Miracle-dz/UniFAR-FTUs huggingface dataset:
Toxicological Assessment of Cellulose Nanomaterials: Oral Exposure

Cellulose nanomaterials (CNMs) have emerged recently as an important group of sustainable bio-based nanomaterials (NMs) with potential applications in multiple sectors, including the food, food packaging, and biomedical fields. The widening of these applications leads to increased human oral exposure to these NMs and, potentially, to adverse health outcomes. Presently, the potential hazards regarding oral exposure to CNMs are insufficiently characterised. There is a need to understand and manage the potential adverse effects that might result from the ingestion of CNMs before products using CNMs reach commercialisation. This work reviews the potential applications of CNMs in the food and biomedical sectors along with the existing toxicological in vitro and in vivo studies, while also identifying current knowledge gaps. Relevant considerations when performing toxicological studies following oral exposure to CNMs are highlighted. An increasing number of studies have been published in the last years, overall showing that ingested CNMs are not toxic to the gastrointestinal tract (GIT), suggestive of the biocompatibility of the majority of the tested CNMs. However, in vitro and in vivo genotoxicity studies, as well as long-term carcinogenic or reproductive toxicity studies, are not yet available. These studies are needed to support a wider use of CNMs in applications that can lead to human oral ingestion, thereby promoting a safe and sustainable-by-design approach.
Perception of Nursing Students Regarding Learning Enhancing Attitudes and Behaviours of Teachers

OBJECTIVES The purpose of this study was to identify the perceptions of nursing students regarding learning-enhancing factors of teachers’ attitudes and behavior. METHODOLOGY A descriptive cross-sectional study was conducted using a convenient sampling technique. Data were collected through a questionnaire from 125 nursing students at two public sector nursing colleges in Peshawar, Pakistan. Ethics approval was obtained from Institutional Review Board. Data were analyzed using SPSS version 20. RESULTS Out of the total selected sample, 31 participants were males and 94 were females. The mean age of respondents was 30 years. All the participants agreed that the attitude and behavior of teachers affected students learning. The most enhancing factors for the learning of nursing students were “Giving value to teaching”, “Motivation towards teaching”, “Accept Responsibility for the lecture”, “Having good knowledge of the subject matter”, and “Confidence in delivering the lecture”, “Interest in the lecture”, “Regular and punctual for class”, “Use Polite Language to students” etc.: While, “being suspicious about students success”, “Extra Expectation from students”, “Favoritism in students”, “Late for class”, “Punishing the students”, etc.: were regarded as not enhancing factors. CONCLUSION The nursing students were not fully satisfied with the nursing institutional environment. So, the teacher must adopt all those attitudinal and behavioral parameters which were perceived enhancing factors and avoid others.
The proper functioning of the sense of smell and its disturbances on the example of COVID-19 infection

COVD-19 disease causes a wide range of respiratory symptoms. One of them is the olfactory disorder, which is also associated with other viral infections. Impaired sense of smell is associated with damage to the respiratory epithelium. Sniffing problems lasting longer than a few days are reported by more than half of patients infected with SARSCov-2 virus. This problem affects the quality of life and may result, among other things, in eating disorders or an increase in exposure to harmful chemicals. The olfactory epithelium, containing receptor cells, is primarily responsible for the proper functioning of the sense of smell. Impaired smell in COVID 19 is associated with damage to the respiratory epithelium. The article is a review of the scientific literature, in which the issues related to the physiology and anatomical structure of the olfactory organ and the influence of SARSCov-2 virus infection on olfactory disorders were discussed.
Tuberculosis Family Support Training’s (TB FaST) Influence on Encouraging TB Treatment Compliance

