Miracle-dz/UniFAR-FTUs huggingface dataset:
AN R- AND I-BAND PHOTOMETRIC VARIABILITY SURVEY OF THE CYGNUS OB2 ASSOCIATION

We present a catalog of photometrically variable stars discovered within two 21. ′3 × 21. ′3 fields centered on the Cygnus OB2 association (Cyg OB2). There have hitherto been no deep optical variability studies of Cyg OB2, despite it being replete with early-type massive stars, likely due to the high and variable extinction (up to AV ≈ 20) that permeates much of the region. Here, we provide results of the first variability study with this combination of spatial coverage (∼0.5 deg) and photometric depth (R ∼ 21 mag). We find 121 stars to be variable in both R and I bands, 115 of them newly discovered. Of the 121 variables, we identify 27 eclipsing binaries and eclipsing-binary candidates, 52 pulsating variables, and 20 potential Herbig Ae/Be stars. Confirming both the status and the cluster membership of the Herbig Ae/Be stars would address the uncertainty regarding the age and star formation history of Cyg OB2. We match our catalog to known variables and binaries in the region, Two Micron All Sky Survey near-IR data, and Chandra X-ray observations to find counterparts to new variables in other wavelengths.
Stabilisation of stochastic complex-valued time-varying coupled systems with jump diffusion via aperiodically intermittent control

This paper considers the stabilisation of stochastic complex-valued time-varying coupled systems with jump diffusion by aperiodically intermittent control (AIC). In addition, as a special case of AIC, impulsive control is also used to achieve stabilisation. It is worth mentioning that the coupling strength of coupled systems is time-varying, which increases the difficulty of the research. In addition, the jump diffusion is taken into account in stochastic complex-valued coupled systems, which generalises the existing results about jump diffusion previously since the real-valued cases are mostly considered before. Based on the graph theory and the Lyapunov method, some stability criteria are given, and the sufficient conditions reflect that the realisation of stability is closely related to the strength of stochastic disturbance, coupling strength and uncontrolled rate. Then, our results are applied to stochastic complex-valued coupled oscillators models with time-varying coupling structure. Ultimately, two numerical examples are given to verify the effectiveness of the theoretical results.
Use of Thyme and Thymol as Immunostimulant Agents to control Experimental ‎Aeromonas hydrophyla Infection in Nile Tilapia (Oreochromis niloticus)‎

In the current investigation, a total of 110 Oreochromis niloticus were collected from aquaculture farm at Sahl Eltina area, North Sinai Governorate suffering from skin and fin ulcers with ascites, exophthalmia, and high mortalities. Aeromonas hydrophyla was isolated with a prevalence rate of 40% and identified biochemically. A . hydrophyla was used to induce experimental infection to Nile Tilapia in which thyme and thymol were used as feed additive. Evaluation of the protective effect of thyme and thymol as immunostimulant agents on fish tissue against experimental infection with Aeromonas infection was studied. A total of ninety apparently healthy fish tilapia were divided into three groups (GA, GB and GC of 30 fish per group) in triplicate. GA (infected non treated group) was fed on basal diet. GB and GC were fed on diet supplemented with Thyme vulgaris (10 g/ kg diet) and Thymol (3 g/ kg diet), respectively for 8 weeks and then the groups were subjected to experimental infection with Aeromonas hydrophyla isolate. The thyme and thymol groups had a nearly similar significant immunostimulant effect than infected non treated group by using lysozyme activity assay. Sever hyperemia of gill filaments and gill arch, epithelial desquamation of the gill filament, enteritis, necrosis and desquamation of epithelial cells of intestine, muscle necrosis, myocardiolysis of heart, hydropic degeneration of liver and hemosiderosis of spleen were observed in infected non treated group. In the treated groups, the prophylactic effect of thyme and thymol on fish tissues were clear against experimental infection with A. hydrophyla . These results indicate that the using thyme or thymol as feed additive could enhance the immunity and protect fish tissues from pathological deterioration induced by infection with Aeromonas hydrophila which is considered as one the main fish pathogens in Egypt.
DISCOVERY OF A SPIN-DOWN STATE CHANGE IN THE LMC PULSAR B0540-69

