Miracle-dz/UniFAR-FTUs huggingface dataset:
The action of phytochemicals present in cocoa in the prevention of vascular dysfunction and atherosclerosis

Background: Chronic non-communicable diseases, including cardiovascular diseases (CVDs), have caused many deaths worldwide. Atherosclerotic plaque formation is common in individuals with CVDs. Thus, antioxidant and anti-inflammatory nutritional strategies can be used to prevent or inhibit this process. Due to its higher concentrations of cocoa, dark chocolate is considered a functional food due to the presence and action of phytochemical compounds, with anti-inflammatory and antioxidant actions. However, the recommended amounts of these compounds to prevent atherosclerosis have not yet been fully elucidated. Aim: The aim of the studywas to review the effects of cocoa and dark chocolate intake on the prevention of cardiovascular dysfunction and atherosclerosis. Methods: This narrative review was based on a search of PubMed and Lilacs. The search was conducted from September 2021 to February 2022 using the following keywords: flavonoids, cocoa, atherosclerosis, oxidative stress, and inflammation. The inclusion criteria were original articles, meta-analyses, and experimental and clinical studies published between 2002 and 2022 in English, focusing on the subject addressed. The exclusion criteria were the title and abstract reading and duplication of articles in the databases. Results: The antioxidant and anti-inflammatory functions of phytochemicals in cocoa and dark chocolate are related to the modulation of nitric oxide through activation/phosphorylation and acting as a vasodilator. Furthermore, these phytochemicals reduce the formation of reactive oxygen species and activate antioxidant enzymes. The anti-inflammatory activities are related to the modulation of nuclear factor kappa B in the reduction of inflammatory markers, such as tumor necrosis factor-alpha, C-reactive protein, and pro-inflammatory cytokines, as well as in the reduction of adhesion molecules in the wall of the vases. Conclusion: The main phytochemicals present in cocoa and dark chocolates are catechins and their epicatechin isomers, which are responsible for improving inflammatory, metabolic, and antioxidant profiles. Its consumption can be encouraged, but with caution, owing to the caloric supply and forms of chocolate production, as these factors can reduce the presence of flavonoids in its composition. Relevance for Patients: The antioxidant and anti-inflammatory functions of the phytochemicals in cocoa and dark chocolate are responsible for modulating nitric oxide via activation/phosphorylation and acting as a vasodilator. Reducing the formation of reactive oxygen species, as well as activating antioxidant enzymes. As for the anti-inflammatory activities, they modulate the nuclear factor kappa B, reducing inflammatory markers, thus improving the antioxidant and inflammatory profile of these patients.
Kepler exoplanets: a new method of population analysis

This paper introduces a new method of inferring the intrinsic exoplanet population from Kepler data, based on the assumption that the frequency of exoplanets can be represented by a smooth function of planet radius and period. The method is applied to the two most recent data releases from the Kepler project, q1-16 and q1-17, over the range of periods 0.5 to 512 days, and radii 0.5 to 16 Earth radii. Both of these releases have known biases, with the first believed to contain excess false positives, and the second excess false negatives, so any analysis of them should be viewed with caution. We apply the new method of population estimation to these releases, treating them like practice data sets. With this method, we tentatively find that the average number of planets per star would be about $5.7\pm0.8$ for F stars, $5.0\pm0.2$ for G stars, $4.0\pm0.3$ for K stars, and $6.5\pm1.7$ for M stars, indicating a decreasing trend with FGK spectral type, but an upward jump for M stars. A second conclusion is that the number of planets per G star, per natural log unit of period (days) and radii (Earths) at the period and radius of the Earth around the Sun, is about $\Gamma_\oplus(G) = 1.1\pm 0.1$. A related parameter, $\eta_{\oplus}$, which in addition depends on the range of period and radius considered, is found to be $\eta_{\oplus}(G) \simeq 1.0 \pm 0.1 $. More definitive conclusions, and validation of these preliminary values, await the final release of Kepler's transiting exoplanet list.
AGN-driven quenching of star formation: morphological and dynamical implications for early-type galaxies

