Miracle-dz/UniFAR-FTUs huggingface dataset:
Automotive algorithm implemented in the microcontroller for adapting regenerative braking

In this paper an original adaptive method for maximizing the energy transferred to the car's battery during regenerative braking is presented. The paper is based on a simulation in Proteus LabCenter, using a battery model, based on functional criteria, with the energy recovered from a reversible motor. The battery management algorithm was implemented on ATMEGA 328 microcontroller, and a MC34063 DC-to-DC converter control circuit. The voltage variations of reversible motor, recovered during braking are simulated with a variable voltage applied on the system input and the results show that the output voltage of the DC-to-DC converter must be continuously adjusted during the braking process. The efficiency lies in the fact that although the braking sequences do not take place for long periods, they are made at currents recovered from magnetic induction of considerable values.
Chiral and deconfinement phase transition in the Hamiltonian approach to QCD in Coulomb gauge

The chiral and deconfinement phase transitions are investigated within the variational Hamiltonian approach to QCD in Coulomb gauge. The temperature $\beta^{- 1}$ is introduced by compactifying a spatial dimension. Thereby the whole temperature dependence is encoded in the vacuum state on the spatial manifold $\mathbb{R}^2 \times S^1 (\beta)$. The chiral quark condensate and the dual quark condensate (dressed Polyakov loop) are calculated as function of the temperature. From their inflection points the pseudo-critical temperatures for the chiral and deconfinement crossover transitions are determined. Using the zero-temperature quark and gluon propagators obtained within the variational approach as input, we find $168 \, \mathrm{MeV}$ and $196 \, \mathrm{MeV}$, respectively, for the chiral and deconfinement transition.
Sagnac with Double-Sense Twisted Low-Birefringence Standard Fiber as Vibration Sensor

In this work, we study a double-sense twisted low-birefringence Sagnac loop structure as a sound/vibration sensing device. We study the relation between the adjustments of a wave retarder inside the loop (which allows controlling the transmission characteristic to deliver 10, 100, and 300 μW average power at the output of the system) and the response of the Sagnac sensor to vibration frequencies ranging from 0 to 22 kHz. For a 300 m loop Sagnac, two sets of experiments were carried out, playing at the same time all the sound frequencies mixed for ∼1 s, and playing a sweep of frequencies for 30 s. In both cases, the time- and frequency-domain transmission amplitudes are larger for an average power of 10 μW, and smaller for an average power of 300 μW. For mixed frequencies, the Fourier analysis shows that the Sagnac response is larger for low frequencies (from 0 to ∼5 kHz) than for high frequencies (from ∼5 kHz to ∼22 kHz). For a sweep of frequencies, the results reveal that the interferometer perceives all frequencies. However, beyond ∼2.5 kHz, harmonics are present each ∼50 Hz, revealing that some resonances are present. The results about the influence of the power transmission through the polarizer and power emission of laser diode (LD) on the Sagnac interferometer response at high frequencies reveal that our system is robust, and the results are highly reproducible, and harmonics do not depend on the state of polarization at the input of the Sagnac interferometer. Furthermore, increasing the LD output power from 5 mW to 67.5 mW allows us to eliminate noisy signals at the system output. in our setup, the minimum sound level detected was 56 dB. On the other hand, the experimental results of a 10 m loop OFSI reveal that the response at low frequencies (1.5 kHz to 5 kHz) is minor compared with the 300 m loop OFSI. However, the response at high frequencies is low but still enables the detection of these frequencies, yielding the possibility of tuning the response of the vibration sensor by varying the length of the Sagnac loop.
The effect of mass ratio on the morphology and time-scales of disc galaxy mergers: Effect of mass ratio on merger morphology

