Miracle-dz/UniFAR-FTUs huggingface dataset:
Optimising Puppy Socialisation–Short- and Long-Term Effects of a Training Programme during the Early Socialisation Period

Simple Summary The socialisation period in dog puppies (approx. 3–12 weeks) is one of the most important periods in determining later behaviour. Nonetheless, only a few studies investigated how socialisation can be optimised. Here, we tested whether providing small “challenge” exercises to puppies early in the socialisation period (between 3 and 6 weeks of age) enables puppies to cope better with stressful stimuli later. Eighty-three puppies from 12 litters of various breeds were enrolled. Half of each litter was assigned to the treatment group and was carefully exposed to potentially startling stimuli, novel objects, and problem-solving tasks over a period of three weeks. The other half of the litter served as a control group and received no additional exercises. All puppies were tested in a behaviour test at 6–7 weeks of age. Puppies from the treatment group were bolder towards a novel object, startled less after a loud noise, solved the problem-solving task faster, and showed higher persistence in problem-solving task than the control group. These findings demonstrate beneficial effects of the exercises. However, at the age of six months, there were no differences in owner-reported personality measures between the groups. To achieve lasting effects, it may be necessary to continue with the training exercises for a longer time period. Abstract The socialisation period in dog puppies is one of the most important periods determining behavioural development in dogs. Here, we aimed to test the effect of providing stimulation (beyond mere exposure) early during the socialisation period (approx. 3–6 weeks) on puppies’ behaviour. Each of 12 litters (83 puppies) of various breeds was divided into a treatment and a control group. Between 3–6 weeks, the treatment group received age-appropriate “challenge” exercises (carefully graded noise exposure, novel objects, and problem-solving tasks) four times per week (total 12 times). The control group spent the same time with the trainer, who cuddled or played with the puppies. In a behaviour test at 6–7 weeks, two of four principal components, “social-startle” and “response to novelty”, differed significantly between the groups. Treatment puppies were bolder towards the novel object, showed a reduced startle reaction, and recovered more quickly after a loud noise. Furthermore, they accomplished the problem-solving task faster and were more persistent during problem-solving than the control group. The control group showed a higher interest in a friendly stranger. It is a possibility that increased handling experienced by the control group had beneficial effects on their sociability. No long-term effects of the treatment were found, as determined by a validated dog personality questionnaire, available for 67 dogs at the age of six months. Likely, a continuation of the treatment over a longer time period would be necessary to obtain lasting effects, since the training took place only during the first third of the socialisation period.
Modeling and Forecasting Monkeypox Cases Using Stochastic Models

Background: Monkeypox virus is gaining attention due to its severity and spread among people. This study sheds light on the modeling and forecasting of new monkeypox cases. Knowledge about the future situation of the virus using a more accurate time series and stochastic models is required for future actions and plans to cope with the challenge. Methods: We conduct a side-by-side comparison of the machine learning approach with the traditional time series model. The multilayer perceptron model (MLP), a machine learning technique, and the Box–Jenkins methodology, also known as the ARIMA model, are used for classical modeling. Both methods are applied to the Monkeypox cumulative data set and compared using different model selection criteria such as root mean square error, mean square error, mean absolute error, and mean absolute percentage error. Results: With a root mean square error of 150.78, the monkeypox series follows the ARIMA (7,1,7) model among the other potential models. Comparatively, we use the multilayer perceptron (MLP) model, which employs the sigmoid activation function and has a different number of hidden neurons in a single hidden layer. The root mean square error of the MLP model, which uses a single input and ten hidden neurons, is 54.40, significantly lower than that of the ARIMA model. The actual confirmed cases versus estimated or fitted plots also demonstrate that the multilayer perceptron model has a better fit for the monkeypox data than the ARIMA model. Conclusions and Recommendation: When it comes to predicting monkeypox, the machine learning method outperforms the traditional time series. A better match can be achieved in future studies by applying the extreme learning machine model (ELM), support vector machine (SVM), and some other methods with various activation functions. It is thus concluded that the selected data provide a real picture of the virus. If the situations remain the same, governments and other stockholders should ensure the follow-up of Standard Operating Procedures (SOPs) among the masses, as the trends will continue rising in the upcoming 10 days. However, governments should take some serious interventions to cope with the virus. Limitation: In the ARIMA models selected for forecasting, we did not incorporate the effect of covariates such as the effect of net migration of monkeypox virus patients, government interventions, etc.
Cosmic chemical evolution with an early population of intermediate-mass stars

