Miracle-dz/UniFAR-FTUs huggingface dataset:
Growth hormone gene polymorphism in Jaisalmeri and Sindhi camels

The present study was aimed to assess the genetic polymorphism of growth hormone (GH) gene in Jaisalmeri and Sindhi camels using polymerase chain reactionâ€“restriction fragment length polymorphism (PCR-RFLP) technique. Genomic DNA were isolated from venous blood samples collected from 93 Indian camels (Jaisalmeri- 38 and Sindhi-55 camels) and 613-base pair fragment of GH gene was amplified from each genomic DNA sample by polymerase chain reaction. The PCR-RFLP was done using restriction enzyme MspI which revealed three genotypes, viz. CC, CT and TT in both the breeds. Our result indicated that both the breeds were polymorphic in nature. The corresponding genotype frequency in Jaisalmeri and Sindhi breeds were 0.474 and 0.345 for the CC, 0.395 and 0.564 for CT, 0.131 and 0.091 for TT genotypes and the corresponding C allele frequency was 0.671 and 0.627 and T allele frequency was 0.329 and 0.373. The CT genotype was found predominant in the Sindhi breed, whereas CC genotype was predominant in Jaisalmeri breed. The frequency of C allele was higher than the T allele in both of the breeds. These camel populations were in Hardy-Weinberg Equilibrium indicating that the populations meet the HWE assumptions and genetic variations were conserved. It could be concluded that Jaisalmeri and Sindhi camels having different genetic variants of GH gene might be investigated for production a DNA marker for growth and production traits in Indian camels.
Multivariate analysis as a tool in the initial selections of golden flax (Linum usitatissimum L.)

The genetic variability in plant populations can be estimated through multivariate analysis, which allows to analyze the genotypes based on a set of traits to identify the traits with the greatest influence for the divergence and the correlation between them. In this sense, the objective of the present work was to estimate the genetic divergence between golden flax lines using multivariate analysis for initial plant selections. For this purpose, 73 lines, in addition to the control, were tested in a randomized complete block design, with three replications, and traits of cycle, stature, and yield were measured. Twelve groups were obtained based on the Mahalanobis distance estimate and Tocher cluster, and the technical length was the most important trait for the dissimilarity. The line of group XI was promising, with early maturation and satisfactory seed productivity. The graphic of dispersion of the canonical variables showed the most divergent lines, and the greatest divergence was observed between groups III and IV. Multivariate analysis was an important tool for the initial choice of superior golden flax.
Impacts of dark energy on weighing neutrinos after Planck 2015

We investigate how dark energy properties impact the cosmological limits on the total mass of active neutrinos. We consider two typical, simple dark energy models (that have only one more additional parameter than $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$), i.e., the $w\mathrm{CDM}$ model and the holographic dark energy (HDE) model, as examples, to make an analysis. In the cosmological fits, we use the Planck 2015 temperature and polarization data, in combination with other low-redshift observations, including the baryon acoustic oscillations, type Ia supernovae, and Hubble constant measurement, as well as the Planck lensing measurements. We find that, once dynamical dark energy is considered, the degeneracy between $\ensuremath{\sum}{m}_{\ensuremath{\nu}}$ and ${H}_{0}$ will be changed, i.e., in the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ model, $\ensuremath{\sum}{m}_{\ensuremath{\nu}}$ is anticorrelated with ${H}_{0}$, but in the $w\mathrm{CDM}$ and HDE models, $\ensuremath{\sum}{m}_{\ensuremath{\nu}}$ becomes positively correlated with ${H}_{0}$. Compared to $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$, in the $w\mathrm{CDM}$ model the limit on $\ensuremath{\sum}{m}_{\ensuremath{\nu}}$ becomes much looser, but in the HDE model the limit becomes much tighter. In the HDE model, we obtain $\ensuremath{\sum}{m}_{\ensuremath{\nu}}l0.113\text{ }\text{ }\mathrm{eV}$ (95% C.L.) with the combined data sets, which is perhaps the most stringent upper limit by far on neutrino mass. Thus, our result in the HDE model is nearly ready to diagnose the neutrino mass hierarchy with the current cosmological observations.
Phase diagram and conformal string excitations of square ice using gauge invariant matrix product states

We investigate the ground state phase diagram of square ice — a U(1) lattice gauge theory in two spatial dimensions — using gauge invariant tensor network techniques. By correlation function, Wilson loop, and entanglement diagnostics, we characterize its phases and the transitions between them, finding good agreement with previous studies. We study the entanglement properties of string excitations on top of the ground state, and provide direct evidence of the fact that the latter are described by a conformal field theory. Our results pave the way to the application of tensor network methods to confining, two-dimensional lattice gauge theories, to investigate their phase diagrams and low-lying excitations.
How accurate are stellar ages based on stellar models ? I. The impact of stellar models uncertainties