In order to understand the physical mechanisms at work during the formation of massive early-type galaxies, we performed six zoomed hydrodynamical cosmological simulations of halos in the mass range 4.3 10^12 < M_vir < 8.0 10^13 M_sun at z=0, using the Adaptive Mesh Refinement code RAMSES. These simulations explore the role of Active Galactic Nuclei (AGN), through jets powered by the accretion onto supermassive black holes on the formation of massive elliptical galaxies. In the absence of AGN feedback, large amounts of stars accumulate in the central galaxies to form overly massive, blue, compact and rotation-dominated galaxies. Powerful AGN jets transform the central galaxies into red extended and dispersion-dominated galaxies. This morphological transformation of disc galaxies into elliptical galaxies is driven by the efficient quenching of the in situ star formation due to AGN feedback, which transform these galaxies into systems built up by accretion. For galaxies mainly formed by accretion, the proportion of stars deposited farther away from the centre increases, and galaxies have larger sizes. The accretion is also directly responsible for randomising the stellar orbits, increasing the amount of dispersion over rotation of stars as a function of time. Finally, we find that our galaxies simulated with AGN feedback better match the observed scaling laws, such as the size-mass, velocity dispersion-mass, fundamental plane relations, and slope of the total density profiles at z~0, from dynamical and strong lensing constraints.
Full Monte Carlo simulations of radio emission from extensive air showers with CoREAS

CoREAS is a Monte Carlo simulation code for the calculation of radio emission from extensive air showers. It is based on the "endpoint formalism" for radiation from moving charges implemented directly in CORSIKA. Consequently, the full complexity of the air-shower physics is taken into account without the need for approximations or assumptions on the emission mechanism. We present results of simulations for an unthinned shower performed with CoREAS for both MHz and GHz frequencies. At MHz frequencies, the simulations predict the well-known mixture of geomagnetic and charge excess radiation. At GHz frequencies, the emission is strongly influenced by Cherenkov effects arising from the varying refractive index in the atmosphere. In addition, a qualitative difference in the symmetry of the GHz radiation pattern is observed when compared to the ones at lower frequencies. We also discuss the strong increase in the ground area subtended by the radio emission when going from near-vertical to very inclined geometries, making very inclined air showers the most promising ones for cosmic ray radio detection.
A study of selection methods for Hα-emitting galaxies at z~1.3 for the Subaru/FMOS galaxy redshift survey for cosmology (FastSound)

The efficient selection of high-redshift emission galaxies is important for future large galaxy redshift surveys for cosmology. Here we describe the target selection methods for the FastSound project, a redshift survey for H alpha emitting galaxies at z=1.2-1.5 using Subaru/FMOS to measure the linear growth rate f\sigma 8 via Redshift Space Distortion (RSD) and constrain the theory of gravity. To select ~400 target galaxies in the 0.2 deg^2 FMOS field-of-view from photometric data of CFHTLS-Wide (u*g'r'i'z'), we test several different methods based on color-color diagrams or photometric redshift estimates from spectral energy distribution (SED) fitting. We also test the improvement in selection efficiency that can be achieved by adding near-infrared data from the UKIDSS DXS (J). The success rates of H alpha detection with FMOS averaged over two observed fields using these methods are 11.3% (color-color, optical), 13.6% (color-color, optical+NIR), 17.3% (photo-z, optical), and 15.1% (photo-z, optical+NIR). Selection from photometric redshifts tends to give a better efficiency than color-based methods, although there is no significant improvement by adding J band data within the statistical scatter. We also investigate the main limiting factors for the success rate, by using the sample of the HiZELS H alpha emitters that were selected by narrow-band imaging. Although the number density of total H alpha emitters having higher H alpha fluxes than the FMOS sensitivity is comparable with the FMOS fiber density, the limited accuracy of photometric redshift and H alpha flux estimations have comparable effects on the success rate of <~20% obtained from SED fitting.
Quantum probabilities of composite events in quantum measurements with multimode states