Family support is necessary for tuberculosis (TB) treatment compliance. Family intentions and practices in providing support to TB patients require considerable improvement, which is possible via training. This study aimed to analyze the influence of tuberculosis family support training (TB FaST) on the family members’ intentions and practices in encouraging TB treatment compliance in the continuation phase. This quasi-experimental study with a pretest-posttest control group design involved 56 TB patients and 56 family members of patients who had undergone the continuation phase of category 1 TB treatment in the third and fourth months. All patients treated with tuberculosis were directly observed with treatment short-course (TB DOTS) at primary health care. All the subjects were divided into intervention and control groups. TB FaST was given only to the intervention group and delivered using a combination of lectures, case-based focused group discussions, and role-playing in problem-solving over two consecutive days. The result showed a significant improvement in the family support practices five weeks after training in the intervention group compared to the control group (p<0.05). However, only a slight improvement was observed in the family intentions (p>0.05). TB FaST mainly affects the practices of family members in providing family support to encourage TB treatment compliance in the continuation phase. We recommend that TB FaST or other educational tools be used again after TB FaST to improve intention.
Simulating galaxy evolution with a non-universal stellar initial mass function

We consider that the stellar initial mass function (IMF) depends on physical properties of star-forming molecular clouds in galaxies and thereby investigate how such a non-universal IMF (NUIMF) influences galaxy evolution. We incorporate a NUIMF model into galaxy-scale chemodynamical simulations in order to investigate the differences in chemical and dynamical evolution of disk galaxies between the NUIMF and universal IMF (UIMF) models. In the adopted NUIMF model, the three slopes of the Kroupa IMF depend independently on densities and metallicities ([Fe/H]) of molecular gas clouds, and production rates of metals and dust from massive and AGB stars can vary according to the time evolution of the three IMF slopes. The preliminary results of the simulations are as follows. Star formation rates in actively star-forming disk galaxies can be significantly lower in the NUIMF model than in the UIMF model, and the differences between the two models can be more remarkable in galaxies with higher SFRs. Chemical enrichment can proceed more rapidly in the NUIMF model and [Mg/Fe] for a given metallicity is higher in the NUIMF model. The evolution of H2 fraction (f_H2) and dust-to-gas ratio (D) is more rapid in the NUIMF model so that the final f_H2 and $D$ can be higher in the NUIMF model. Formation of massive stellar clumps in gas-rich disks is more strongly suppressed owing to the stronger SN feedback effect in the NUIMF model. The radial density profiles of new stars within the central 1kpc are shallower in the NUIMF model.
String dynamics and ejection along the axis of a spinning black hole

Relativistic current carrying strings moving axisymmetrically on the background of a Kerr black hole are studied. The boundaries and possible types of motion of a string with a given energy and current are found. Regions of parameters for which the string falls into the black hole, is trapped in a toroidal volume, or can escape to infinity, are identified, and representative trajectories are examined by numerical integration, illustrating various interesting behaviors. In particular, we find that a string can start out at rest near the equatorial plane and, after bouncing around, be ejected out along the axis, some of its internal (elastic or rotational kinetic) energy having been transformed into translational kinetic energy. The resulting velocity can be an order unity fraction of the speed of light. This process results from the presence of an outer tension barrier and an inner angular momentum barrier that are deformed by the gravitational field. We speculatively discuss the possible astrophysical significance of this mechanism as a means of launching a collimated jet of magnetohydrodynamics plasma flux tubes along the spin axis of a gravitating system fed by an accretion disk.
WIDE-FIELD HUBBLE SPACE TELESCOPE OBSERVATIONS OF THE GLOBULAR CLUSTER SYSTEM IN NGC 1399