We report the discovery of a large, sudden, and persistent increase in the spin-down rate of B0540-69, a young pulsar in the Large Magellanic Cloud, using observations from the Swift and RXTE satellites. The relative increase in the spin-down rate &ngr; ˙ ? > of 36% is unprecedented for B0540-69. No accompanying change in the spin rate is seen, and no change is seen in the pulsed X-ray emission from B0540-69 following the change in the spin-down rate. Such large relative changes in the spin-down rate are seen in the recently discovered class of “intermittent pulsars,” and we compare the properties of B0540-69 to such pulsars. We consider possible changes in the magnetosphere of the pulsar that could cause such a large change in the spin-down rate.
Exploring the link between spectral variance and upper canopy taxonomic diversity in a tropical forest: influence of spectral processing and feature selection

The rapid loss of biodiversity in tropical rainforests calls for new remote sensing approaches capable of providing rapid estimates of biodiversity over large areas. Imaging spectroscopy has shown potential for the estimation of taxonomic diversity, but the link with spectral diversity has not been investigated extensively with experimental data so far. We explored the relationship between taxonomic diversity and visible to near infrared spectral variance derived from various spectral processing techniques by means of a labeled dataset comprising 2000 individual tree crowns from 200 species from an experimental tropical forest station in French Guiana. We generated a set of artificially assembled communities covering a broad range of taxonomic diversity from this experimental dataset. We analyzed the impact of various processing steps: spectral normalization, spectral transformation through principal component analysis, and feature selection. Correlation between taxonomic diversity and inter‐specific spectral variance was strong. Correlation was lower with total spectral variance, with or without normalization and transformation. Dimensionality reduction through feature selection resulted in dramatic improvement of the correlation between Shannon index and spectral variance. While airborne diversity mapping of tropical forest may not be at hand yet, our results confirm that spectral diversity metrics, when computed on properly preprocessed and selected spectral information can predict taxonomic diversity in tropical ecosystems.
INFLUENCE OF INTELLECTUAL CAPITAL ON COMPANY PERFORMANCE

Insights into the intellectual capital (IC) on financial performance is relatively a modern phenomenon, attracts the interest of global researchers. Though famous in the banking and communication sectors, little evidence finds in Real Estate and the Consumer Service Sectors. This study focuses to assess the relationship between IC and financial performance (FP) of 46 Real Estate and Consumer Service PLCs listed in Colombo Stock Exchange, Sri Lanka, during 2015 - 2018. The Value-Added Intellectual Capital (VAIC) model with its three primary components is represented by secondary data from annual reports of companies on IC. The FP was represented by Return on Assets and Return on Equity. The findings indicated that VAIC has a positive relationship with FP of the above 46 PLCs, indicating that CEE and FP have a significant positive effect. Recommends, more investments in IC associated activities, ensuring better performance where moderate and weak relationships exist.
Relief of frustration in the Heisenberg pyrochlore antiferromagnet Gd 2 Pt 2 O 7

The gadolinium pyrochlores, Gd$_2B_2$O$_7$, are amongst the best realizations of antiferromagnetically coupled Heisenberg spins on a pyrochlore lattice. We present a magnetic characterization of Gd$_2$Pt$_2$O$_7$, a unique member of this family. Magnetic susceptibility, heat capacity, and muon spin relaxation measurements show that Gd$_2$Pt$_2$O$_7$ undergoes an antiferromagnetic ordering transition at $T_N = 1.6$ K. This transition is strongly first order, as indicated by the sharpness of the heat capacity anomaly, thermal hysteresis in the magnetic susceptibility, and a non-divergent relaxation rate in $\mu$SR. The form of the heat capacity below $T_N$ suggests that the ground state is an anisotropic collinear antiferromagnet with an excitation spectrum that is gapped by 0.245(1) meV. The ordering temperature in Gd$_2$Pt$_2$O$_7$, $T_N = 1.6$ K, is a substantial 160% increase from other gadolinium pyrochlores, which have been found to order at 1 K or lower. We attribute this enhancement in $T_N$ to the $B$-site cation, platinum, which, despite being non-magnetic, has a filled $5d$ $t_{2g}$ orbital and an empty $5d$ $e_g$ orbital that can facilitate superexchange. Thus, the magnetic frustration in Gd$_2$Pt$_2$O$_7$ is partially "relieved", thereby promoting magnetic order.
Results of Pulmonary Artery Debanding: Simple Band Removal Versus Pulmonary Artery Repair with Pericardial Patch

