Miracle-dz/UniFAR-FTUs huggingface dataset:
Effect of two levels of olive leaf and doum powder and their mixture in female rats suffering from acute nephritis using CCL4

37 Abstract Olive leaves and doum are two of several herbal medicines that are used either as food or adrink.This study was designed to explore the potential protective effect of doum, olive leaves and a mixture of them using percentages (4% and 8%) during infecting female rats With acute kidney injury using carbon tetrachloride with paraffin oil ( v/v 1ml/kg of body weight) three-time/week for 4 weeks, where the duration of the experiment was 5 weeks, one week of them was to rehabilitate the rat. The rats weighing an average of (190±10) forty of rats were divided into eight groups (n=5 rats). G 1 was fed on the basal diet and kept as a negative control group.The other 7 groups were injectedintraperitoneally with CCL 4 and paraffin oil( v/v) 1ml/kg of body weight)three time/week for 4 weeksto induce acute damage in the kidney.G2 was fed on a basal diet and left as a positive control group and group (3 and 4),(5 and 6) and (7 and 8) were fed on supplemented diet with( 4% and 8%) olive leaves,doum and mixture of them,respectively.The obtained results revealed that the treating groups with olive leaves,doum and a mixture of them had significantly reduced serum levels of (lipid profile, except HDL-c ) andkidney functions,liver enzymes, while these treatments induced no significant in feed intake (FI),body weight gain(BWG),feed efficiency ratio (FER) and a significant increase in serum levels of HDL-c,glutathioneperoxidase(GPX),superoxide dismutase (SOD) and catalase (CAT) enzymes ,as well as partially improvements in kidneys structures compared to those of positive control group.The best improvements in all the biochemical parameters and histological structures of the liver and kidneys which were tended toward normal results were observed in protective groups(7&8).
Sleep Quality as a Predictor for Academic Performance in Menoufia University Medical Students

Background: Poor sleep quality is an important public health problem with multiple unfavourable consequences. Sleep disorders are widespread among university students and have a significant impact on their general health and academic performance. Aim: To investigate the relationship between sleep quality and academic performance among medical students in Menoufia University. Participants and methods: This cross-sectional study was carried out from 1 st November 2021 to the end of March 2022 on 1033 undergraduate medical students from Menoufia University in Egypt. The data were collected using self-administered questionnaire to obtain information regarding sociodemographic variables, academic achievement in the previous year, sleep habits and environmental sleep factors like smoking, exercise and media use. The Pittsburgh Sleep Quality Index (PSQI) was used to assess sleep quality. Results: The mean overall score of the PSQI was 18.03 (SD ± 7.59); the majority of students (96.5%) had bad sleep quality with PSQI score greater than 5. There was a highly significant difference between good and bad academic performance regarding Pittsburgh sleep quality score. Mean sleep duration was 6.67 (SD ± 2.05) hours. Most of participants were non-smokers (91.9%), physically not active (50.6%), and use the internet for more than two hours daily (55.8%). Conclusion: Poor sleep is a major problem for Egyptian medical students, and there was also a significant relationship between sleep quality and academic performance.
EXPLAINING THE OBSERVED VELOCITY DISPERSION OF DWARF GALAXIES BY BARYONIC MASS LOSS DURING THE FIRST COLLAPSE

In the widely adopted Λ cold dark matter (ΛCDM) scenario for galaxy formation, dwarf galaxies are the building blocks of larger galaxies. Since they formed at relatively early epochs when the background density was relatively high, they are expected to retain their integrity as satellite galaxies when they merge to form larger entities. Although many dwarf spheroidal galaxies are found in the galactic halo around the Milky Way, their phase-space density (or velocity dispersion) appears to be significantly smaller than that expected for satellite dwarf galaxies in the ΛCDM scenario. In order to account for this discrepancy, we consider the possibility that they may have lost a significant fraction of their baryonic matter content during the first infall at the Hubble expansion turnaround. Such mass loss arises naturally due to the feedback by relatively massive stars that formed in their centers briefly before the maximum contraction. Through a series of N-body simulations, we show that the timely loss of a significant fraction of the dSphs initial baryonic matter content can have profound effects on their asymptotic half-mass radius, velocity dispersion, phase-space density, and the mass fraction between residual baryonic and dark matter.
Exact black hole solutions in shift symmetric scalar–tensor theories