The problem of defining quantum probabilities of composite events is considered. This problem is of great importance for the theory of quantum measurements and for quantum decision theory, which is a part of measurement theory. We show that the Lüders probability of consecutive measurements is a transition probability between two quantum states and that this probability cannot be treated as a quantum extension of the classical conditional probability. The Wigner distribution is shown to be a weighted transition probability that cannot be accepted as a quantum extension of the classical joint probability. We suggest the definition of quantum joint probabilities by introducing composite events in multichannel measurements. The notion of measurements under uncertainty is defined. We demonstrate that the necessary condition for mode interference is the entanglement of the composite prospect together with the entanglement of the composite statistical state. As an illustration, we consider an example of a quantum game. Special attention is paid to the application of the approach to systems with multimode states, such as atoms, molecules, quantum dots, or trapped Bose-condensed atoms with several coherent modes.
Child Custody after Divorce Laws in Malaysia: Muslim Parents and Children Perspective

Child custody after divorce laws in Malaysia advocates sole custody as the main practice. Sole custody means the child will live with a parent and have contact with the other parent through access. The parent living with the child will also have parental responsibility. Social studies have suggested that sole custody generates problems that affect the best interests of the child. Some problems are lack of contact and the child being deprived of maintenance. Other countries have undergone legal reforms to better the situation through joint custody. Joint custody advocates sharing the child's residence and parental responsibility. Therefore, this article examines the experiences the selected Muslim parents and children faced regarding child custody. The experiences concern the legal process of divorce, child custody, the residence of the child and access, parental responsibility, and parental relationships. An important finding is the general recognition of joint custody by the Shari'ah courts, the parents, and the children. However, the recognition must be in line with the best interests of the child.
Optical and radio properties of extragalactic radio sources with recurrent jet activity

We present a sample of 74 radio sources with recurrent jet activity. The sample consists of 67 galaxies, 2 quasars and 5 unidentified sources, selected from the published data or are newly recognized. The sample's redshift range is 0.002 < z < 0.7 and the size of inner and outer structures varies from 0.02 to 4248 kpc. We analyse the optical and radio properties of the sample and compare them with the characteristics of ordinary one-off FRII radio sources. With the help of stellar population modelling, we derive black hole masses and stellar masses of host galaxies of 35 restarting radio sources, finding that the black hole masses in restarting radio sources are comparable to those of typical single-cycle FRII radio sources. The obtained median values of log M$_{BH}$ are 8.58 and 8.62 M$_{\odot}$ Unlike the black hole masses, the stellar masses in restarting radio sources tend to be smaller than in the FRII sources. Although the stellar populations of the hosts of recurrent activity sources are dominated by old stars, a significant fraction of young stars can be observed as well. Based on the Sloan Digital Sky Survey photometric observations, we also analyse the morphology of the host galaxies and obtained significantly smaller concentration indices for the restarting radio sources when compared to the classical FRII hosts. This effect can be interpreted as a result of frequent merger events in the history of host galaxies of restarting radio sources.
TOWARD A DETERMINISTIC MODEL OF PLANETARY FORMATION. VII. ECCENTRICITY DISTRIBUTION OF GAS GIANTS

The ubiquity of planets and diversity of planetary systems reveal that planet formation encompasses many complex and competing processes. In this series of papers, we develop and upgrade a population synthesis model as a tool to identify the dominant physical effects and to calibrate the range of physical conditions. Recent planet searches have led to the discovery of many multiple-planet systems. Any theoretical models of their origins must take into account dynamical interactions between emerging protoplanets. Here, we introduce a prescription to approximate the close encounters between multiple planets. We apply this method to simulate the growth, migration, and dynamical interaction of planetary systems. Our models show that in relatively massive disks, several gas giants and rocky/icy planets emerge, migrate, and undergo dynamical instability. Secular perturbation between planets leads to orbital crossings, eccentricity excitation, and planetary ejection. In disks with modest masses, two or less gas giants form with multiple super-Earths. Orbital stability in these systems is generally maintained and they retain the kinematic structure after gas in their natal disks is depleted. These results reproduce the observed planetary mass–eccentricity and semimajor axis–eccentricity correlations. They also suggest that emerging gas giants can scatter residual cores to the outer disk regions. Subsequent in situ gas accretion onto these cores can lead to the formation of distant (≳ 30 AU) gas giants with nearly circular orbits.
GAS GAPS IN THE PROTOPLANETARY DISK AROUND THE YOUNG PROTOSTAR HL TAU

