Miracle-dz/UniFAR-FTUs huggingface dataset:
Investigation of the Relationship Between the Pod Properties and Quality Values of Some Bean Varieties

It is important to know the quality values of the products in terms of production and consumption of plant-based foods, and at the same time, it brings the examined product to the forefront in terms of production and consumption. For this reason, 11 commercial bean varieties were grown as the first crop in Kahramanmaraş ecological conditions in 2018, and in this study, it was aimed to examine the relationship between the pod characteristics and quality values of 11 commercial bean varieties. In the study, the correlations between bean cultivars' pod setting time, pod length, grain yield per plant, thousand-seed weight, pod ratio per plant, protein ratio, oil ratio and starch ratio, as well as all correlations between investigated characteristics were also investigated. It was determined that there were statistically significant (p< 0.01) differences between bean cultivars in terms of pod setting time, pod length, thousand-seed weight, pod ratio and protein content per plant, and significant (p< 0.05) differences in grain yield and oil content per plant. It was noted that there was no significant difference between bean varieties in terms of starch ratio.
EVOLUTION OF DARK MATTER PHASE-SPACE DENSITY DISTRIBUTIONS IN EQUAL-MASS HALO MERGERS

We use dissipationless N-body simulations to investigate the evolution of the true coarse-grained phase-space density distribution f(x, v) in equal-mass mergers between dark matter (DM) halos. The halo models are constructed with various asymptotic power-law indices ρ ∝ r−γ ranging from steep cusps to core-like profiles and we employ the phase-space density estimator “EnBid” developed by Sharma & Steinmetz to compute f(x, v). The adopted force resolution allows robust phase-space density profile estimates in the inner ∼1% of the virial radii of the simulated systems. We confirm that merger events result in a decrease of the coarse-grained phase-space density in accordance with expectations from Mixing Theorems for collisionless systems. We demonstrate that binary mergers between identical DM halos produce remnants that retain excellent memories of the inner slopes and overall shapes of the phase-space density distribution of their progenitors. The robustness of the phase-space density profiles holds for a range of orbital energies, and a variety of encounter configurations including sequences of several consecutive merger events, designed to mimic hierarchical merging, and collisions occurring at different cosmological epochs. If the progenitor halos are constructed with appreciably different asymptotic power-law indices, we find that the inner slope and overall shape of the phase-space density distribution of the remnant are substantially closer to that of the initial system with the steepest central density cusp. These results explicitly demonstrate that mixing is incomplete in equal-mass mergers between DM halos, as it does not erase memory of the progenitor properties. Our results also confirm the recent analytical predictions of Dehnen regarding the preservation of merging self-gravitating central density cusps.
Protostellar collapse and fragmentation using an MHD gadget

Although the influence of magnetic fields is regarded as vital in the star formation process, only a few magnetohydrodynamics (MHD) simulations have been performed on this subject within the smoothed particle hydrodynamics method. This is largely due to the unsatisfactory treatment of non-vanishing divergence of the magnetic field. Recently smoothed particle magnetohydrodynamics (SPMHD) simulations based on Euler potentials have proven to be successful in treating MHD collapse and fragmentation problems, however these methods are known to have some intrinsic difficulties. We have performed SPMHD simulations based on a traditional approach evolving the magnetic field itself using the induction equation. To account for the numerical divergence, we have chosen an approach that subtracts the effects of numerical divergence from the force equation, and additionally we employ artificial magnetic dissipation as a regularization scheme. We apply this realization of SPMHD to a widely known setup, a variation of the ‘Boss and Bodenheimer standard isothermal test case’, to study the impact of the magnetic fields on collapse and fragmentation. In our simulations, we concentrate on setups, where the initial magnetic field is parallel to the rotation axis. We examine different field strengths and compare our results to other findings reported in the literature. We are able to confirm specific results found elsewhere, namely the delayed onset of star formation for strong fields, accompanied by the tendency to form only single stars. We also find that the ‘magnetic cushioning effect’, where the magnetic field is wound up to form a ‘cushion’ between the binary, aids binary fragmentation in a case where previously only formation of a single protostar was expected.
Data Curation and Quality Evaluation for Machine Learning-Based Cyber Intrusion Detection

