Miracle-dz/UniFAR-FTUs huggingface dataset:
Recognizing Edge-Based Diseases of Vocal Cords by Using Convolutional Neural Networks

During clinical consultations and case training, doctors analyze numerous images and sounds. A high-pressure consultation environment can increase the probability of a doctor making incorrect inferences regarding vocal cord (VC) disease. Therefore, this study applied deep learning to design an edge-based VC disease detection system (EVC-DD) for common VC conditions (e.g., nodules, polyps, and cancer) to assist doctors in conducting consultations and case studies and in verifying the consistency of their disease inferences. Through deep learning, the model extracted and recorded clinically confirmed information in its disease inference model. The experiment data set comprised videos of nodules, polyps, and cancer that were used to evaluate the performance of the proposed model. From 13 cases confirmed by two doctors, 1740 images were extracted from 13 case videos and used in the experiment. In total, 1044 (60%), 348 (20%), and 348 (20%) images were randomly obtained through five-fold cross-validation for training, validation, and testing, respectively. During the model training process, the EVC-DD model achieved 100% accuracy in detecting the three conditions required for optimal experiment results. For the results in the analysis of the independent test data with optimized configuration. the EVC-DD model achieved 99.42%, 99.42%, 99.42%, 99.42%, 98.91%, and 0.9957 for averaged F1 score, averaged recall rate, averaged precision, accuracy, Matthews correlation coefficient, and area under the curve, respectively. The EVC-DD model required only 400 s to complete its training using 1740 images. The results indicate that the inferences of the EVC-DD model were highly consistent with the results of the clinical examination by doctors and that its training was data- and time-efficient, thereby allowing the model to learn new cases quickly. Thus, the EVC-DD model can assist doctors in consultations and case analyses by providing reliable disease inferences and real-time input regarding new case knowledge.
DISCOVERY AND EVOLUTION OF THE NEW BLACK HOLE CANDIDATE SWIFT J1539.2−6227 DURING ITS 2008 OUTBURST

We report on the discovery by the Swift Gamma-Ray Burst Explorer of the black hole (BH) candidate Swift J1539.2−6227 and the subsequent course of an outburst beginning in 2008 November and lasting at least seven months. The source was discovered during normal observations with the Swift Burst Alert Telescope on 2008 November 25. An extended observing campaign with the Rossi X-Ray Timing Explorer and Swift provided near-daily coverage over 176 days, giving us a good opportunity to track the evolution of spectral and timing parameters with fine temporal resolution through a series of spectral states. The source was first detected in a hard state during which strong low-frequency quasi-periodic oscillations (QPOs) were detected. The QPOs persisted for about 35 days and a signature of the transition from the hard- to soft-intermediate states was seen in the timing data. The source entered a short-lived thermal state about 40 days after the start of the outburst. There were variations in spectral hardness as the source flux declined and returned to a hard state at the end of the outburst. The progression of spectral states and the nature of the timing features provide strong evidence that Swift J1539.2−6227 is a candidate BH in a low-mass X-ray binary system.
Model for nodal quasiparticle scattering in a disordered vortex lattice

Recent scanning tunneling experiments on $Ca_{2-x}Na_xCuO_2Cl_2$ by Hanaguri et al. observe field-dependent quasiparticle interference effects which are sensitive to the sign of the d-wave order parameter. Their analysis of spatial fluctuations in the local density of states shows that there is a selective enhancement of quasiparticle scattering events that preserve the gap sign, and a selective depression of the quasiparticle scattering events that reverse the gap sign. We introduce a model which accounts for this phenomenon as a consequence of vortex pinning to impurities. Each pinned vortex embeds several impurities in its core. The observations of recent experiments can be accounted for by assuming that the scattering potentials of the impurities inside the vortex cores acquire an additional resonant or Andreev scattering component, both of which induce gap sign preserving scattering events.
Gas Content and Kinematics in Clumpy, Turbulent Star-forming Disks