We derive a variety of exact black hole solutions in a subclass of Horndeski's scalar-tensor theory possessing shift symmetry, phi -> phi + c and reflection symmetry, phi -> -phi The theory admits two arbitrary functions of X := -(partial derivative phi)(2)/2, and our solutions are constructed without specifying the concrete form of the two functions, implying that black hole solutions in specific scalar-tensor theories found in the literature can be extended to a more general class of theories with shift symmetry. Our solutions include a black hole in the presence of an effective cosmological constant, the Nariai spacetime, the Lifshitz black hole, and other nontrivial solutions, all of which exhibit nonconstant scalar-field profiles.
THE 1.6 μm NEAR-INFRARED NUCLEI OF 3C RADIO GALAXIES: JETS, THERMAL EMISSION, OR SCATTERED LIGHT?

Using HST NICMOS 2 observations we have measured 1.6 μm near-infrared nuclear luminosities of 100 3CR radio galaxies with z < 0.3, by modeling and subtracting the extended emission from the host galaxy. We performed a multiwavelength statistical analysis (including optical and radio data) of the properties of the nuclei following classification of the objects into FR I and FR II, and low-ionization galaxies (LIGs), high-ionization galaxies (HIGs), and broad-line objects (BLOs) using the radio morphology and optical spectra, respectively. The correlations among near-infrared, optical, and radio nuclear luminosity support the idea that the near-infrared nuclear emission of FR Is has a non-thermal origin. Despite the difference in radio morphology, the multiwavelength properties of FR II LIG nuclei are statistically indistinguishable from those of FR Is, an indication of a common structure of the central engine. All BLOs show an unresolved near-infrared nucleus and a large near-infrared excess with respect to FR II LIGs and FR Is of equal radio core luminosity. This requires the presence of an additional (and dominant) component other than the non-thermal light. Considering the shape of their spectral energy distribution, we ascribe the origin of their near-infrared light to hot circumnuclear dust. A near-infrared excess is also found in HIGs, but their nuclei are substantially fainter than those of BLO. This result indicates that substantial obscuration along the line of sight to the nuclei is still present at 1.6 μm. Nonetheless, HIG nuclei cannot simply be explained in terms of dust obscuration: a significant contribution from light reflected in a circumnuclear scattering region is needed to account for their multiwavelength properties.
Study of the decays B->D_s1(2536)+ anti-D(*)