Background: Among the complications noted after debanding is those related to residual pulmonary stenosis. Removal of band without repairing pulmonary artery could be enough. Others recommend patching pulmonary artery at the site of band during debanding because of possibility of residual gradient caused by a residual shelf or narrowing and distortion of the arterial wall. This may necessitate re-operation especially if it leads to pressure over-load on the right ventricle. Objective: To compare between simple band removal and band removal with pulmonary artery repair using pericardial patch, at time of debanding; concerning early postoperative pressure gradients across the main pulmonary artery. Patients and methods: This retrospective observational study included 40 patients who underwent pulmonary artery debanding in the period between January 2016 and January 2020 at the Cardiothoracic Surgery Department, Cairo University hospitals and Atfal Masr Hospital. Patients were divided into two groups; group A, which included 20 patients who underwent simple band removal and group B, which included 20 patients who underwent pulmonary artery debanding with pericardial patch repair. Results: The median pressure gradient across the main pulmonary artery postoperatively was 15 mm Hg for group A (mean 22.58±18.0) and 10 mm Hg for group B (mean 11.3±8.0) with statistically significant value (p=0.020). 40.0% of cases in Group A had significant residual pressure gradient compared to only 10.0% of cases in Group B, and that difference was statistically significant (p=0.028). The median pressure gradient across the band immediate preoperatively was 60mmHg for group A (mean 62.0±9.8) and 70mmHg (mean 64.2±10.6) with statistically insignificant value (p=0.065). Conclusion: Pulmonary artery repair with pericardial patch showed the advantage of reducing the risk of significant residual pressure gradient across the band site over simple band removal in pulmonary artery debanding.
Water in the interstellar media of galaxies

Abstract This paper reviews recent observations of water in Galactic interstellar clouds and nearby galactic nuclei. Two results are highlighted: (1) Multi-line H2O mapping of the Orion Bar shows that the water chemistry in PDRs is driven by photodissociation and -desorption, unlike in star-forming regions. (2) High-resolution spectra of H2O and its ions toward 5 starburst / AGN systems reveal low ionization rates, unlike as found from higher-excitation lines. We conclude that the chemistry of water strongly depends on radiation environment, and that the ionization rates of interstellar clouds decrease by at least 10 between galactic nuclei and disks.
Predictors of Endoscopy Success in Treatment of Pediatric Idiopathic Obstructive Hydrocephalus

Background: Hydrocephalus is defined as an inappropriate increased pressure of cerebrospinal fluid (CSF) within the intracranial spaces with an inappropriate amount of CSF. Endoscopic third ventriculostomy (ETV) is considered an effective procedure that is safe. Purpose : The aim of the current work was to detect the factors those predict success parameters in selecting patients with idiopathic obstructive hydrocephalus as candidates for the ETV procedure at a pediatric age. Patients and methods: A clinical prospective cohort study was conducted at Benha University Hospitals from September 2018 to July 2021. A total of 61 patients with inclusion criteria of idiopathic (congenital) obstructive hydrocephalus of pediatric age (under 18 years old) with and without previous ventriculoperitoneal (VP) shunt insertion were included according to calculated sample size who undergoing ETV with a follow-up period of 6-12 months. All patients were evaluated by pre and post-operative operative MRI CSF flowmetry. Results : Sixty-one patients were operated on, with age ranged from 3 to 120 months, and the median (IQR) was 13.0 (5.5-24). Previous VP shunting was done in 15 patients (24.6%). According to the receiving operator characteristic (ROC) curve, the cut off point for ETV success age was 11.5 months; while the cut off point for ETV success score (ETVSS) was 70. MRI CSF flowmetry detected and measured the size of the ventriculostomy stoma and evaluated the flow direction and stroke volume. Conclusions : It could be concluded that endoscopy has reliable validity and safety in the treatment of idiopathic obstructive hydrocephalus. ETV success predictors are patients’ age above 11.5 months and ETVSS ≥70, led to increase validity of endoscopy. MRI CSF flowmetry is safe and accurate method for evaluation of the ventriculostomy stoma.
THE Hα LUMINOSITY FUNCTION AND STAR FORMATION RATE VOLUME DENSITY AT z = 0.8 FROM THE NEWFIRM Hα SURVEY