We present molecular gas-mass estimates for a sample of 13 local galaxies whose kinematic and star-forming properties closely resemble those observed in z ≈ 1.5 main-sequence galaxies. Plateau de Bure observations of the CO[1-0] emission line and Herschel Space Observatory observations of the dust emission both suggest molecular gas-mass fractions of ∼20%. Moreover, dust emission modeling finds Tdust < 30 K, suggesting a cold dust distribution compared to their high infrared luminosity. The gas-mass estimates argue that z ∼ 0.1 DYNAMO galaxies not only share similar kinematic properties with high-z disks, but they are also similarly rich in molecular material. Pairing the gas-mass fractions with existing kinematics reveals a linear relationship between fgas and σ/vc, consistent with predictions from stability theory of a self-gravitating disk. It thus follows that high gas-velocity dispersions are a natural consequence of large gas fractions. We also find that the systems with the lowest tdep (∼0.5 Gyr) have the highest ratios of σ/vc and more pronounced clumps, even at the same high molecular gas fraction.
IMPLICATIONS FOR THE BLAZAR SEQUENCE AND INVERSE COMPTON MODELS FROM FERMI BRIGHT BLAZARS

In this paper, we use the quasi-simultaneous spectra of Fermi bright blazars and Fermi-detected narrow-line Seyfert 1 (NLS1) to study the blazar sequence and inverse Compton models. (1) The synchrotron peak luminosities (Ls) significantly correlate inversely with the synchrotron peak frequencies (νs), Ls∝ν−0.44 ± 0.11s, which is consistent with the blazar sequence. In addition to the correlation, there are some blazars showing low νs and low Ls. To study the relation between these low-νs–low-Ls blazars and the blazar sequence, we present correlations of the parameter Lsν1/4s with the ratio of Compton to synchrotron peak frequencies (rCs ≡ νC/νs) and with the ratio of Compton to synchrotron luminosities (CD ≡ LC/Ls). The results indicate that both correlations are significant with a Pearson's probability for a null correlation of p = 0.0218 and p = 0.0286, respectively. This does not support the idea that the low-νs–low-Ls blazars are sources with less beaming. Another possibility, as suggested by Ghisellini & Tavecchio, is that these blazars have relatively lower black hole masses. To test this, we collect the black hole masses of 30 blazars from archives and find that the black hole mass correlates with the parameter Lsν0.44s (p = 0.0344). Therefore, the black hole masses of low-νs–low-Ls blazars are statistically small. The NLS1s are thought to have lower black hole masses. We find that the four NLS1s detected by Fermi have low νs and low Ls. This supports the above result. (2) The ratio rCs correlates with CD significantly (p = 0.00375). The external Compton model can naturally explain this correlation, while the synchrotron self-Compton model cannot. This agrees with the findings of many authors that the EC process dominates the gamma-ray emission of flat spectrum radio quasars.
SUBMILLIMETER H2O MEGAMASERS IN NGC 4945 AND THE CIRCINUS GALAXY

We present 321 GHz observations of five active galactic nuclei (AGNs) from ALMA Cycle 0 archival data: NGC 5793, NGC 1068, NGC 1386, NGC 4945, and the Circinus galaxy. Submillimeter maser emission is detected for the first time toward NGC 4945, and we present a new analysis of the submillimeter maser system in Circinus. None of the other three galaxies show maser emission, although we have detected and imaged the continuum from every galaxy. Both NGC 4945 and Circinus are known to host strong (≳10 Jy) 22 GHz megamaser emission, and VLBI observations have shown that the masers reside in the innermost ∼1 pc of the galaxies. The peak flux densities of the 321 GHz masers in both systems are substantially weaker (by a factor of ∼100) than what is observed at 22 GHz, although the corresponding isotropic luminosities are more closely matched (within a factor of ∼10) between the two transitions. We compare the submillimeter spectra presented here to the known 22 GHz spectra in both galaxies, and we argue that while both transitions originate from the gaseous environment near the AGNs, not all sites are in common. In Circinus, the spectral structure of the 321 GHz masers indicates that they may trace the accretion disk at radii interior to the 22 GHz masers. The continuum emission in NGC 4945 and NGC 5793 shows a spatial distribution indicative of an origin in the galactic disks (likely thermal dust emission), while for the other three galaxies the emission is centrally concentrated and likely originates from the nucleus.
On time dilation in quasar light curves