T. Aushev, I. Adachi, K. Arinstein, 36 V. Aulchenko, 36 A. M. Bakich, V. Balagura, V. Bhardwaj, M. Bischofberger, A. Bondar, 36 A. Bozek, M. Bračko, T. E. Browder, M. -C. Chang, A. Chen, P. Chen, B. G. Cheon, R. Chistov, I. -S. Cho, K. Cho, K. -S. Choi, Y. Choi, J. Dalseno, 45 M. Danilov, A. Drutskoy, S. Eidelman, 36 D. Epifanov, 36 V. Gaur, N. Gabyshev, 36 A. Garmash, 36 B. Golob, 16 H. Ha, K. Hayasaka, H. Hayashii, Y. Horii, Y. Hoshi, W. -S. Hou, H. J. Hyun, T. Iijima, K. Inami, A. Ishikawa, R. Itoh, M. Iwabuchi, Y. Iwasaki, T. Iwashita, T. Julius, J. H. Kang, T. Kawasaki, H. J. Kim, H. O. Kim, J. H. Kim, M. J. Kim, Y. J. Kim, K. Kinoshita, B. R. Ko, P. Kodyš, P. Križan, 16 T. Kuhr, T. Kumita, A. Kuzmin, 36 Y. -J. Kwon, S. -H. Kyeong, J. S. Lange, S. -H. Lee, J. Li, C. Liu, Y. Liu, D. Liventsev, R. Louvot, A. Matyja, S. McOnie, K. Miyabayashi, H. Miyata, Y. Miyazaki, R. Mizuk, G. B. Mohanty, M. Nakao, H. Nakazawa, Z. Natkaniec, S. Neubauer, S. Nishida, O. Nitoh, S. Ogawa, T. Ohshima, S. L. Olsen, 9 W. Ostrowicz, P. Pakhlov, G. Pakhlova, H. K. Park, R. Pestotnik, M. Petrič, L. E. Piilonen, A. Poluektov, 36 K. Prothmann, 45 M. Röhrken, S. Ryu, H. Sahoo, K. Sakai, Y. Sakai, O. Schneider, C. Schwanda, K. Senyo, O. Seon, M. E. Sevior, M. Shapkin, V. Shebalin, 36 C. P. Shen, J.-G. Shiu, B. Shwartz, 36 F. Simon, 45 J. B. Singh, P. Smerkol, Y. -S. Sohn, A. Sokolov, E. Solovieva, S. Stanič, M. Starič, M. Sumihama, 6 T. Sumiyoshi, S. Tanaka, Y. Teramoto, I. Tikhomirov, K. Trabelsi, M. Uchida, 49 T. Uglov, S. Uno, Y. Usov, 36 S. E. Vahsen, G. Varner, K. Vervink, A. Vinokurova, 36 A. Vossen, C. H. Wang, M. -Z. Wang, P. Wang, Y. Watanabe, K. M. Williams, B. D. Yabsley, Y. Yamashita, Y. Yusa, Z. P. Zhang, V. Zhilich, 36 P. Zhou, V. Zhulanov, 36 A. Zupanc, and O. Zyukova 36
METHODOLOGICAL NOTES Expressions for the energy density and evolved heat in the electrodynamics of a dispersive and absorptive medium

The question of the expressions for the energy density W and evolved heat (dissipation) Q in the electrodynamics of a dispersive and absorptive medium is discussed. Attention is concentrated on explaining the fact that W and Q are not expressed, generally speaking, in terms of the complex dielectric permittivity e(ω). This statement is illustrated with the example of a medium consisting of a collection of oscillators and with the example of the simplest model of a plasma. A convenient expression for the energy density of a field with arbitrary time dependence in a transparent medium is obtained in the Appendix. A derivation of the high-frequency average of (1/4π)∂D/∂t for a quasi-monochromatic field in an absorptive dispersive medium is also given there.
Journal of Information Security and Applications

With the rapid progress and significant successes in various applications, machine learning has been considered a crucial component in the Internet of Things ecosystem. However, machine learning models have recently been vulnerable to carefully crafted perturbations, so-called adversarial attacks. A capable insider adversary can subvert the machine learning model at either the training or testing phase, causing them to behave differently. The vulnerability of machine learning to adversarial attacks becomes one of the significant risks. Therefore, there is a need to secure machine learning models enabling the safe adoption in malicious insider cases. This paper reviews and organizes the body of knowledge in adversarial attacks and defense presented in IoT literature from an insider adversary point of view. We proposed a taxonomy of adversarial methods against machine learning models that an insider can exploit. Under the taxonomy, we discuss how these methods can be applied in real-life IoT applications. Finally, we explore defensive methods against adversarial attacks. We believe this can draw a comprehensive overview of the scattered research works to raise awareness of the existing insider threats landscape and encourages others to safeguard machine learning models against insider threats in the IoT ecosystem.
Radiative transfer and radiative driving of outflows in active galactic nuclei and starbursts