We present new measurements of the Hα luminosity function (LF) and star formation rate (SFR) volume density for galaxies at z ∼ 0.8. Our analysis is based on 1.18 μm narrowband data from the NEWFIRM Hα (NewHα) Survey, a comprehensive program designed to capture deep samples of intermediate redshift emission-line galaxies using narrowband imaging in the near-infrared. The combination of depth (≈1.9 × 10−17 erg s−1 cm−2 in Hα at 3σ) and areal coverage (0.82 deg2) of the 1.18 μm observations complements other recent Hα studies at similar redshifts, and enables us to minimize the impact of cosmic variance and place robust constraints on the shape of the LF. The present sample contains 818 NB118 excess objects, 394 of which are selected as Hα emitters. Optical spectroscopy has been obtained for 62% of the NB118 excess objects. Empirical optical broadband color classification is used to sort the remainder of the sample. A comparison of the LFs constructed for the four individual fields covered by the observations reveals significant cosmic variance, emphasizing that multiple, widely separated observations are required for such analyses. The dust-corrected LF is well described by a Schechter function with L⋆ = 1043.00±0.52 erg s−1, Φ⋆ = 10−3.20±0.54 Mpc−3, and α = −1.6 ± 0.19. We compare our Hα LF and SFR density to those at z ≲ 1, and find a rise in the SFR density ∝(1 + z)3.4, which we attribute to significant L⋆ evolution. Our Hα SFR density of 10−1.00±0.18 M☉ yr−1 Mpc−3 is consistent with UV and [O ii] measurements at z ∼ 1. We discuss how these results compare to other Hα surveys at z ∼ 0.8, and find that the different methods used to determine survey completeness can lead to inconsistent results. This suggests that future surveys probing fainter luminosities are needed, and more rigorous methods of estimating the completeness should be adopted as standard procedure (for example, with simulations which try to simultaneously reproduce the observed Hα LF and equivalent width distributions).
STAR FORMATION IN DISK GALAXIES. II. THE EFFECT OF STAR FORMATION AND PHOTOELECTRIC HEATING ON THE FORMATION AND EVOLUTION OF GIANT MOLECULAR CLOUDS

We investigate the effect of star formation and diffuse photoelectric heating on the properties of giant molecular clouds (GMCs) formed in high-resolution (≲10 pc) global (∼20 kpc) simulations of isolated Milky-Way-type galaxy disks. The clouds are formed through gravitational fragmentation, and structures with densities nH,c>100 cm−3 are identified as GMCs. Between 1000 and 1500 clouds are created in the simulations with masses M>105 M☉ and 180–240 with masses M>106 M☉ in agreement with estimates of the Milky Way's population. We find that the effect of photoelectric heating is to suppress the fragmentation of the interstellar medium, resulting in a filamentary structure in the warm gas surrounding clouds. This environment suppresses the formation of a retrograde rotating cloud population, with 88% of the clouds rotating prograde with respect to the galaxy after 300 Myr. The diffuse heating also reduces the initial star formation rate (SFR), slowing the conversation of gas into stars. We therefore conclude that the interstellar environment plays an important role in the GMC evolution. Our clouds live between 0 and 20 Myr with a high infant mortality (t′ < 3 Myr) due to cloud mergers and star formation. Other properties, including distributions of mass, size, and surface density, agree well with observations. Collisions between our clouds are common, occurring at a rate of ∼ 1/4 of the orbital period. It is not clear whether such collisions trigger or suppress star formation at our current resolution. Our SFR is a factor of 10 higher than observations in local galaxies. This is likely due to the absence of localized feedback in our models.
Diophantine approximation by orbits of Markov maps

In 1995, Hill and Velani introduced the shrinking targets theory. Given a dynamical system $([0,1],T)$, they investigated the Hausdorff dimension of sets of points whose orbits are close to some fixed point. In this paper, we study the sets of points well-approximated by orbits $\{T^n x\}_{n\geq 0}$, where $T$ is an expanding Markov map with a finite partition supported by $[0,1]$. The dimensions of these sets are described using the multifractal properties of invariant Gibbs measures.
An assessment and correlation of emotional Intelligence and mental health of medical students

Introduction: Emotions like joy, anger, grief, jealousy, love, fear make our life worthwhile. Whatever we do, incites some emotion in us. If we are able to enjoy our emotions, without them having excessive control over us, then we can make ours as well as others’ lives better. Aim of the study was to assess and correlate emotional Intelligence with mental health. Methods: Type of study: Descriptive type of cross sectional study. Sampling: Simple random sampling. Study population: Under graduate students in a private medical college in western Uttar Pradesh. Study duration: 1/07/2019 to 1/09/2019. Sample size: 246. Results: The average emotional intelligence score was 26.82 with standard deviation of ±5.80. Average emotional intelligence among males was 27.04(±6.72) and was 26.63(±5.07) among females. Spearman Rank correlation coefficient “r” =0.789, showed highly positive correlation between ranks from both the score. (p=0.0000). Conclusions: The medical students showing higher scores of emotional intelligence are less likely to be mentally stressed.
Pulsations of rapidly rotating stars: II. Realistic modelling for intermediate-mass stars