We explore the effect of an early population of intermediate-mass stars in the 2-8 M ⊙ range on the cosmic chemical evolution. We discuss the implications of this population as it pertains to several cosmological and astrophysical observables. For example, some very metal poor Galactic stars show large enhancements of carbon, typical of the C-rich ejecta of intermediate-mass stars; moreover, halo star carbon and oxygen abundances show wide scatter, which imply a wide range of star formation and nucleosynthetic histories contributed to the first generations of stars. Also, recent analyses of the 4 He abundance in metal-poor extragalactic H II regions suggest an elevated abundance Y p ≃ 0.256 by mass, higher than the predicted result from the big bang nucleosynthesis, assuming the baryon density determined by the WMAP, Y p = 0.249. Although there are large uncertainties in the observational determination of 4 He, this offset may suggest a prompt initial enrichment of 4 He in early metal-poor structures. We also discuss the effect of intermediate-mass stars on the global cosmic evolution, the reionization of the Universe, the density of white dwarfs, as well as Type II supernovae (SN II) and SN Ia rates at high redshift. We also comment on the early astration of D and 7 Li. We conclude that if intermediate-mass stars are to be associated with Population III stars, their relevance is limited (primarily from observed abundance patterns) to low-mass structures involving a limited fraction of the total baryon content of the Universe.
Four questions for quantum-classical hybrid theory

Four questions are discussed which may be addressed to any proposal of a quantum-classical hybrid theory which concerns the direct coupling of classical and quantum mechanical degrees of freedom. In particular, we consider the formulation of hybrid dynamics presented recently in Ref. [1]. This linear theory differs from the nonlinear ensemble theory of Hall and Reginatto, but shares with it to fulfil all consistency requirements discussed in the literature, while earlier attempts failed. - Here, we additionally ask: Does the theory allow for superposition, separable, and entangled states originating in the quantum mechanical sector? Does it allow for "Free Will", as introduced, in this context, by Diósi [2]? Is it local? Does it provide hints for the emergence of quantum mechanics from dynamics beneath?
Physical as Well as Psychological Distress and Coping with Situational Dilemmas Experienced by People Infected with COVID-19: A Mixed Method Study

The COVID-19 pandemic caused serious health problems that affected people around the globe. This study aims to understand the physical distress (PhyD), psychological distress (PsyD), and coping experiences among people infected with COVID-19, develop a grounded theory, and examine PhyD, PsyD, and coping among people infected with COVID-19. A sequential exploratory mixed methods strategy is employed. A qualitative procedure is based on a grounded theory; data collection includes observation and in-depth interviews with 25 participants, aged 18 years and above. The quantitative one included 180 participants. Content analysis was applied using the Strauss and Corbin method, and ATLAS.ti software. Descriptive statistics, Pearson’s correlation, and the independent t-test were used. Results: The six major themes, including (1) severity of COVID-19 symptoms, (2) death anxiety, (3) uncertainty, (4) barrier to healthcare access, (5) compliance and self-regulation coping (6) post-COVID-19 effects. PhyD, PsyD, and coping were all at a moderate level. The relationship between PhyD, PsyD, and coping was positive. The prevalence in post-COVID-19 effects was 70% (95% CI 63.3-76.4%). There were higher amounts in women than men. The most frequent residual symptoms were decreased activity tolerance (40%), fatigue (33.3%), anxiety and fear of abnormal lungs (33.3%), dyspnea (27.8%), allergy (24.4%), and lung impairment (22.2%). Moreover, the prevalence of more than two symptoms was 54% (95% CI 47.2–61.7%). This study considers that the healthcare providers should be concerned with sufficient healthcare services. Interventions are needed for supporting their recovery from COVID-19 effects.
Ultralight Axion Dark Matter and Its Impact on Dark Halo Structure in N-body Simulations