Among the various methods used to age-date stars, methods based on stellar model predictions are widely used, for nearly all kind of stars in large ranges of masses, chemical compositions and evolutionary stages. The precision and accuracy on the age determination depend on both the precision and number of observational constraints, and on our ability to correctly describe the stellar interior and evolution. The imperfect input physics of stellar models as well as the uncertainties on the initial chemical composition of stars are responsible for uncertainties in the age determination. We present an overview of the calculation of stellar models and discuss the impact on age of their numerous inputs.
Lean practices and supply-chain competitiveness in the steel industry in Gauteng, South Africa

Background: The steel industry in South Africa suffered significantly when imported steel took over the market and collapsed big players in the industry in the last decade. The industry requires new business models and paradigms to improve its supply-chain strategies and adopt international standards such as lean supply-chain management practices to become competitive.Aim: In the study the relationships are investigated between lean supply-chain management practices, lean culture, and supply-chain competitiveness in the steel industry in Gauteng Province.Setting: The study was conducted in the steel manufacturing industry in the Gauteng Province, South Africa.Methods: In the study a quantitative method involving 265 supply-chain and operations managers and practitioners was employed. The Statistical Packages for Social Sciences (SPSS version 27.0) was used to analyse the data in which correlations and regression analysis were employed to test the research hypotheses.Results: The results of the study showed that four lean practices, namely Just in Time, Total Quality Management, Strategic Partnerships and Waste Elimination, all predict the establishment of a lean culture. However, Human Resource Management was statistically insignificant. The results further showed that a lean culture predicts competitiveness in the steel supply chain.Conclusion: The adoption of lean supply chain management in the steel industry is an essential contributor to its success.
Gravitational collapse of thin shell of dust in shape dynamics

We studied the gravitational collapse of a shell of dust in shape dynamics. We found out static and oscillatory solutions. In the large momentum limit we found out that the shell never reaches the singularity when the momentum of the shell is much larger than the mass of the shell in magnitude. The shell does not reach to the origin in a finite amount of time however when the momentum of the shell becomes comparable to minus the mass of shell, the large momentum approximation breaks down. Therefore more detailed future works hopefully may be able to answer the question of singularity formation in this setup.
ournal of C osmology and A stroparticle hysics Anisotropic universe with anisotropic sources

We analyze the state space of a Bianchi-I universe with anisotropic sources. Here we consider an extended state space which includes null geodesics in this background. The evolution equations for all the state observables are derived. Dynamical systems approach is used to study the evolution of these equations. The asymptotic stable ﬁxed points for all the evolution equations are found. We also check our analytic results with numerical analysis of these dynamical equations. The evolution of the state observables are studied both in cosmic time and using a dimensionless time variable. Then we repeat the same analysis with a more realistic scenario, adding the isotropic (dust like dark) matter and a cosmological constant (dark energy) to our anisotropic sources, to study their co-evolution. The universe now approaches a de Sitter space asymptotically dominated by the cosmological constant. The cosmic microwave background anisotropy maps due to shear are also generated in this scenario, assuming that the universe contains anisotropic matter along with the usual (dark) matter and vacuum (dark) energy since decoupling. We ﬁnd that they contribute dominantly to the CMB quadrupole. We also constrain the current level of anisotropy and also search for any cosmic preferred axis present in the data. We use the Union 2 Supernovae data to this extent. An anisotropy axis close to the mirror symmetry axis seen in the cosmic microwave background data from Planck probe is found.
OGLE-2017-BLG-0482Lb: A Microlensing Super-Earth Orbiting a Low-mass Host Star

We report the discovery of a planetary system in which a super-Earth orbits a late M-dwarf host. The planetary system was found from the analysis of the microlensing event OGLE-2017-BLG-0482, wherein the planet signal appears as a short-term anomaly to the smooth lensing light curve produced by the host. Despite its weak signal and short duration, the planetary signal was firmly detected from the dense and continuous coverage by three microlensing surveys. We find a planet/host mass ratio of q ∼ 1.4 × 10−4. We measure the microlens parallax from the long-term deviation in the observed lensing light curve, but the angular Einstein radius cannot be measured because the source trajectory did not cross the planet-induced caustic. Using the measured event timescale and the microlens parallax, we find that the masses of the planet and the host are and , respectively, and the projected separation between them is au. The estimated distance to the lens is kpc. The discovery of the planetary system demonstrates that microlensing provides an important method to detect low-mass planets orbiting low-mass stars.
Appraisal of Resistivity Inversion Models With Convolutional Variational Encoder–Decoder Network