In this paper we set out to measure time dilation in quasar light curves. In order to detect the effects of time dilation, sets of light curves from two monitoring programmes are used to construct Fourier power spectra covering time-scales from 50 d to 28 yr. Data from high- and low-redshift samples are compared to look for the changes expected from time dilation. The main result of the paper is that quasar light curves do not show the effects of time dilation. Several explanations are discussed, including the possibility that time dilation effects are exactly offset by an increase in time-scale of variation associated with black hole growth, or that the variations are caused by microlensing in which case time dilation would not be expected.
The occurrence of antibiotic resistance Vibrio isolates from brackish water shrimp ponds in the coastal area in Thua Thien Hue, Vietnam

The indiscriminate and improper use of antibiotics in shrimp farming can have a number of negative consequences, including the development of drug-resistant bacteria that render disease prevention and treatment ineffective, negatively impact the user’s health, and alter the natural microflora. In addition, exporting and consuming farmed shrimp items that have antibiotic residues will be also prohibited. The aim of this study was to detect antibiotic-resistant Vibrio species in extensive white leg shrimp farming systems in Thua Thien Hue, Vietnam. Microbial culture techniques were utilized to isolate Vibrio , determine antibiotic resistance, and estimate the minimal bacterial inhibitory concentration. The species of Vibrio were identified using 16S rRNA sequencing, and a phylogenetic tree was constructed using the maximum likelihood estimation with a bootstrap of 1000 replications. The results showed the supply brackish water consisted of 10 2.5 –10 3.8 CFU/mL of Vibrio . After 3 months of cultivation, the Vibrio concentration in white leg shrimp ponds increased rapidly, reaching 10 4 –10 6.6 CFU/mL. Antibiotic susceptibility testing demonstrated the antibiotic resistance of Vibrio present in supply brackish water. Vibrio bacteria in shrimp ponds were resistant to gentamicin, kanamycin, streptomycin, oxytetracycline hydrochloride, and doxycycline, up to 98.87% of the antibiotics tested, ciprofloxacin was the most potent inhibitor of Vibrio . MIC evaluation of ciprofloxacin-resistant Vibrio isolates showed that they were resistant to many other antibiotics. This discovery demonstrates the need for using the optimum antibiotics in white leg shrimp farming to prevent the dissemination of antibiotic-resistant Vibrio bacteria.
Extinction law in the range 0.4 - 4.8 μm and the 8620 Å DIB towards the stellar cluster Westerlund 1

The young stellar cluster Westerlund 1 (Wd 1: $l$=339.6$^\circ$, b=$-$0.4$^\circ$) is one of the most massive in the local Universe, but accurate parameters are pending on better determination of its extinction and distance. Based on our photometry and data collected from other sources, we have derived a reddening law for the cluster line-of-sight representative of the Galactic Plane (-5$^\circ $ 4).
X-Ray Eclipses of Active Galactic Nuclei

X-ray variation is a ubiquitous feature of active galactic nuclei (AGNs); however, its origin is not well understood. In this paper, we show that the X-ray flux variations in some AGNs, and correspondingly, the power spectral densities (PSDs) of the variations, may be interpreted as being caused by absorptions of eclipsing clouds or clumps in the broad-line region (BLR) and the dusty torus. By performing Monte Carlo simulations for a number of plausible cloud models, we systematically investigate the statistics of the X-ray variations resulting from the cloud eclipsing and the PSDs of the variations. For these models, we show that the number of eclipsing events can be significant and the absorption column densities due to those eclipsing clouds can be in the range from 1021 to , leading to significant X-ray variations. We find that the PSDs obtained from the mock observations for the X-ray flux and the absorption column density resulting from these models can be described by a broken double power law, similar to those directly measured from observations of some AGNs. The shape of the PSDs depend strongly on the kinematic structures and the intrinsic properties of the clouds in AGNs. We demonstrate that the X-ray eclipsing model can naturally lead to a strong correlation between the break frequencies (and correspondingly the break timescales) of the PSDs and the masses of the massive black holes (MBHs) in the model AGNs, which can be well consistent with the one obtained from observations. Future studies of the PSDs of the AGN X-ray (and possibly also the optical-UV) flux and column density variations may provide a powerful tool to constrain the structure of the BLR and the torus and to estimate the MBH masses in AGNs.
New and revised parameters for several southern OB binaries