Ultralight axion is a dark matter candidate with mass and de Broglie wavelength of order kiloparsec. Such an axion, also called fuzzy dark matter (FDM), thermalizes via gravitational force and forms a Bose–Einstein condensate. Recent studies suggested that the quantum pressure from FDM can significantly affect structure formation in small scales, thus alleviating the so-called “small-scale crisis. ” In this paper, we develop a new technique to discretize the quantum pressure and illustrate the interactions among FDM particles in an N-body simulation that accurately simulates the formation of the dark matter halo and its inner structure in the region outside the softening length. In a self-gravitationally bound virialized halo, we find a constant density solitonic core, which is consistent with theoretical prediction. The existence of the solitonic core reveals the nonlinear effect of quantum pressure and impacts structure formation in the FDM model.
THE SPECTACULAR RADIO-NEAR-IR-X-RAY JET OF 3C 111: THE X-RAY EMISSION MECHANISM AND JET KINEMATICS

Relativistic jets are the most energetic manifestation of the active galactic nucleus (AGN) phenomenon. AGN jets are observed from the radio through gamma-rays and carry copious amounts of matter and energy from the sub-parsec central regions out to the kiloparsec and often megaparsec scale galaxy and cluster environs. While most spatially resolved jets are seen in the radio, an increasing number have been discovered to emit in the optical/near-IR and/or X-ray bands. Here we discuss a spectacular example of this class, the 3C 111 jet, housed in one of the nearest, double-lobed FR II radio galaxies known. We discuss new, deep Chandra and Hubble Space Telescope (HST) observations that reveal both near-IR and X-ray emission from several components of the 3C 111 jet, as well as both the northern and southern hotspots. Important differences are seen between the morphologies in the radio, X-ray, and near-IR bands. The long (over 100 kpc on each side), straight nature of this jet makes it an excellent prototype for future, deep observations, as it is one of the longest such features seen in the radio, near-IR/optical, and X-ray bands. Several independent lines of evidence, including the X-ray and broadband spectral shape as well as the implied velocity of the approaching hotspot, lead us to strongly disfavor the EC/CMB model and instead favor a two-component synchrotron model to explain the observed X-ray emission for several jet components. Future observations with NuSTAR, HST, and Chandra will allow us to further constrain the emission mechanisms.
Faint dwarf galaxies in the Next Generation Virgo cluster Survey

The Next Generation Virgo Cluster Survey (NGVS) is a CFHT Large Program that is using the wide field of view capabilities of the MegaCam camera to map the entire Virgo Cluster from its core to virial radius. The observing strategy has been optimized to detect very low surface brightness structures in the cluster, including intracluster stellar streams and faint dwarf spheroidal galaxies. We present here the current status of this ongoing survey, with an emphasis on the detection and analysis of the very low-mass galaxies in the cluster that have been revealed by the NGVS.
Screening of Toxoplasmosis in Owned and Stray Dogs of District Faisalabad, Pakistan through Latex Agglutination and Indirect ELISA

Introduction: Toxoplasma gondii (an intracellular protozoan) causes toxoplasmosis in warm-blooded animals, including humans and dogs. The present study was carried out to investigate the seroprevalence of canine toxoplasmosis in the owned and stray populations of dogs in Faisalabad District, Punjab, Pakistan. Materials and Methods: Commercially available Latex Agglutination Test (LAT) kits were used for the screening of samples (139 stray and 150 owned), followed by confirmation through ELISA. For the statistical analyses, chi-square was used to correlate the prevalence of toxoplasmosis with various factors. Results: The overall prevalence of toxoplasmosis, determined by the LAT, was 22.5% and, by ELISA, was 21.8%. A nonsignificant association of toxoplasmosis was determined among owned and stray dogs. Among owned dog breeds, Bulldogs showed 28.30% prevalence, and among stray dogs, the highest prevalence was determined in Bhakarwal dogs (39.29%). Young and female dogs showed a slightly higher prevalence of toxoplasmosis than adults and males, respectively. Conclusions: The present study determined by LAT and ELISA in owned dogs showed the same results, while a little variation was found in the stray dogs. It is concluded that both owned and stray dogs are infected with toxoplasmosis in Faisalabad District, and based on this, it is recommended that province-wide epidemiological studies be carried out to examine the prevalence of Toxoplasma and develop policies in order to control toxoplasmosis.
Competition between spin-orbit coupling, magnetism, and dimerization in the honeycomb iridates: α -Li 2 IrO 3 under pressure