To facilitate the study of black hole fuelling, star formation and feedback in galaxies, we outline a method for treating the radial forces on interstellar gas due to absorption of photons by dust grains. The method gives the correct behaviour in all of the relevant limits [dominated by the central point source; dominated by the distributed isotropic source; optically thin; optically thick to ultraviolet (UV)/optical; optically thick to infrared (IR)] and reasonably interpolates between the limits when necessary. The method is explicitly energy conserving so that UV/optical photons that are absorbed are not lost, but are rather redistributed to the IR where they may scatter out of the galaxy. We implement the radiative transfer algorithm in a two-dimensional hydrodynamical code designed to study feedback processes in the context of early-type galaxies. We find that the dynamics and final state of simulations are measurably but only moderately affected by radiative forces on dust, even when assumptions about the dust-to-gas ratio are varied from zero to a value appropriate for the Milky Way. In simulations with high gas densities designed to mimic ultraluminous IR galaxies with a star formation rate of several hundred solar masses per year, dust makes a more substantial contribution to the dynamics and outcome of the simulation. We find that, despite the large opacity of dust to UV radiation, the momentum input to the flow from radiation very rarely exceeds L/c due to two factors: the low opacity of dust to the re-radiated IR and the tendency for dust to be destroyed by sputtering in hot gas environments. We also develop a simplification of our radiative transfer algorithm that respects the essential physics but is much easier to implement and requires a fraction of the computational cost.
PHOTOMETRIC AMPLITUDE DISTRIBUTION OF STELLAR ROTATION OF KOIs—INDICATION FOR SPIN–ORBIT ALIGNMENT OF COOL STARS AND HIGH OBLIQUITY FOR HOT STARS

The observed amplitude of the rotational photometric modulation of a star with spots should depend on the inclination of its rotational axis relative to our line of sight. Therefore, the distribution of observed rotational amplitudes of a large sample of stars depends on the distribution of their projected axes of rotation. Thus, comparison of the stellar rotational amplitudes of the Kepler objects of interest (KOIs) with those of Kepler single stars can provide a measure to indirectly infer the properties of the spin–orbit obliquity of Kepler planets. We apply this technique to the large samples of 993 KOIs and 33,614 single Kepler stars in temperature range of 3500–6500 K. We find with high significance that the amplitudes of cool KOIs are larger, on the order of 10%, than those of the single stars. In contrast, the amplitudes of hot KOIs are systematically lower. After correcting for an observational bias, we estimate that the amplitudes of the hot KOIs are smaller than the single stars by about the same factor of 10%. The border line between the relatively larger and smaller amplitudes, relative to the amplitudes of the single stars, occurs at about 6000 K. Our results suggest that the cool stars have their planets aligned with their stellar rotation, while the planets around hot stars have large obliquities, consistent with the findings of Winn et al. and Albrecht et al. We show that the low obliquity of the planets around cool stars extends up to at least 50 days, a feature that is not expected in the framework of a model that assumes the low obliquity is due to planet–star tidal realignment.
IONIZED GAS IN THE GALACTIC CENTER: NEW OBSERVATIONS AND INTERPRETATION

We present new observations of the [Ne ii] emission from the ionized gas in Sgr A West with improved resolution and sensitivity. About half of the emission comes from gas with kinematics indicating it is orbiting in a plane tipped about 25° from the Galactic plane. This plane is consistent with that derived previously for the circumnuclear molecular disk and the northern arm and western arc ionized features. However, unlike most previous studies, we conclude that the ionized gas is not moving along the ionized features, but on more nearly circular paths. The observed speeds are close to, but probably somewhat less than expected for orbital motions in the potential of the central black hole and stars and have a small inward component. The spatial distribution of the emission is well fitted by a spiral pattern. We discuss possible physical explanations for the spatial distribution and kinematics of the ionized gas, and conclude that both may be best explained by a one-armed spiral density wave, which also accounts for both the observed low velocities and the inward velocity component. We suggest that a density wave may result from the precession of elliptical orbits in the potential of the black hole and stellar mass distribution.
Use of Selective Serotonin Reuptake Inhibitors Is Associated with a Lower Risk of Colorectal Cancer among People with Family History