The majority of galaxy mergers are expected to be minor mergers. The observational signatures of minor mergers are not well understood, thus there exist few constraints on the minor merger rate. This paper seeks to address this gap in our understanding by determining if and when minor mergers exhibit disturbed morphologies and how they differ from the morphology of major mergers. We simulate a series of unequalmass moderate gas-fraction disc galaxy mergers. With the resulting g-band images, we determine how the time-scale for identifying galaxy mergers via projected separation and quantitative morphology (the Gini coefficient G, asymmetry A, and the secondorder moment of the brightest 20% of the light M20) depends on the merger mass ratio, relative orientations and orbital parameters. We find that G−M20 is as sensitive to 9:1 baryonic mass ratio mergers as 1:1 mergers, with observability time-scales ∼ 0.2−0.4 Gyr. In contrast, asymmetry finds mergers with baryonic mass ratios between 4:1 and 1:1 (assuming local disc galaxy gas-fractions). Asymmetry time-scales for moderate gas-fraction major disc mergers are∼ 0.2−0.4 Gyr, and less than 0.06 Gyr for moderate gas-fraction minor mergers. The relative orientations and orbits have little effect on the time-scales for morphological disturbances. Observational studies of close pairs often select major mergers by choosing paired galaxies with similar luminosities and/or stellar masses. Therefore, the various ways of finding galaxy mergers (G − M20, A, close pairs) are sensitive to galaxy mergers of different mass ratios. By comparing the frequency of mergers selected by different techniques, one may place empirical constraints on the major and minor galaxy merger rates.
Tomographic Mapping of Water Temperature and Current in a Reservoir by Trust-Region Method Based on CAT

Remote sensing of water parameters and flow dynamic progress is of critical importance to water environment observation. Underwater acoustic tomography technology uses multiple sound stations to construct distributed sensing network for large-scale measurement, which has big superiority in water parameter observation compared with fix-point measurement. Water parameter variation progress can be monitored with an underwater acoustic tomography sensing system. This article develops a grid-averaged trust-region method for water parameter detailed profiling with coastal acoustic tomography (CAT) systems. A remote sensing experiment was conducted with five CAT systems from February 28 to March 7, 2022, in the Huangcai Reservoir in Changsha, China. Four CAT systems were deployed in the same position with different depths of sound transceivers, and another CAT station was set 650 m apart. Water temperature and flow current reconstruction results along the sound propagate Section were analyzed with the trust-region method and compared with the temperature data acquired with the temperature sensor. The accuracy and feasibility of this method are verified with observation results.
THE DISKMASS SURVEY. IV. THE DARK-MATTER-DOMINATED GALAXY UGC 463

We present a detailed and unique mass budget for the high surface brightness galaxy UGC 463, showing it is dominated by dark matter (DM) at radii beyond one scale length (hR) and has a baryonic-to-DM mass ratio of approximately 1:3 within 4.2hR. Assuming a constant scale height (hz; calculated via an empirical oblateness relation), we calculate dynamical disk mass surface densities from stellar kinematics, which provide vertical velocity dispersions after correcting for the shape of the stellar velocity ellipsoid (measured to have σθ/σR = 1.04 ± 0.22 and σz/σR = 0.48 ± 0.09). We isolate the stellar mass surface density by accounting for all gas mass components and find an average K-band mass-to-light ratio of ; Zibetti et al. and Bell et al. predict, respectively, 0.56 and 3.6 times our dynamical value based on stellar-population-synthesis modeling. The baryonic matter is submaximal by a factor of ∼3 in mass and the baryonic-to-total circular-speed ratio is 0.61+0.07−0.09(ran)+0.12−0.18(sys) at 2.2hR; however, the disk is globally stable with a multi-component stability that decreases asymptotically with radius to Q ∼ 2. We directly calculate the circular speed of the DM halo by subtracting the baryonic contribution to the total circular speed; the result is equally well described by either a Navarro–Frenk–White halo or a pseudo-isothermal sphere. The volume density is dominated by DM at heights of |z| ≳ 1.6hz for radii of R ≳ hR. As is shown in follow-up papers, UGC 463 is just one example among nearly all galaxies we have observed that contradict the hypothesis that high surface brightness spiral galaxies have maximal disks.
A tool for the morphological classification of galaxies: the concentration index

Using galaxy data from the Sloan Digital Sky Survey Data Release 8, I explore whether the concentration index is a good morphological classification tool and find that a reasonable sample of pure late-type galaxies can be constructed with the choice of the r-band concentration index ci=2.85. The opposite is not true, however, due to the fairly high contamination of an early-type sample by late-type galaxies. In such an analysis, the influence of selection effects is less important. To disentangle correlations of the morphology and concentration index with stellar mass, star formation rate (SFR), specific star formation rate (SSFR) and active galactic nucleus (AGN) activity, I investigate correlations of the concentration index with these properties at a fixed morphology and correlations of the morphology with these properties at a fixed concentration index. It is found that at a fixed morphology, high-concentration galaxies are preferentially more massive and have a lower SFR and SSFR than low-concentration galaxies, whereas at a fixed concentration index, elliptical galaxies are preferentially more massive and have a lower SFR and SSFR than spiral galaxies. This result shows that the stellar mass, SFR and SSFR of a galaxy are correlated with its concentration index as well as its morphology. In addition, I note that AGNs are preferentially found in more concentrated galaxies only in the sample of spiral galaxies.
Textual Analysis of Quality Assurance Development in Bosnia and Herzegovina’s Higher Education Sector