Single-crystal x-ray diffraction studies with synchrotron radiation on the honeycomb iridate $\alpha$-Li$_{2}$IrO$_{3}$ reveal a pressure-induced structural phase transition with symmetry lowering from monoclinic to triclinic at a critical pressure of $P_{c}$ = 3.8 GPa. According to the evolution of the lattice parameters with pressure, the transition mainly affects the $ab$ plane and thereby the Ir hexagon network, leading to the formation of Ir--Ir dimers. These observations are independently predicted and corroborated by our \textit{ab initio} density functional theory calculations where we find that the appearance of Ir--Ir dimers at finite pressure is a consequence of a subtle interplay between magnetism, correlation, spin-orbit coupling, and covalent bonding. Our results further suggest that at $P_{c}$ the system undergoes a magnetic collapse. Finally we provide a general picture of competing interactions for the honeycomb lattices $A_{2}$$M$O$_{3}$ with $A$= Li, Na and $M$ = Ir, Ru.
Large-Eddy Simulation of Turbulent Barotropic Flows in Spectral Space on a Sphere

AbstractNumerical simulations of atmospheric circulation models are limited by their finite spatial resolution, so large-eddy simulation (LES) is a preferred approach to study these models. In LES, a low-pass filter is applied to the flow field to separate the large- and small-scale motions. In implicitly filtered LES, the computational mesh and discretization schemes are considered to be the low-pass filter, while in the explicitly filtered LES approach, the filtering procedure is separated from the grid and discretization operators and allows for better control of the numerical errors. The aim of this paper is to study and compare implicitly filtered and explicitly filtered LES of atmospheric circulation models in spectral space. To achieve this goal, the results of implicitly filtered and explicitly filtered LES of a barotropic atmosphere circulation model on a sphere in spectral space are presented and compared with the results obtained from direct numerical simulation (DNS). Different numerical exper.
Dark gas in the solar neighborhood from extinction data

Context. When modeling infrared or γ-ray data as a linear combination of observed gas tracers, excess emission has been detected compared to expectations from known neutral and molecular gas traced by HI and CO measurements, respectively. This excess might correspond to additional gas component. This so-called “dark gas” (DG) has been observed in our Galaxy, as well as the Magellanic Clouds. Aims. For the first time, we investigate the correlation between visible extinction (AV) data and gas tracers on large scales in the solar neighborhood, to detect DG and to verify our compatibility with previous studies. Methods. Our work focuses on both the solar neighborhood (|b| > 10 ◦ ), and the inner and outer Galaxy, as well as on four individual regions: Taurus, Orion, Cepheus-Polaris, and Aquila-Ophiuchus. Thanks to the recent production of an all-sky AV map, we first perform the correlation between AV and both HI and CO emission over the most diffuse regions (with low-to-intermediate gas column densities), to derive the optimal (AV/NH) ref ratio. We then iterate the analysis over the entire regions (including low and high gas column densities) to estimate the CO-to-H2 conversion factor, as well as the DG mass fraction. Results. The average extinction to gas column-density ratio in the solar neighborhood is found to be (AV/NH) ref = 6.53 × 10 −22 mag cm 2 , with significant differences between the inner and outer Galaxy, of about 60%. We derive an average value of the CO-to-H2 conversion factor of XCO = 1.67 × 10 20 H2 cm −2 /(K km s −1 ), with significant variations between nearby clouds. In the solar neighborhood, the gas mass in the dark component is found to be 19% relative to that in the atomic component and 164% relative to the one traced by CO. These results are compatible with a recent analysis of Planck data within the uncertainties of our measurements. We estimate the ratio of dark gas to total molecular gas to be 0.62 in the solar neighborhood. The HI-to-H2 and H2-to-CO transitions appear for AV � 0.2 mag and AV � 1.5 mag, respectively, in agreement with theoretical models of dark-H2 gas.
The Energetics of White-light Flares Observed by SDO/HMI and RHESSI