Recovering the actual subsurface electrical resistivity properties from the electrical resistivity tomography data is challenging because the inverse problem is nonlinear and ill-posed. This article proposes a variational encoder-decoder (VED)-based network to obtain resistivity model, which maps the apparent resistivity data (input) to true resistivity data (output). Since deep learning (DL) models are highly dependent on training sets and providing a meaningful geological resistivity model is complex, we have first developed an algorithm to construct many realistic resistivity synthetic models. Our algorithm automatically constructs an apparent resistivity pseudo-section from these resistivity models. We further computed the resistivity from two different neural architectures for comparison–UNet, and attention UNet with and without input depth encoding apparent data. In the end, we have compared our DL results with traditional inversion and borewell data on apparent resistivity datasets collected for aquifer mapping in the hard rock terrain of the West Medinipur district of West Bengal, India. A detailed qualitative and quantitative evaluation reveals that our VED approach is the most effective for the inversion compared to other approaches considered.
Convex Quadratic Programming for Slimming Convolutional Networks

To reduce the computational and memory cost of ConvNets, structured pruning consists in removing features in convolutional and/or fully-connected layers of a pretrained network. As a novel contribution, we study the selection of features as a convex quadratic program with linear constraints. In addition, the updating of weights is treated as the resolution of a linear least-squares system. The quadratic objective function arises from the least-squares reconstruction error on the outputs of pruned layers. Experiments show that our method gives accuracies on par with other reconstruction error-based methods, while achieving a clear gain on computation time.
Validation of a Bullying Scale in Peruvian Adolescents and Gender-Speciﬁc Diﬀerences

Abstract The objective of the study was to evaluate the psychometric properties of the European Bullying Intervention Project Questionnaire (EBIPQ) inPeruvian adolescents and to determine gender-specific differences. The sample comprised 532 students in sixth grade of elementary school to third grade of high school. To validate the instrument, we requested an expert judgement and conducted a pilot test. Subsequently, we performed the exploratory factorial analysis, which showed that all the questions were correctly loaded in both components, an aspect that explained the 48.6%variance. We determined the reliability by means of the internal-consistency method using the Cronbach’s alfa (αtotal= .856;αvictimization= .807;αaggression= .828). We found gender-specific differences in bullying roles(p<.001). In conclusion, the factorial structure of the EBIPQ in Peruvian adolescents is similar to the original questionnaire and presents high reliability and construct validity.
ON THE DYNAMICS AND TIDAL DISSIPATION RATE OF THE WHITE DWARF IN 4U 1820-30

It has been suggested that the 170 day period in the light curve of the low-mass X-ray binary 4U 1820-30 arises from the presence of a third body with a large inclination to the binary orbit. We show that this long-period motion arises if the system is librating around the stable fixed point in a Kozai resonance. We demonstrate that mass transfer drives the system toward this fixed point and calculate, both analytically and via numerical integrations, that the period of libration is of order 170 days when the mutual inclination is near the Kozai critical value. The non-zero eccentricity of the binary, combined with tidal dissipation, implies that the rate of change of the binary period would be slower than, or even of opposite sign to, that implied by standard mass transfer models. If the 170 day period results from libration, then, contrary to appearances, the orbital period of the inner binary is increasing with time; in that case, (e/0.009)2Q/k2 ≳ 2.5 × 109, where k2 ≈ 0.01 is the tidal Love number and e = 0.009 is the fiducial eccentricity of the inner binary. It appears unlikely that the observed negative period derivative results from the smaller than expected (but positive) value of combined with the previously suggested acceleration of the system in the gravitational field of the host globular cluster NGC 6624. The discrepancy between the observed and the expected period derivative requires further investigation.
Excitation of multiple 2-mode parametric resonances by a single driven mode

We demonstrate autoparametric excitation of two distinct sub-harmonic mechanical modes by the same driven mechanical mode corresponding to different drive frequencies within its resonance dispersion band. This experimental observation is used to motivate a more general physical picture wherein multiple mechanical modes could be excited by the same driven primary mode within the same device as long as the frequency spacing between the sub-harmonic modes is less than half the dispersion bandwidth of the driven primary mode. The excitation of both modes is seen to be threshold-dependent and a parametric back-action is observed impacting on the response of the driven primary mode. Motivated by this experimental observation, modified dynamical equations specifying 2-mode auto-parametric excitation for such systems are presented.
The Evolution of Molecular Gas Fraction Traced by the CO Tully–Fisher Relation