Education is the bedrock of any nation. It is essential for individual and societal growth and development. This study investigates the role of quality assurance in achieving the expected outcome of education in Bosnia and Herzegovina’s higher education sector. A textual analysis is used to examine the National Qualification Framework. The study is based on a documented review and descriptive analysis of student enrollment and programs of studies. The textual analysis is largely qualitative in nature. Unlike the global trend, it can be seen that student enrollment is on the decline in Bosnia and Herzegovina. It was found that quality assurance is an indispensable tool for strengthening the higher education sector and for achieving the desired change and outcomes that education offers. It was also found that study programs and curricula are pivotal for teaching and learning processes, and that a unified qualification framework is essential for achieving set objectives of education at all levels. The study recommended that sound quality assurance systems as well as an appropriate structure for monitoring and accreditation be put in place and be judiciously followed in order to achieve the desired outcomes in conjunction with the set objectives of higher education in the country. Moreover, certain pressures (i.e., democratic, economic, and systemic) and obstacles are looked at that show signs of epistemological, political, and institutional barriers that Bosnia and Herzegovina faces as a developing country Europeanizing its system of education.
THE UNUSUAL VERTICAL MASS DISTRIBUTION OF NGC 4013 SEEN THROUGH THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G)

NGC 4013 is a nearby Sb edge-on galaxy known for its “prodigious” H i warp and its “giant” tidal stream. Previous work on this unusual object shows that it cannot be fitted satisfactorily by a canonical thin+thick disk structure. We have produced a new decomposition of NGC 4013, considering three stellar flattened components (thin+thick disk plus an extra and more extended component) and one gaseous disk. All four components are considered to be gravitationally coupled and isothermal. To do so, we have used the 3.6 μm images from the Spitzer Survey of Stellar Structure in Galaxies. We find evidence for NGC 4013 indeed having a thin and a thick disk and an extra flattened component. This smooth and extended component (scale height zEC ∼ 3 kpc) could be interpreted as a thick disk or as a squashed ellipsoidal halo and contains ∼20% of the total mass of all three stellar components. We argue it is unlikely to be related to the ongoing merger or due to the off-plane stars from a warp in the other two disk components. Instead, we favor a scenario in which the thick disk and the extended component were formed in a two-stage process, in which an initially thick disk has been dynamically heated by a merger soon enough in the galaxy history to have a new thick disk formed within it.
High energy neutrinos from charm in astrophysical sources

We show that charm provides significant enhancement of the very high energy neutrino flux, when neutrinos originate in astrophysical sources with jets driven by central engines, such as gamma ray bursts or supernovae with jets. The neutrino flux from semi‐leptonic decays of charmed mesons is subject to much less hadronic and radiative cooling than the conventional flux from pion and kaon decays and therefore has a dominant contribution at higher energies, of relevance to future ultrahigh energy neutrino experiments.
LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations

The Local Cluster Substructure Survey (LoCuSS, Smith et al.) is a systematic multi-wavelength survey of more than 100 X-ray luminous galaxy clusters in the redshift range 0.14-0.3 selected from the ROSAT All Sky Survey. We used data on 37 LoCuSS clusters from the XMM-Newton archive to investigate the global scaling relations of galaxy clusters. The scaling relations based solely on the X-ray data ($S{-}T$, $S{-}Y_{\rm X}$, $P{-}Y_{\rm X}$, $M{-}T$, $M{-}Y_{\rm X}$, $M{-}M_{\rm gas}$, $M_{\rm gas}{-}T$, $L{-}T$, $L{-}Y_{\rm X}$, and $L{-}M$) obey empirical self-similarity and reveal no additional evolution beyond the large-scale structure growth. They also reveal up to 17 per cent segregation between all 37 clusters and non-cool core clusters. Weak lensing mass measurements are also available in the literature for 19 of the clusters with XMM-Newton data. The average of the weak lensing mass to X-ray based mass ratio is $1.09\pm 0.08$, setting the limit of the non-thermal pressure support to $9 \pm 8$ per cent. The mean of the weak lensing mass to X-ray based mass ratio of these clusters is ~1, indicating good agreement between X-ray and weak lensing masses for most clusters, although with 31-51 per cent scatter. The scatter in the mass-observable relations ($M{-}Y_{\rm X}$, $M{-}M_{\rm gas}$, and $M{-}T$) is smaller using X-ray based masses than using weak lensing masses by a factor of 2. With the scaled radius defined by the Y X profile – $r_{500}^{ Y_{\rm X},X}$, $r_{500}^{Y_{\rm X},{\rm wl}}$, and $r_{500}^{Y_{\rm X},{\rm si}}$, we obtain lower scatter in the weak lensing mass based mass-observable relations, which means the origin of the scatter is M wl and $M^{\rm X}$ instead of Y X . The normalization of the $M{-}Y_{\rm X}$ relation using X-ray mass estimates is lower than the one from simulations by up to 18–24 per cent at $3\sigma$ significance. This agrees with the $M{-}Y_{\rm X}$ relation based on weak lensing masses, the normalization of the latter being ~20 per cent lower than the one from simulations at ~$2\sigma$ significance. This difference between observations and simulations is also indicated in the $M{-}M_{\rm gas}$ and $M{-}T$ relations. Despite the large scatter in the comparison of X-ray to lensing, the agreement between these two completely independent observational methods is an important step towards controlling astrophysical and measurement systematics in cosmological scaling relations.
Halos in Dark Ages: Formation and Chemistry