Intrusion detection is an essential task for protecting the cyber environment from attacks. Many studies have proposed sophisticated models to detect intrusions from a large amount of data, yet they ignored the fact that poor data quality has a direct impact on the performance of intrusion detection systems. Examples of poor data quality include mislabeled, inaccurate, incomprehensive, irrelevant, inconsistent, duplicated, and overlapped data. In order to investigate how data quality may affect machine learning performance, we conducted a series of experiments on 11 host-based intrusion datasets using eight machine learning (ML) models and two pre-trained language models BERT and GPT-2. The experimental results showed: 1. BERT and GPT-2 outperformed the other models on every dataset. 2. Data duplications and overlaps in a dataset had different performance impacts on the pre-trained models and the classic ML models. The pre-trained models were less susceptible to duplicate and overlapped data than the classic ML models. 3. Removing overlaps and duplicates from training data with a normal range of sequence similarities could improve the pre-trained models’ performances on most datasets. However, it may have adverse effects on model performance in datasets with highly similar sequences. 4. The reliability of model evaluation could be affected when testing data contains duplicates. 5. The overlapped rate between the normal class and the intrusion class seemed to have an inverse relationship to the performance of the pre-trained models in intrusion detection. Given the results, we proposed a framework for model selection and data quality assurance for building a high-quality machine learning-based intrusion detection system.
THE STELLAR HALOS OF MASSIVE ELLIPTICAL GALAXIES

We use the Mitchell Spectrograph (formerly VIRUS-P) on the McDonald Observatory 2.7 m Harlan J. Smith Telescope to search for the chemical signatures of massive elliptical galaxy assembly. The Mitchell Spectrograph is an integral-field spectrograph with a uniquely wide field of view (107″ × 107″), allowing us to achieve remarkably high signal-to-noise ratios of ∼20–70 pixel−1 in radial bins of 2–2.5 times the effective radii of the eight galaxies in our sample. Focusing on a sample of massive elliptical galaxies with stellar velocity dispersions σ* > 150 km s−1, we study the radial dependence in the equivalent widths (EW) of key metal absorption lines. By twice the effective radius, the Mgb EWs have dropped by ∼50%, and only a weak correlation between σ* and Mgb EW remains. The Mgb EWs at large radii are comparable to those seen in the centers of elliptical galaxies that are ∼ an order of magnitude less massive. We find that the well-known metallicity gradients often observed within an effective radius continue smoothly to 2.5 Re, while the abundance ratio gradients remain flat. Much like the halo of the Milky Way, the stellar halos of our galaxies have low metallicities and high α-abundance ratios, as expected for very old stars formed in small stellar systems. Our observations support a picture in which the outer parts of massive elliptical galaxies are built by the accretion of much smaller systems whose star formation history was truncated at early times.
The Parallel-Repeated Magic Square Game is Rigid

We show that the $n$-round parallel repetition of the Magic Square game of Mermin and Peres is rigid, in the sense that for any entangled strategy succeeding with probability $1 -\varepsilon$, the players' shared state is $O(\mathrm{poly}(n\varepsilon))$-close to $2n$ EPR pairs under a local isometry. Furthermore, we show that, under local isometry, the players' measurements in said entangled strategy must be $O(\mathrm{poly}(n\varepsilon))$ close to the "ideal" strategy when acting on the shared state.
The first high precision differential abundance analysis of Extremely Metal Poor stars