We present a comprehensive high spatial resolution imaging study of globular clusters (GCs) in NGC 1399, the central giant elliptical cD galaxy in the Fornax galaxy cluster, conducted with the Advanced Camera for Surveys (ACS) aboard the Hubble Space Telescope (HST). Using a novel technique to construct drizzled point-spread function libraries for HST/ACS data, we accurately determine the fidelity of GC structural parameter measurements from detailed artificial star cluster experiments and show the superior robustness of the GC half-light radius, rh, compared with other GC structural parameters, such as King core and tidal radius. The measurement of rh for the major fraction of the NGC 1399 GC system reveals a trend of increasing rh versus galactocentric distance, Rgal, out to about 10 kpc and a flat relation beyond. This trend is very similar for blue and red GCs, which are found to have a mean size ratio of rh, red/rh, blue = 0.82 ± 0.11 at all galactocentric radii from the core regions of the galaxy out to ∼40 kpc. This suggests that the size difference between blue and red GCs is due to internal mechanisms related to the evolution of their constituent stellar populations. Modeling the mass density profile of NGC 1399 shows that additional external dynamical mechanisms are required to limit the GC size in the galaxy halo regions to rh ≈ 2 pc. We suggest that this may be realized by an exotic GC orbit distribution function, an extended dark matter halo, and/or tidal stress induced by the increased stochasticity in the dwarf halo substructure at larger galactocentric distances. We compare our results with the GC rh distribution functions in various galaxies and find that the fraction of extended GCs with rh ⩾ 5 pc is systematically larger in late-type galaxies compared with GC systems in early-type galaxies. This is likely due to the dynamically more violent evolution of early-type galaxies. We match our GC rh measurements with radial velocity data from the literature and split the resulting sample at the median rh value into compact and extended GCs. We find that compact GCs show a significantly smaller line-of-sight velocity dispersion, 〈σcmp〉 = 225 ± 25 km s−1, than their extended counterparts, 〈σext〉 = 317 ± 21 km s−1. Considering the weaker statistical correlation in the GC rh color and the GC rh–Rgal relations, the more significant GC size–dynamics relation appears to be astrophysically more relevant and hints at the dominant influence of the GC orbit distribution function on the evolution of GC structural parameters.
RESOLVING THE RADIO SOURCE BACKGROUND: DEEPER UNDERSTANDING THROUGH CONFUSION

We used the Karl G. Jansky Very Large Array to image one primary beam area at 3 GHz with 8″ FWHM resolution and 1.0 μJy beam−1 rms noise near the pointing center. The P(D) distribution from the central 10 arcmin of this confusion-limited image constrains the count of discrete sources in the 1 < S(μJy) < 10 range. At this level, the brightness-weighted differential count S2n(S) is converging rapidly, as predicted by evolutionary models in which the faintest radio sources are star-forming galaxies; and ≈96% of the background originating in galaxies has been resolved into discrete sources. About 63% of the radio background is produced by active galactic nuclei (AGNs), and the remaining 37% comes from star-forming galaxies that obey the far-infrared (FIR)/radio correlation and account for most of the FIR background at λ ≈ 160 μm. Our new data confirm that radio sources powered by AGNs and star formation evolve at about the same rate, a result consistent with AGN feedback and the rough correlation of black hole and stellar masses. The confusion at centimeter wavelengths is low enough that neither the planned Square Kilometre Array nor its pathfinder ASKAP EMU survey should be confusion limited, and the ultimate source detection limit imposed by “natural” confusion is ⩽0.01 μJy at ν = 1.4 GHz. If discrete sources dominate the bright extragalactic background reported by ARCADE 2 at 3.3 GHz, they cannot be located in or near galaxies and most are ⩽0.03 μJy at 1.4 GHz.
A luminous hot accretion flow in the low-luminosity active galactic nucleus NGC 7213

The active galactic nucleus (AGN) NGC 7213 shows a complex correlation between the monochromatic radio luminosity $L_R$ and the 2--10 keV X-ray luminosity $L_X$, i.e. the correlation is unusually weak with $p\sim 0$ (in the form $L_R\propto L_X^p$) when $L_X$ is below a critical luminosity, and steep with $p>1$ when $L_X$ is above that luminosity. Such a hybrid correlation in individual AGNs is unexpected as it deviates from the Fundamental Plane of AGN activity. Interestingly, a similar correlation pattern is observed in the black hole X-ray binary H1743--322, where it has been modelled by switching between different modes of accretion. We propose that the flat $L_R$--$L_X$ correlation of NGC 7213 is due to the presence of a luminous hot accretion flow, an accretion model whose radiative efficiency is sensitive to the accretion rate. Given the low luminosity of the source, $L_X\sim 10^{-4}$ of the Eddington luminosity, the viscosity parameter is determined to be small, $\alpha\approx 0.01$. We also modelled the broad-band spectrum from radio to $\gamma$-rays, the time lag between the radio and X-ray light curves, and the implied size and the Lorentz factor of the radio jet. We predict that NGC 7213 will enter into a two-phase accretion regime when $L_X > 1.5 \times 10^{42}\, {\rm erg\,s^{-1}}$. When this happens, we predict a softening of the X-ray spectrum with the increasing flux and a steep radio/X-ray correlation.
The Effect of Augmented Reality-based Learning Media on Student Learning Motivation for Computer Course