Using ESO FEROS archive spectra of several southern OB-type binaries, we derived periods for three SB2 spectroscopic binaries, HD 97166, HD 115455, and HD 123590, and two SB1 systems, HD 130298 and HD 163892. It was also possible to use new FEROS spectra to improve the parameters of the known binaries, KX Vel and HD 167263. For KX Vel, we determined a dynamic mass of the primary of 16.8 M� , while the evolutionary model suggests a higher value of 20.2 M� . We derived an improved period for HD 167263, and in its spectra, we recognized contributions of both of its interferometric components.
Comparison of approximate gravitational lens equations and a proposal for an improved new one

Keeping the exact general relativistic treatment of light bending as a reference, we compare the accuracy of commonly used approximate lens equations. We conclude that the best approximate lens equation is the Ohanian lens equation, for which we present a new expression in terms of distances between observer, lens, and source planes. We also examine a realistic gravitational lensing case, showing that the precision of the Ohanian lens equation might be required for a reliable treatment of gravitational lensing and a correct extraction of the full information about gravitational physics.
HOW BRIGHT ARE THE GAPS IN CIRCUMBINARY DISK SYSTEMS?

When a circumbinary disk surrounds a binary whose secondary’s mass is at least the primary’s mass, a nearly empty cavity with radius a few times the binary separation is carved out of the disk. Narrow streams of material pass from the inner edge of the circumbinary disk into the domain of the binary itself, where they eventually join onto the small disks orbiting the members of the binary. Using data from three-dimensional magnetohydrodynamics simulations of this process, we determine the luminosity of these streams; it is mostly due to weak laminar shocks, and is in general only a few percent of the luminosity of adjacent regions of either the circumbinary disk or the “mini-disks. ” This luminosity therefore hardly affects the deficit in the thermal continuum predicted on the basis of a perfectly dark gap region.
Chronic Ulcerative Stomatitis (CUS) as an Interdisciplinary Diagnostic Challenge: A Literature Review

Chronic ulcerative stomatitis (CUS) is a rarely reported disease affecting the oral cavity, most often affecting middle-aged Caucasian females. The aim of the present study is to present the diagnosis, differentiation, and interdisciplinary treatment of this rare disease. CUS is characterized by the presence of an oral erosive or ulcerative lesion. The autoimmune pathogenesis of CUS includes affecting the antigen’s activity by DNA-breaking and protein-hydrolyzing enzymes. The stratified epithelium-specific antinuclear antibodies (SES-ANA) are associated with CUS development. Clinically, the lesions presented in oral mucosa might resemble an erosive form of oral lichen planus, whereas gingival lesions seem to be similar to desquamative gingivitis related to dermatological diseases manifested in the oral cavity. Patients often report subjective symptoms related to oral mucosa and general symptoms. Histopathological presentation of CUS is often non-specific and includes sub-epithelial separation from underlying connective tissue, atrophic epithelium, and inflammatory infiltrate with an increased number of plasma cells and lymphocytes. Direct immunofluorescence (DIF) might be used in CUS diagnostics. CUS generally remains nonsusceptible to corticosteroid treatments; however, antimalarial drugs and calcineurin inhibitors are more effective. Further research should be conducted in order to implement a diagnostic protocol and observe the long-term results of CUS management.
Nutritional and Therapeutic Properties of Fermented Camel Milk Fortified with Red Chenopodium quinoa Flour on Hypercholesterolemia Rats