Context: Studies of extremely metal-poor stars indicate that chemical abundance ratios [X/Fe] have an rms scatter as low as 0.05 dex (12 \%). It remains unclear whether this reflects observational uncertainties or intrinsic astrophysical scatter arising from physical conditions in the ISM at early times. Aims: Measure differential chemical abundance ratios in extremely metal-poor stars to investigate the limits of precision and to understand whether cosmic scatter or observational errors are dominant. Methods: We used high resolution (R $\sim 95,000$) and high S/N (S/N $= 700$ at 5000$\AA$) HIRES/Keck spectra, to determine high precision differential abundances between two extremely metal-poor stars through a line-by-line differential approach. We determined stellar parameters for the star G64-37 with respect to the standard star G64-12. We performed EW measurements for the two stars for the lines recognized in both stars and performed spectral synthesis to study the carbon abundances. Results: The differential approach allowed us to obtain errors of $\sigma$(T$_{eff}$ ) $=$ 27 K, $\sigma$(log $g$) $=$ 0.06 dex, $\sigma$([Fe/H]) $=$ 0.02 dex and $\sigma$(v$_{t}$ ) $=$ 0.06 kms$^{-1}$. We estimated relative chemical abundances with a precision as low as $\sigma$([X/Fe]) $\approx$ 0.01 dex. The small uncertainties demonstrate that there are genuine abundance differences larger than the measurement errors. The observed Li difference can not be explained by the difference in mass, because the less massive star has more Li. Conclusions: It is possible to achieve an abundance precision around $\approx$ 0.01-0.05 dex for extremely metal-poor stars, opening new windows on the study of the early chemical evolution of the Galaxy.
THE SPATIAL CLUSTERING OF ROSAT ALL-SKY SURVEY ACTIVE GALACTIC NUCLEI. IV. MORE MASSIVE BLACK HOLES RESIDE IN MORE MASSIVE DARK MATTER HALOS

This is the fourth paper in a series that reports on our investigation of the clustering properties of active galactic nuclei (AGNs) identified in the ROSAT All-Sky Survey and Sloan Digital Sky Survey (SDSS). In this paper we investigate the cause of the X-ray luminosity dependence of the clustering of broad-line, luminous AGNs at 0.16 < z < 0.36 . > We fit the Hα line profile in the SDSS spectra for all X-ray and optically selected broad-line AGNs, determine the mass of the supermassive black hole (SMBH), M BH , ? > and infer the accretion rate relative to Eddington ( L / L EDD ? > ). Since M BH ? > and L / L EDD ? > are correlated, we create AGN subsamples in one parameter while maintaining the same distribution in the other parameter. In both the X-ray and optically selected AGN samples, we detect a weak clustering dependence with M BH ? > and no statistically significant dependence on L / L EDD . > We find a difference of up to 2. 7σ when comparing the objects that belong to the 30% least and 30% most massive M BH ? > subsamples, in that luminous broad-line AGNs with more massive black holes reside in more massive parent dark matter halos at these redshifts. These results provide evidence that higher accretion rates in AGNs do not necessarily require dense galaxy environments, in which more galaxy mergers and interactions are expected to channel large amounts of gas onto the SMBH. We also present semianalytic models that predict a positive M DMH ? > dependence on M BH , ? > which is most prominent at M BH ∼ 10 8 − 9 M ⊙ . >
Dynamical boundary for anti–de Sitter space

We argue that a natural boundary condition for gravity in asymptotically AdS spaces is to hold the {\em renormalized} boundary stress tensor density fixed, instead of the boundary metric. This leads to a well-defined variational problem, as well as new counter-terms and a finite on-shell action. We elaborate this in various (even and odd) dimensions in the language of holographic renormalization. Even though the {\em form} of the new renormalized action is distinct from the standard one, once the cut-off is taken to infinity, their {\em values} on classical solutions coincide when the trace anomaly vanishes. For AdS$_4$, we compute the ADM form of this renormalized action and show in detail how the correct thermodynamics of Kerr-AdS black holes emerge. We comment on the possibility of a consistent quantization with our boundary conditions when the boundary is dynamical, and make a connection to the results of Compere and Marolf. The difference between our approach and microcanonical-like ensembles in standard AdS/CFT is emphasized.
Conserved charges in 3D gravity