Carbon monoxide (CO) observations show a luminosity−line width correlation that evolves with redshift. We present a method to use CO measurements alone to infer the molecular gas fraction (fmol) and constrain the CO−H2 conversion factor (αCO). We compile from the literature spatially integrated low-J CO observations of six galaxy populations, including a total of 449 galaxies between 0.01 ≤ z ≤ 3.26. The CO data of each population provide an estimate of the -normalized mean molecular gas fraction (fmol/αCO). The redshift evolution of the luminosity−line width correlation thus indicates an evolution of fmol/αCO. We use a Bayesian-based Monte Carlo Markov Chain sampler to derive the posterior probability distribution functions of fmol/αCO for these galaxy populations, accounting for random inclination angles and measurement errors in the likelihood function. We find that the molecular gas fraction evolves rapidly with redshift, with β ≃ 2, for both normal star-forming and starburst galaxies. Furthermore, the evolution trend agrees well with that inferred from the Kennicutt–Schmidt relation and the star-forming main sequence. Finally, at z < 0.1 normal star-forming galaxies (SFGs) require a ∼5× larger αCO than starburst galaxies to match their molecular gas fractions, but at z > 1 both star-forming types exhibit sub-Galactic αCO values and normal SFGs appear more gas rich than starbursts. Future applications of this method include calibrating Tully–Fisher relations without inclination correction and inferring the evolution of the atomic gas fraction with H i observations.
CORE-COLLAPSE SUPERNOVAE FROM 9 TO 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONS

Nucleosynthesis, light curves, explosion energies, and remnant masses are calculated for a grid of supernovae (SNe) resulting from massive stars with solar metallicity and masses from 9.0 to 120 M ⊙ . The full evolution is followed using an adaptive reaction network of up to 2000 nuclei. A novel aspect of the survey is the use of a one-dimensional neutrino transport model for the explosion. This explosion model has been calibrated to give the observed energy for SN 1987A, using five standard progenitors, and for the Crab SN using a 9.6 M ⊙ progenitor. As a result of using a calibrated central engine, the final kinetic energy of the SN is variable and sensitive to the structure of each pre-SN star. Many progenitors with extended core structures do not explode, but become black holes (BHs), and the masses of exploding stars do not form a simply connected set. The resulting nucleosynthesis agrees reasonably well with the Sun provided that a reasonable contribution from SNe Ia is also allowed, but with a deficiency of light s-process isotopes. The resulting neutron star initial mass function has a mean gravitational mass near 1.4 M ⊙ . The average BH mass is about 9 M ⊙ if only the helium core implodes, and 14 M ⊙ if the entire pre-SN star collapses. Only ∼10% of SNe come from stars over 20 M ⊙ , and some of these are Type Ib or Ic. Some useful systematics of Type IIp light curves are explored.
How odd: Diverging effects of predictability and plausibility violations on sentence reading and word memory

Abstract How do violations of predictability and plausibility affect online language processing? How does it affect longer-term memory and learning when predictions are disconfirmed by plausible or implausible words? We investigated these questions using a self-paced sentence reading and noun recognition task. Critical sentences violated predictability or plausibility or both, for example, “Since Anne is afraid of spiders, she doesn’t like going down into the … basement (predictable, plausible), garden (unpredictable, somewhat plausible), moon (unpredictable, deeply implausible). ” Results from sentence reading showed earlier-emerging effects of predictability violations on the critical noun, but later-emerging effects of plausibility violations after the noun. Recognition memory was exclusively enhanced for deeply implausible nouns. The earlier-emerging predictability effect indicates that having word form predictions disconfirmed is registered very early in the processing stream, irrespective of semantics. The later-emerging plausibility effect supports models that argue for a staged architecture of reading comprehension, where plausibility only affects a post-lexical integration stage. Our memory results suggest that, in order to facilitate memory and learning, a certain magnitude of prediction error is required.
Investigating the origin of the faint non-thermal emission of the Arches cluster using the 2015–2016NuSTARandXMM–NewtonX-ray observations

Recent NuSTAR and XMM-Newton observations of the molecular cloud around the Arches stellar cluster demonstrate a dramatic change both in morphology and intensity of its non-thermal X-ray emission, similar to that observed in many molecular clouds of the Central Molecular Zone at the Galactic Center. These variations trace the propagation of illuminating fronts, presumably induced by past flaring activities of Sgr A$^{\star}$. In this paper we present results of a long NuSTAR observation of the Arches complex in 2016, taken a year after the previous XMM+NuSTAR observations which revealed a strong decline in the cloud emission. The 2016 NuSTAR observation shows that both the non-thermal continuum emission and the Fe K$_{\alpha}$ 6.4~keV line flux are consistent with the level measured in 2015. No significant variation has been detected in both spectral shape and Fe K$_{\alpha}$ equivalent width EW$_{\rm 6.4\ keV}$, which may be interpreted as the intensity of the Arches non-thermal emission reaching its stationary level. At the same time, the measured 2016 non-thermal flux is not formally in disagreement with the declining trend observed in 2007-2015. Thus, we cannot assess whether the non-thermal emission has reached a stationary level in 2016, and new observations, separated by a longer time period, are needed to draw stringent conclusions. Detailed spectral analysis of three bright clumps of the Arches molecular cloud performed for the first time showed different EW$_{\rm 6.4\ keV}$ and absorption. This is a strong hint that the X-ray emission from the molecular cloud is a mix of two components with different origins.