We have analyzed the HCO+ (1–0) data of the Class I–II protostar, HL Tau, obtained from the Atacama Large Millimeter/submillimeter Array long baseline campaign. We generated the HCO+ image cube at an angular resolution of ∼0. ″07 (∼10 au) and performed azimuthal averaging on the image cube to enhance the signal-to-noise ratio and measure the radial profile of the HCO+ integrated intensity. Two gaps at radii of ∼28 and ∼69 au and a central cavity are identified in the radial intensity profile. The inner HCO+ gap is coincident with the millimeter continuum gap at a radius of 32 au. The outer HCO+ gap is located at the millimeter continuum bright ring at a radius of 69 au and overlaps with the two millimeter continuum gaps at radii of 64 and 74 au. On the contrary, the presence of the central cavity is likely due to the high optical depth of the 3 mm continuum emission and not the depletion of the HCO+ gas. We derived the HCO+ column density profile from its intensity profile. From the column density profile, the FWHM widths of the inner and outer HCO+ gaps are both estimated to be ∼14 au, and their depths are estimated to be ∼2.4 and ∼5.0. These results are consistent with the expectation from the gaps opened by forming (sub-)Jovian mass planets, while placing tight constraints on the theoretical models solely incorporating the variation of dust properties and grain sizes.
Angular momentum evolution in dark matter haloes: a study of the Bolshoi and Millennium simulations

We use three different cosmological dark matter simulations to study how the orientation of the angular momentum vector (AM) in dark matter haloes evolve with time. We find that haloes in this kind of simulations are constantly affected by a spurious change of mass, which translates into an artificial change in the orientation of the AM. After removing the haloes affected by artificial mass change, we found that the change in the orientation of the AM vector is correlated with time. The change in its angle and direction (i.e. the angle subtended by the AM vector in two consecutive timesteps) that affect the AM vector has a dependence on the change of mass that affects a halo, the time elapsed in which the change of mass occurs and the halo mass. We create a Monte-Carlo simulation that reproduces the change of angle and direction of the AM vector. We reproduce the angular separation of the AM vector since a look back time of 8.5 Gyrs to today ( $\rm \alpha$) with an accuracy of approximately 0.05 in $\rm cos(\alpha)$. We are releasing this Monte-Carlo simulation together with this publication. We also create a Monte Carlo simulation that reproduces the change of the AM modulus. We find that haloes in denser environments display the most dramatic evolution in their AM direction, as well as haloes with a lower specific AM modulus. These relations could be used to improve the way we follow the AM vector in low-resolution simulations.
Correlation between Bulk Thermodynamic Measurements and the Low-Temperature-Resistance Plateau in SmB 6

Topological insulators are materials characterized by dissipationless, spin-polarized surface states resulting from non-trivial band topologies. Recent theoretical models and experiments suggest that SmB6 is the first topological Kondo insulator, in which the topologically non-trivial band structure results from electron-electron interactions via Kondo hybridization. Here, we report that the surface conductivity of SmB6 increases systematically with bulk carbon content. Further, addition of carbon is linked to an increase in n-type carriers, larger low temperature electronic contributions to the specific heat with a characteristic temperature scale of T* = 17 K, and a broadening of the crossover to the insulating state. Additionally, X-ray absorption spectroscopy shows a change in Sm valence at the surface. Our results highlight the importance of phonon dynamics in producing a Kondo insulating state and demonstrate a correlation between the bulk thermodynamic state and low temperature resistance of SmB6.
Minimum-error discrimination of qubit states: Methods, solutions, and properties