The covariant canonical expression for the conserved charges, proposed by Nester, is tested on several solutions in three-dimensional gravity with or without torsion and topologically massive gravity. In each of these cases, the calculated values of energy momentum and angular momentum are found to satisfy the first law of black hole thermodynamics.
Few-Mode Fiber Technology, Deployments, and Systems

Mode-division multiplexing (MDM) using few-mode fibers (FMFs) appears as a promising technology to increase fiber capacity by a few orders of magnitude and sustain the traffic demand for the decades to come. The potential of MDM lies in its ability to exploit multiple modes within a single optical fiber strand. Since 2011 and the first promising demonstrations, impressive progress has been made. In this article, we will show how the most recent advances in design and fabrication have improved the performance of FMFs and MDM systems, and allowed to turn research demonstrations into practical deployments.
Relation of Photosynthetic Rates to Yield in Sweet Potato Genotypes1

Significant differences were observed in yield, net photosynthetic rates (Pn), percent leaf nitrogen, chlorophyll content, stomatal density and specific leaf weight in various genotypes of sweet potato (Ipomoea batatas (L.) Lam. ) but these characters were not correlated with root yield.
Electromagnetic hiss and relativistic electron losses in the inner zone. [of magnetosphere]

Broad band incoherent electromagnetic waves, called hiss, have been detected in the inner zone magnetosphere (L 10−6 γ²/Hz at the start of storm recovery phases, 10−7 – 10−6 γ²/Hz during substorms, and 0.4 to >3.1 MeV from L = 2 to L = 1.1, respectively. Characteristic lifetimes of inner zone electrons, calculated in order of magnitude fashion on the basis of pitch angle diffusion into the loss cone driven by the cyclotron resonant interaction, are found to range between 10 and 60 days. These computed lifetimes are consistent with observations of enhanced electron precipitation for L > 1.25 during storms. Although Coulomb scattering appears to be the dominant loss mechanism for L < 1.25, pitch angles scattering by the hiss may make a significant contribution to electron losses, especially during magnetically active intervals. The source of inner zone hiss has also been investigated. Two possible mechanisms of locally generating hiss in the inner zone, an electron cyclotron instability and a Landau resonance, are studied but are found to be unlikely candidates to give rise to hiss. Most features of inner zone hiss can be explained by the hypothesis that hiss originates in the vicinity of the plasmapause as plasmaspheric hiss, which is then able to propagate into the inner zone. There are two major effects that will allow this to occur during storms and substorms. The first is the intensification of plasmaspheric hiss as the freshly injected electrons convect and drift across the plasmapause into the high-density plasmasphere, leading to cyclotron instability. The second is the displacement of the plasmapause, and the presumed source region, to low L values during strong magnetic activity. This reduces the length of the ray paths leading to the inner zone and hence the amount of Landau damping. The present observations are compared with this propagation model and the two are found to be in good agreement.
SPITZER MID-INFRARED SPECTROSCOPY OF COMPACT SYMMETRIC OBJECTS: WHAT POWERS RADIO-LOUD ACTIVE GALACTIC NUCLEI?