Very high precision seismic space missions such as CoRoT and Kepler provide the means for testing the modelling of transport processes in stellar interiors. For some stars, such as $\delta$ Scuti $\gamma$ Doradus and Be stars, for instance, the observed pulsation spectra are modified by rotation to such an extent that it prevents any fruitful interpretation. Our aim is to characterise acoustic pulsation spectra of realistic stellar models in order to be able to interpret asteroseismic data from such stars. The 2-dimensional oscillation code ACOR, which treats rotation in a non-perturbative manner, is used to study pulsation spectra of highly distorted evolved models of stars. 2D models of stars are obtained by a self-consistent method which distorts spherically averaged stellar models a posteriori, at any stage of evolution, and for any type of rotation law. Four types of modes are calculated in a very dense frequency spectrum, among which are island modes. The regularity of the island modes spectrum is confirmed and yields a new set of quantum numbers, with which an \'echelle diagram can be built. Mixed gravito-acoustic modes are calculated in rapidly rotating models for the first time.
PRECISE BLACK HOLE MASSES FROM MEGAMASER DISKS: BLACK HOLE–BULGE RELATIONS AT LOW MASS

The black hole (BH)–bulge correlations have greatly influenced the last decade of efforts to understand galaxy evolution. Current knowledge of these correlations is limited predominantly to high BH masses (MBH≳108 M☉) that can be measured using direct stellar, gas, and maser kinematics. These objects, however, do not represent the demographics of more typical L < L* galaxies. This study transcends prior limitations to probe BHs that are an order of magnitude lower in mass, using BH mass measurements derived from the dynamics of H2O megamasers in circumnuclear disks. The masers trace the Keplerian rotation of circumnuclear molecular disks starting at radii of a few tenths of a pc from the central BH. Modeling of the rotation curves, presented by Kuo et al., yields BH masses with exquisite precision. We present stellar velocity dispersion measurements for a sample of nine megamaser disk galaxies based on long-slit observations using the B&C spectrograph on the Dupont telescope and the Dual Imaging Spectrograph on the 3.5 m telescope at Apache Point. We also perform bulge-to-disk decomposition of a subset of five of these galaxies with Sloan Digital Sky Survey imaging. The maser galaxies as a group fall below the MBH–σ* relation defined by elliptical galaxies. We show, now with very precise BH mass measurements, that the low-scatter power-law relation between MBH and σ* seen in elliptical galaxies is not universal. The elliptical galaxy MBH–σ* relation cannot be used to derive the BH mass function at low mass or the zero point for active BH masses. The processes (perhaps BH self-regulation or minor merging) that operate at higher mass have not effectively established an MBH–σ* relation in this low-mass regime.
Coalescence of Growing Bubbles in Highly Viscous Liquids

Bubble coalescence in ascending magma is a key process that controls the eruption violence and the texture of volcanic pyroclasts. In the present study, we performed in situ experiments to investigate the coalescence of two growing bubbles in highly viscous liquids (102 and 1,020 Pa ⋅ s). A new experimental apparatus enables us to directly observe the drainage of the film between growing bubbles in three dimensions. We combined the experimental results and a simple scaling analysis to reveal the dynamics of film drainage in terms of a capillary number Ca=ηṘ/σ $Ca=\eta \dot{R}/\sigma $ depending on the liquid viscosity η, the bubble growth rate Ṙ $\dot{R}$ , and the surface tension σ. The capillary number represents the interplay between the viscous force arising from bubble growth and the capillary force. At Ca ≪ 1, two adjacent bubbles retain their spherical shapes until the film ruptures, and the capillary forces control the drainage timescale. In contrast, at Ca ≫ 1, bubbles largely flatten and bubble growth itself drives film drainage. We also provide a general formula for the drainage timescale over a wide range of capillary numbers (10−3 < Ca < 101). Our results highlight the importance of bubble growth in the coalescence process. The variations of bubble shape and number density during decompression can be explained by the capillary number.