Quinoa is a nutrient-dense food that lowers chronic disease risk. This study evaluated the physicochemical and sensory qualities of fermented camel milk with 1, 2, 3, and 4% quinoa. The results showed that improvement in camel’s milk increased the total solids, protein, ash, fiber, phenolic content, and antioxidant activity more effectively. Fermented camel milk with 3% of quinoa flour exhibited the highest sensory characteristics compared to other treatments. Fermented camel milk enriched with 3% red quinoa flour was studied in obese rats. Forty male Wistar rats were separated into five groups: the first group served as a normal control, while groups 2–4 were fed a high-fat, high-cholesterol (HF)-diet and given 2 mL/day of fermented milk and quinoa aqueous extract. Blood glucose, malondialdehyde (MDA), low-density lipoprotein (LDL), cholesterol, triglyceride, aspartate transaminase (AST), alanine transaminase (ALT), alkaline phosphatase (ALP), creatinine, and urea levels decreased dramatically in comparison to the positive control group, while high-density lipoprotein (HDL), albumin, and total protein concentrations increased significantly. Fortified fermented camel milk decreased the number of giant adipocytes while increasing the number of tiny adipocytes in the body. The results showed that the liver and renal functions of hypercholesterolemic rats were enhanced by consuming fermented milk and quinoa. These results demonstrated the ability of quinoa and camel milk to protect rats from oxidative stress and hyperlipidemia. Further studies are needed to clarify the mechanisms behind the metabolic effects of fermented camel milk and quinoa.
Vortex motion around a circular cylinder

The motion of a pair of counter-rotating point vortices placed in a uniform flow around a circular cylinder forms a rich nonlinear system that is often used to model vortex shedding. The phase portrait of the Hamiltonian governing the dynamics of a vortex pair that moves symmetrically with respect to the centerline---a case that can be realized experimentally by placing a splitter plate in the center plane---is presented. The analysis provides new insights and reveals novel dynamical features of the system, such as a nilpotent saddle point at infinity whose homoclinic orbits define the region of nonlinear stability of the so-called F\"oppl equilibrium. It is pointed out that a vortex pair properly placed downstream can overcome the cylinder and move off to infinity upstream. In addition, the nonlinear dynamics resulting from antisymmetric perturbations of the F\"oppl equilibrium is studied and its relevance to vortex shedding discussed.
Gravitational potential wells and the cosmic bulk flow

The bulk flow is a volume average of the peculiar velocities and a useful probe of the mass distribution on large scales. The gravitational instability model views the bulk flow as a potential flow that obeys a Maxwellian Distribution. We use two N-body simulations, the LasDamas Carmen and the Horizon Run, to calculate the bulk flows of various sized volumes in the simulation boxes. Once we have the bulk flow velocities as a function of scale, we investigate the mass and gravitational potential distribution around the volume. We found that matter densities can be asymmetrical and difficult to detect in real surveys, however, the gravitational potential and its gradient may provide better tools to investigate the underlying matter distribution. This study shows that bulk flows are indeed potential flows and thus provides information on the flow sources. We also show that bulk flow magnitudes follow a Maxwellian distribution on scales $>10\ h^{-1}$Mpc.
PHYSICAL CONDITIONS IN THE X-RAY EMISSION-LINE GAS IN NGC 1068

We present a detailed, photoionization modeling analysis of XMM-Newton/Reflection Grating Spectrometer observations of the Seyfert 2 galaxy NGC 1068. The spectrum, previously analyzed by Kinkhabwala et al., reveals a myriad of soft X-ray emission lines, including those from H- and He-like carbon, nitrogen, oxygen, and neon, and M- and L-shell iron. As noted in the earlier analysis, based on the narrowness of the radiative recombination continua, the electron temperatures in the emission-line gas are consistent with photoionization, rather than collisional ionization. The strengths of the carbon and nitrogen emission lines, relative to those of oxygen, suggest unusual elemental abundances, which we attribute to the star formation history of the host galaxy. Overall, the emission lines are blueshifted with respect to systemic, with radial velocities ∼160 km s−1, similar to that of [O iii] λ5007, and thus consistent with the kinematics and orientation of the optical emission-line gas and, hence, likely part of an active galactic nucleus driven outflow. We were able to achieve an acceptable fit to most of the strong emission lines with a two-component photoionization model, generated with cloudy. The two components have ionization parameters and column densities of logU = −0.05 and 1.22 and logNH = 20.85 and 21.2 and covering factors of 0.35 and 0.84, respectively. The total mass of the X-ray gas is roughly an order of magnitude greater than the mass of ionized gas determined from optical and near-IR spectroscopy, which indicates that it may be the dominant component of the narrow-line region. Furthermore, we suggest that the medium that produces the scattered/polarized optical emission in NGC 1068 possesses similar physical characteristics to those of the more highly ionized of the X-ray model components.