We present low- and high-resolution mid-infrared (mid-IR) spectra and photometry for eight compact symmetric objects (CSOs) taken with the Infrared Spectrograph on the Spitzer Space Telescope. The hosts of these young, powerful radio galaxies show significant diversity in their mid-IR spectra. This includes multiple atomic fine-structure lines, H2 gas, polycyclic aromatic hydrocarbon (PAH) emission, warm dust from T = 50to150 K, and silicate features in both emission and absorption. There is no evidence in the mid-IR of a single template for CSO hosts, but 5/8 galaxies show similar moderate levels of star formation (<10 M☉ yr−1 from PAH emission) and silicate dust in a clumpy torus. The total amount of extinction ranges from AV ∼ 10to30, and the high-ionization [Ne v] 14.3 and 24.3 μm transitions are not detected for any galaxy in the sample. Almost all CSOs show contributions both from star formation and active galactic nuclei (AGNs), suggesting that they occupy a continuum between pure starbursts and AGNs. This is consistent with the hypothesis that radio galaxies are created following a galactic merger; the timing of the radio activity onset means that contributions to the IR luminosity from both merger-induced star formation and the central AGN are likely. Bondi accretion is capable of powering the radio jets for almost all CSOs in the sample; the lack of [Ne v] emission suggests an advection-dominated accretion flow mode as a possible candidate. Merging black holes (BHs) with MBH > 108 M☉ likely exist in all of the CSOs in the sample; however, there is no direct evidence from these data that BH spin energy is being tapped as an alternative mode for powering the radio jets.
THE COMPOSITIONAL DIVERSITY OF EXTRASOLAR TERRESTRIAL PLANETS. I. IN SITU SIMULATIONS

Extrasolar planet host stars have been found to be enriched in key planet-building elements. These enrichments have the potential to drastically alter the composition of material available for terrestrial planet formation. Here, we report on the combination of dynamical models of late-stage terrestrial planet formation within known extrasolar planetary systems with chemical equilibrium models of the composition of solid material within the disk. This allows us to determine the bulk elemental composition of simulated extrasolar terrestrial planets. A wide variety of resulting planetary compositions are found, ranging from those that are essentially “Earth like,” containing metallic Fe and Mg silicates, to those that are dominated by graphite and SiC. This shows that a diverse range of terrestrial planets may exist within extrasolar planetary systems.
Knowledge of Carcinoma Cervix among rural women of Reproductive age in Trichy district, India

Introduction and objectives: Cervical cancer is one of the leading causes of morbidity and mortality worldwide. It is imperative for women to be aware about the disease and its prevention. So this study was carried out to assess the knowledge of cervical cancer among women in rural areas of Trichy District. Materials and methods: Community Based- Cross sectional study was conducted in the months of February and March 2016 in the rural areas of Vellanur and Pullambadi with a sample size of 300. Only Reproductive age group women (15 years-45 years) were included. Convenient sampling method was used. Data were entered in Microsoft Excel and Analysed by using SPSS v20. Results: Out of the 300 women studied, 89% had heard about cervical cancer, of which only 12.73% had good knowledge on cervical cancer. Knowledge regarding symptoms, risk factors, cause, preventability, availability of screening tests and vaccines were 11.61%, 19.48%, 30.71%, 41.95%, 60.30% and 9.36% respectively. A significant association was found between knowledge of cervical cancer with younger age and with higher education. Conclusion: Knowledge among women in the study area was found to be low. To reduce the incidence of cervical cancer, awareness regarding the disease has to be created among the public.
Accelerated Transition Between Dry and Wet Periods in a Warming Climate

The consecutive occurrence of meteorological dry and wet extremes has been receiving increasing attention due to potentially larger social and environmental impacts than single extremes. However, the changing characteristics of transitions between dry and wet periods remain poorly understood. Here we investigate the dynamic evolution of dry‐to‐wet transitions in response to climate warming, using the Standardized Precipitation Evapotranspiration Index as well as observations and general circulation models for the periods of 1954–2014 and 2040–2100. We find that approximately three‐fifths of global land area are projected to experience an accelerated dry‐to‐wet transition. Southern Asia has been experiencing the most severe dry‐to‐wet transitions and is projected to suffer more frequent, more intense, and accelerated dry‐to‐wet transitions. The increasing potential evapotranspiration (PET) variability plays an important role in accelerating the dry‐to‐wet transition in Southern Asia, while precipitation and PET variabilities contribute to the intensification of dry‐to‐wet transitions in Southern North America.