: Augmented reality is one of the most developed technologies today. Augmented reality has the advantage of visualizing objects in 3D form against the object in the marker. The advantages of Augmented Reality can be utilized in education, especially to visualize objects that are difficult to visualize. This study aims to determine the effect of augmented reality-based learning media on learning motivation. This research is quantitative research with an experimental quasi approach. This research was conducted in two classes namely the experimental class, namely the class that was given augmented reality-based learning media, and the control class using conventional methods. Data collection techniques were taken using tests and questionnaires. The population in this study were all students of the educational technology curriculum who took computer basics courses. To determine the results of the hypothesis, the normality test, homogeneity test, and hypothesis testing were carried out.
Influences of Galaxy Interactions on AGN Activity

Abstract Using two volume-limited Main galaxy samples of the Sloan Digital Sky Survey Data Release 7 , we explore influences of galaxy interactions on AGN activity. It is found that in the faint volume-limited sample, paired galaxies have a slightly higher AGN fraction than isolated galaxies, whereas in the luminous volume-limited sample, an opposite trend can be observed. The significance is <1σ. Thus, we do not observe strong evidence that interactions or mergers likely trigger the AGN activity.
The role of cold flows and reservoirs in galaxy formation with strong feedback

We examine gas accretion and subsequent star formation in representative galaxies from the McMaster Unbiased Galaxy Simulations (Stinson et al. 2010). Accreted gas is bimodal with a natural temperature division at $10^5$ K, near the peak of the cooling curve. Cold-mode accretion dominates inflows at early times, creating a peak in total accretion at redshift z=2-4 and declining exponentially below z$\sim$2. Hot-mode accretion peaks near z=1-2 and declines gradually. Hot-mode exceeds cold-mode accretion at z$\sim$1.8 for all four galaxies rather than when the galaxy reaches a characteristic mass. Cold-mode accretion can fuel immediate star formation, while hot-mode accretion preferentially builds a large, hot gas reservoir in the halo. Late-time star formation relies on reservoir gas accreted 2-8 Gyr prior. Thus, the reservoir allows the star formation rate to surpass the current overall gas accretion rate. Stellar feedback cycles gas from the interstellar medium back into the hot reservoir. Stronger feedback results in more gas cycling, gas removal in a galactic outflow and less star formation overall, enabling simulations to match the observed star formation history. For lower mass galaxies in particular, strong feedback can delay the star formation peak to z=1-2 from the accretion peak at z=2-4.
Electronic spin susceptibilities and superconductivity in HgBa 2 CuO 4 +δ from nuclear magnetic resonance

Nuclear magnetic resonance (NMR) experiments on single crystals of HgBa$_{2}$CuO$_{4+\delta}$ are presented that identify two distinct temperature-dependent spin susceptibilities: one is due to a spin component that is temperature-dependent above the critical temperature for superconductivity ($T_{\rm c}$) and reflects pseudogap behavior; the other is Fermi-liquid-like in that it is temperature independent above $T_{\rm c}$ and vanishes rapidly below $T_{\rm c}$. In addition, we demonstrate the existence of a third, hitherto undetected spin susceptibility: it is temperature independent at higher temperatures, vanishes at lower temperatures (below $T_0\neq T_{\rm c}$), and changes sign near optimal doping. This susceptibility either arises from the coupling between the two spin components, or it could be given by a distinct third spin component.
MODELING THE GAMMA-RAY EMISSION IN THE GALACTIC CENTER WITH A FADING COSMIC-RAY ACCELERATOR

