galaxies (15.0%). However, these trends are simply caused by the fact that AGN-host galaxies are on average more massive and redder than non-AGN galaxies because the fraction of strong-barred galaxies (fSB) increases with u − r color and stellar velocity dispersion. When u − r color and velocity dispersion (or stellar mass) are fixed, both the excess of fSB in AGN-host galaxies and the enhanced AGN fraction in strong-barred galaxies disappears. Among AGN-host galaxies we find no strong difference of the Eddington ratio distributions between barred and non-barred systems. These results indicate that AGN activity is not dominated by the presence of bars, and that AGN power is not enhanced by bars. In conclusion, we do not find clear evidence that bars trigger AGN activity.
Twisted Mass Finite Volume Effects

We calculate finite-volume effects on the pion masses and decay constant in twisted mass lattice QCD at finite lattice spacing. We show that the lighter neutral pion in twisted mass lattice QCD gives rise to finite-volume effects that are exponentially enhanced when compared to those arising from the heavier charged pions. We demonstrate that the recent two flavor twisted mass lattice data can be better fitted when twisted mass effects in finite-volume corrections are taken into account.
MOLECULAR CLOUDS IN THE TRIFID NEBULA M20: POSSIBLE EVIDENCE FOR A CLOUD–CLOUD COLLISION IN TRIGGERING THE FORMATION OF THE FIRST GENERATION STARS

A large-scale study of the molecular clouds toward the Trifid Nebula, M20, has been made in the J = 2–1 and J = 1–0 transitions of 12CO and 13CO. M20 is ionized predominantly by an O7.5 star HD164492. The study has revealed that there are two molecular components at separate velocities peaked toward the center of M20 and that their temperatures—30–50 K as derived by a large velocity gradient analysis—are significantly higher than the 10 K of their surroundings. We identify the two clouds as the parent clouds of the first generation stars in M20. The mass of each cloud is estimated to be ∼103 M☉ and their separation velocity is ∼8 km s−1 over ∼1–2 pc. We find that the total mass of stars and molecular gas in M20 is less than ∼3.2 × 103 M☉, which is too small by an order of magnitude to gravitationally bind the system. We argue that the formation of the first generation stars, including the main ionizing O7.5 star, was triggered by the collision between the two clouds in a short timescale of ∼1 Myr, a second example alongside Westerlund 2, where a super-star cluster may have been formed due to cloud–cloud collision triggering.
On the nature of the barlens component in barred galaxies

Barred galaxies have very interesting morphological features. Here we examine the barlens, a lens-like component whose extent along the bar major axis is shorter than that of the bar and whose outline is oval or circular. We show that such a component can also be found in a number of N-body plus SPH simulations. We analyse its properties by converting simulation snapshots into images, which we then analyse in the same way as images of observed galaxies. We make extensive comparisons with galaxies from the NIRS0S (Near Infrared S0 Survey) and the S$^4$G (Spitzer Stellar Structure Survey of Galaxies) samples and find very good agreement. These comparisons include morphology, radial projected density profiles, shapes, sizes and fluxes. We observe the barlens component in our simulations from different viewing angles. This reveals that {\it barlenses are the vertically thick part of the bar seen face-on, i.e. that a barlens seen edge-on is a boxy/peanut/X bulge}. This finding makes it possible to follow barlens dynamics in terms of already studied families of periodic orbits. Some barlenses, notably those with near-circular projected isodensity curves, can be mistaken for classical bulges in morphological studies and classifications. This can introduce severe errors in modelling of individual galaxies, since the dynamics of classical bulges is very different from that of peanuts, and a bias in statistical morphological studies, leading to overestimates of the true frequency and mass of classical bulges. Thus, properly accounting for the barlens component will show that the fraction of disc galaxies lacking a classical bulge can be much larger than so far believed. Finally, based on the shape of the isodensity curves, we propose a rule of thumb for measuring the barlens extent along the bar major axis of galaxies sufficiently far from edge-on for the peanut not to be visible.
PRESUPERNOVA EVOLUTION AND EXPLOSIVE NUCLEOSYNTHESIS OF ZERO METAL MASSIVE STARS

We present a new set of zero metallicity models in the range 13–80 M☉ together to the associated explosive nucleosynthesis. These models are fully homogeneous with the solar metallicity set we published in Limongi & Chieffi and will be freely available at the Online Repository for the FRANEC Evolutionary Output Web site. A comparison between these yields and an average star that represents the average behavior of most of the very metal-poor stars in the range −5.0 < [Fe/H] < −2.5 confirms previous findings that only a fraction of the elemental [X/Fe] may be fitted by the ejecta of standard core collapse supernovae.
CCTV News’ Asymmetric Impact on the Chinese Stock Market during COVID-19: A Combination Analysis Based on the SVAR and NARDL Models

ABSTRACT This study uses the structural vector autoregression (SVAR) and nonlinear autoregressive distributed lag (NARDL) models to examine the long- and short-term asymmetric effects of structural state media shocks on the Chinese stock market. The findings, obtained using Xinwen Lianbo as a stand-in for state media, indicate that attention shocks on Xinwen Lianbo have an asymmetrical impact on the aggregate stock market returns in both the short and long run. The sectoral and overall stock market results are similar, with CCTV having a stronger impact in the first half of the pandemic. Employing other COVID-19 news measurements, we validated our primary findings and discovered that the price function differs among various state media’s attention to COVID-19.