White-light (WL) flares have been observed and studied for more than a century since their first discovery. However, some fundamental physics behind the brilliant emission remains highly controversial. One of the important facts in addressing the flare energetics is the spatio-temporal correlation between the WL emission and the hard X-ray (HXR) radiation, presumably suggesting that energetic electrons are the energy sources. In this study, we present a statistical analysis of 25 strong flares (≥M5) observed simultaneously by the Helioseismic and Magnetic Imager (HMI), on board the Solar Dynamics Observatory (SDO), and the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). Among these events, WL emission was detected by SDO/HMI in 13 flares, associated with HXR emission. To quantitatively describe the strength of WL emission, equivalent area (EA) is defined as the integrated contrast enhancement over the entire flaring area. Our results show that the EA is inversely proportional to the HXR power-law index, indicating that stronger WL emission tends to be associated with a larger population of high energy electrons. However, no obvious correlation is found between WL emission and flux of non-thermal electrons at 50 keV. For the other group of 13 flares without detectable WL emission, the HXR spectra are softer (larger power-law index) than those flares with WL emission, especially for the X-class flares in this group.
Out-of-equilibrium dynamics in the bidimensional spin-ice model

We study the dynamics of 2d spin-ice following a quench from a fully disordered initial condition (equilibrium at infinite temperature) into its disordered, ferromagnetic and antiferromagnetic phases. We analyze the evolution of the density of topological defects and we show that these take finite density over very long periods of time in all kinds of quenches. We identify the leading mechanisms for the growth of domains in the ordered phases and we evaluate the (anisotropically) growing lengths involved in dynamic scaling.
OBSERVATIONS OF OUTFLOWING ULTRAVIOLET ABSORBERS IN NGC 4051 WITH THE COSMIC ORIGINS SPECTROGRAPH

We present new Hubble Space Telescope (HST)/Cosmic Origins Spectrograph (COS) observations of the narrow-line Seyfert 1 galaxy NGC 4051. These data were obtained as part of a coordinated observing program including X-ray observations with the Chandra/High Energy Transmission Grating (HETG) spectrometer and Suzaku. We detected nine kinematic components of UV absorption, which were previously identified using the HST/Space Telescope Imaging Spectrograph (STIS). None of the absorption components showed evidence for changes in column density or profile within the ∼10 yr between the STIS and COS observations, which we interpret as evidence of (1) saturation, for the stronger components, or (2) very low densities, i.e., nH < 1 cm−3, for the weaker components. After applying a +200 km s−1 offset to the HETG spectrum, we found that the radial velocities of the UV absorbers lay within the O vii profile. Based on photoionization models, we suggest that, while UV components 2, 5, and 7 produce significant O vii absorption, the bulk of the X-ray absorption detected in the HETG analysis occurs in more highly ionized gas. Moreover, the mass-loss rate is dominated by high-ionization gas which lacks a significant UV footprint.
A Highly Stable Physically Unclonable Function Using Algorithm-Based Mismatch Hardening Technique in 28-nm CMOS

Physically unclonable function (PUF) is an emerging security solution for Internet of Things (IoT) devices. However, PUF faces a critical design challenge: responses should remain the same regardless of environmental conditions. This article presents an algorithm-based mismatch hardening technique that provides an effective and efficient solution to stabilizing PUF responses, which could be applied to various PUF circuits. The proposed stabilization technique combines multiple mismatches to achieve high reliability with minimum loss of utility. Moreover, the proposed approach requires only the available digitized PUF responses, avoiding any auxiliary measurement circuit to minimize additional implementation and testing overhead. The PUF test chip implemented in 28-nm CMOS technology shows that the proposed stabilization technique achieves a highly stable performance, lowering the nominal bit error rate (BER) to 0.0016%. It also exhibits excellent reliability with a worst-case BER of 0.16% across 0.7 to 1.2 V and −50 to 125°C, proving to be a promising candidate for security primitive for IoT applications.