Recent HESS observations of the ∼200 pc scale diffuse gamma-ray emission from the central molecular zone (CMZ) suggest the presence of a PeV cosmic-ray accelerator (PeVatron) located in the inner 10 pc region of the Galactic center. Interestingly, the gamma-ray spectrum of the point-like source (HESS J1745-290) in the Galactic center shows a cutoff at ∼10 TeV, implying a cutoff around 100 TeV in the cosmic-ray proton spectrum. Here we propose that the gamma-ray emission from the inner and the outer regions may be explained self-consistently by run-away protons from a single yet fading accelerator. In this model, gamma-rays from the CMZ region are produced by protons injected in the past, while gamma-rays from the inner region are produced by protons injected more recently. We suggest that the blast wave formed in a tidal disruption event (TDE) caused by the supermassive black hole (Sgr A*) could serve as such a fading accelerator. With typical parameters of the TDE blast wave, gamma-ray spectra of both the CMZ region and HESS J1745-290 can be reproduced simultaneously. Meanwhile, we find that the cosmic-ray energy density profile in the CMZ region may also be reproduced in the fading accelerator model when appropriate combinations of the particle injection history and the diffusion coefficient of cosmic rays are adopted.
THE BEAMING STRUCTURES OF JUPITER’S DECAMETRIC COMMON S-BURSTS OBSERVED FROM THE LWA1, NDA, AND URAN2 RADIO TELESCOPES

On 2015 February 21, simultaneous observations of Jupiter's decametric radio emission between 10 and 33 MHz were carried out using three powerful low-frequency radio telescopes: the Long Wavelength Array Station One in the USA, the Nançay Decameter Array in France, and the URAN2 telescope in Ukraine. We measured the lag times of short-bursts (S-bursts) for 105 minutes of data over effective baselines of up to 8460 km by using cross-correlation analysis of the spectrograms from each instrument. Of particular interest is the measurement of the beaming thickness of S-bursts, testing if either flashlight- or beacon-like beaming is emanating from Jupiter. We find that the lag times for all pairs drift slightly as time elapses, in agreement with expectations from the flashlight-like beaming model. This leads to a new constraint of the minimum beaming thickness of 2. ″66. Also, we find that most of the analyzed data abound with S-bursts, whose occurrence probability peaks at 17–18 MHz.
Ligament Alteration in Diabetes Mellitus

Connective tissue ageing is accelerated by the progressive accumulation of advanced glycation end products (AGEs). The formation of AGEs is characteristic for diabetes mellitus (DM) progression and affects only specific proteins with relatively long half-lives. This is the case of fibrillar collagens that are highly susceptible to glycation. While collagen provides a framework for plenty of organs, the local homeostasis of specific tissues is indirectly affected by glycation. Among the many age- and diabetes-related morphological changes affecting human connective tissues, there is concurrently reduced healing capacity, flexibility, and quality among ligaments, tendons, bones, and skin. Although DM provokes a wide range of known clinical disorders, the exact mechanisms of connective tissue alteration are still being investigated. Most of them rely on animal models in order to conclude the patterns of damage. Further research and more well-designed large-cohort studies need to be conducted in order to answer the issue concerning the involvement of ligaments in diabetes-related complications. In the following manuscript, we present the results from experiments discovering specific molecules that are engaged in the degenerative process of connective tissue alteration. This review is intended to provide the report and sum up the investigations described in the literature concerning the topic of ligament alteration in DM, which, even though significantly decreasing the quality of life, do not play a major role in research.
Implications of barrier ephemerality in geogenomic research

Previous population genetic and phylogeographical studies have shown how generation time and dispersal affect population divergence in the presence of a vicariant barrier. More recently, speciation genomic studies have revealed that selection and recombination can be equally impactful. Here, we test how the interaction of these factors shapes the divergence expected in response to an ephemeral barrier and compare these results to empirical literature using the Baja California peninsula as a test case.