Simple Summary Individuals with a family history of colorectal cancer (CRC) are at a high risk of developing CRC. We performed a nationwide cohort study to explore whether selective serotonin reuptake inhibitors (SSRIs) play a role in preventing CRC among individuals with family history. This report suggests that SSRI use was associated with a reduced incidence of CRC among people with a family history of CRC, and the decreased risk of CRC showed a non-linear, dose-dependent pattern. In addition, we found that the use of SSRIs was strongly associated with CRC diagnosed at an advanced stage rather than at an earlier stage, suggesting that the SSRIs might reduce the metastatic potential of cancer cells leading to stage migration. This population-based cohort study suggests that the use of SSRIs is associated with a reduced risk of CRC among individuals with a family history of CRC. Abstract Individuals with a family history of colorectal cancer (CRC) are at a high risk of developing CRC. Preclinical and population-based evidence suggests that selective serotonin reuptake inhibitors (SSRIs) might play a role in preventing CRC. We performed a nationwide cohort study to explore whether the use of SSRIs could reduce CRC risk among individuals with family history. We identified individuals aged 50 and above who had one or more first-degree relatives diagnosed with CRC. A total of 38,617 incident SSRI users were identified and matched with 115,851 non-users, on a ratio of 1:3. The Cox regression model was used to calculate hazard ratios (HRs) and 95% CI confidence intervals (CIs). We found a significant negative association between SSRI use and the risk of CRC (adjusted HR, 0.77; 95% CI, 0.70–0.85). Restricted cubic spline regression showed a non-linear dose-responded relationship between SSRI use and CRC risk. The association was stronger in rectal cancer than colon cancer (adjusted HR, 0.73 vs. 0.79), and more pronounced in advanced-stage CRC than early-stage CRC (adjusted HR, 0.73 vs. 0.80). This population-based cohort study suggests that the use of SSRIs is associated with a reduced risk of CRC among individuals with a family history of CRC.
A quantification of the non-spherical geometry and accretion of collapsing cores

We present the first detailed classification of the structures of Class 0 cores in a high-resolution simulation of a giant molecular cloud. The simulated cloud contains 104 M⊙ and produces over 350 cores which allows for meaningful statistics. Cores are classified into three types according to how much they depart from spherical symmetry. We find that three-quarters of the cores are better described as irregular filaments than as spheres. Recent Herschel results have shown that cores are formed within a network of filaments, which we find has had a significant impact on the resulting core geometries. We show that the column densities and ram pressure seen by the protostar are not uniform and generally peak along the axes of the filament. The angular momentum vector of the material in the cores varies both in magnitude and direction, which will cause the rotation vector of the central source to fluctuate during the collapse of the core. In the case of the more massive stars, accretion from the environment outside the original core volume is even more important than that from the core itself. This additional gas is primarily accreted on to the cores along the dense filaments in which the cores are embedded, and the sections of the surfaces of the cores which do not coincide with a filament have very little additional material passing through them. The assumption of spherical symmetry cannot be applied to the majority of collapsing cores, and is never a good description of how stars accrete gas from outside the original core radius. This has ramifications for our understanding of collapsing cores, in particular their line profiles, the effect of radiation upon them and their ability to fragment.
ON THE BINARY FREQUENCY OF THE LOWEST MASS MEMBERS OF THE PLEIADES WITH HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3

We present the results of a Hubble Space Telescope Wide Field Camera 3 (WFC3) imaging survey of 11 of the lowest mass brown dwarfs in the Pleiades known (25–40 MJup). These objects represent the predecessors to T dwarfs in the field. Using a semi-empirical binary point-spread function (PSF)-fitting technique, we are able to probe to 0. ″ 03 (0.75 pixel), better than 2x the WFC3/UVIS diffraction limit. We did not find any companions to our targets. From extensive testing of our PSF-fitting method on simulated binaries, we compute detection limits which rule out companions to our targets with mass ratios of ≳0.7 and separations ≳4 AU. Thus, our survey is the first to attain the high angular resolution needed to resolve brown dwarf binaries in the Pleiades at separations that are most common in the field population. We constrain the binary frequency over this range of separation and mass ratio of 25–40 MJup Pleiades brown dwarfs to be <11% for 1σ (<26% at 2σ). This binary frequency is consistent with both younger and older brown dwarfs in this mass range.