We show a geometric formulation for minimum-error discrimination of qubit states that can be applied to arbitrary sets of qubit states given with arbitrary a priori probabilities. In particular, when qubit states are given with equal a priori probabilities, we provide a systematic way of finding optimal discrimination and the complete solution in a closed form. This generally gives a bound to cases when prior probabilities are unequal. Then it is shown that the guessing probability does not depend on detailed relations among the given states, such as the angles between them, but on a property that can be assigned by the set of given states itself. This also shows how a set of quantum states can be modified such that the guessing probability remains the same. Optimal measurements are also characterized accordingly, and a general method of finding them is provided. DOI: 10.1103/PhysRevA.87. 012334
Origin of the Characteristic X-ray Spectral Variations of IRAS 13224$-$3809

The Narrow-line Seyfert 1 galaxy (NLS1) IRAS 13224$-$3809 is known to exhibit significant X-ray spectral variation, a sharp spectral drop at $\sim$ 7 keV, strong soft excess emission, and a hint of iron L-edge feature, which is very similar to the NLS1 1H 0707$-$495. We have proposed the "Variable Double Partial Covering (VDPC) model" to explain the energy spectra and spectral variability of 1H 0707$-$495 (Mizumoto, Ebisawa and Sameshima 2014, PASJ, 66, 122). In this model, the observed flux/spectral variations below 10 keV within a $\sim$day are primarily caused by change of the partial covering fraction of patchy clouds composed by double absorption layers in the line of sight. In this paper, we apply the VDPC model to IRAS 13224$-$3809. Consequently, we have found that the VDPC model can explain the observed spectral variations of IRAS 13224$-$3809 in the 0.5$-$10 keV band. In particular, we can explain the observed Root Mean Square (RMS) spectra (energy dependence of the fractional flux variation) in the entire 0.5$-$10 keV band. In addition to the well-known significant drop in the iron K-band, we have found intriguing iron L-peaks in the RMS spectra when the iron L-edge is particularly deep. This feature, which is also found in 1H 0707$-$495, is naturally explained with the VDPC model, such that the RMS variations increase at the energies where optical depths of the partial absorbers are large. The absorbers have a larger optical depth at the iron L-edge than in the adjacent energy bands, thus a characteristic iron L-peak appears. On the other hand, just below the iron K-edge, the optical depth is the lowest and the RMS spectrum has a broad dip.
Magnetars: fact or fiction?

Anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs) are enigmatic pulsar-like objects. The energy budget is the fundamental problem in their studies. In the magnetar model, they are supposed to be powered by the extremely strong magnetic fields (>~ 10^14 G) of neutron stars. Observations for and against the magnetar model are both summarized. Considering the difficulties encountered by the magnetar model to comfortably understand more and more observations, one may doubt that AXPs and SGRs are really magnetars. If they are not magnetar candidates (including magnetar-based models), then they must be "quark star/fallback disk" systems.
The Power and Paradoxes of Evaluation Systems – Increasing Use but Impeding Change

In recent years, evaluation systems have become increasingly embedded within public sector organisations. This trend of systematising and institutionalising evaluation activities has generally been perceived as a way to increase the use – and thus the power - of evaluations. However, this article argues that the power of evaluation systems is of a more complicated nature than merely increasing the uptake of evaluative knowledge. By applying the concept of “contestability differential” to a concrete example of an evaluation system within the Danish employment services, it is shown how the institutionalisation of an asymmetric power relation between evaluation system and evaluand creates inherent paradoxes. The analysis shows how the strong contestability differential between evaluation system and evaluand – necessary for securing the influence of evaluation systems - hinges on the permanence, organisational embeddedness and epistemological fixation of such systems. However, these same elements simultaneously also limit the usefulness of the evaluative knowledge and the capability of the evaluation system to invoke radical change and development in the evaluand. The article thus highlights an inherent paradox of evaluation systems in that they are simultaneously increasing and decreasing the power of evaluations.