Formation of halos in the dark ages from initial spherical perturbations is analyzed in a four-component universe (dark matter, dark energy, baryonic matter, and radiation) in the approximation of relativistic hydrodynamics. Evolution of density and velocity perturbations of each component is obtained by integration of a system of nine differential equations from z = 108 up to virialization, which is described phenomenologically. It is shown that the number density of dark matter halos with masses M ∼ 108–109 M⊙ virialized at z ∼ 10 is close to the number density of galaxies in comoving coordinates. The dynamical dark energy of classical scalar field type does not significantly influence the evolution of the other components, but dark energy with a small value of effective sound speed can affect the final halo state. Simultaneously, the formation/dissociation of the first molecules has been analyzed in the halos that are forming. The results show that number densities of molecules H2 and HD at the moment of halo virialization are ∼103 and ∼400 times larger, respectively, than on a uniformly expanding background. This is caused by increased density and rates of reactions at quasi-linear and nonlinear evolution stages of density and velocity of the baryonic component of halos. It is shown also that the temperature history of the halo is important for calculating the concentration of molecular ions with low binding energy. Hence, in a halo with virial temperature ∼105 K the number density of the molecular ion HeH+ is approximately 100 times smaller than that on the cosmological background.
Tasmanian Dairy Farmers’ Attitudes towards Using E-Extension Methods; Strengthening the Dairy Extension System for a Sustainable Dairy Industry in Tasmania, Australia

The Tasmanian dairy industry is one of the major contributors to the Tasmanian economy and Australia’s export portfolio. The Tasmanian Government funding plan (2018–2023) for RD&E focuses on sustainable dairy farm production with an impact pathway incorporating provisions for extension services. Considering the need for an effective extension system, the continued adaptation of extension services is required to ensure that there is a collaborative and learning mechanism between extension experts and farmers that supports relationship building and innovation. E-extension methods can increase dairy farmers’ access to timely information while addressing time and cost challenges by reducing personal visits and establishing frequent communications between farmers and extension workers. This study uses the Technology Acceptance Model (TAM) to understand the attitudes of dairy farmers toward using E-extension methods. It was revealed that dairy farmers who are young, educated, and managing dairy farms with large herd sizes hold positive attitudes toward E-extension. These farmers regularly seek online dairy-related guidance as well as regularly participate in different extension activities. This study concludes that establishing a hybrid framework incorporating E-extension methods with complementary face-to-face extension activities will help maintain a profitable and sustainable dairy industry in Tasmania.
On the evolution of the entropy and pressure profiles in X-ray luminous galaxy clusters at z > 0.4

Galaxy clusters are the most recent products of hierarchical accretion over cosmological scales. The gas accreted from the cosmic field is thermalized inside the cluster halo. Gas entropy and pressure are expected to have a self-similar behaviour with their radial distribution following a power law and a generalized Navarro-Frenk-White profile, respectively. This has been shown also in many different hydrodynamical simulations. We derive the spatially-resolved thermodynamical properties of 47 X-ray galaxy clusters observed with Chandra in the redshift range 0.4 0.75, where, in the central regions, we observe higher values of the entropy (by a factor of 2.2) and systematically lower estimates (by a factor of 2.5) of the pressure. The effective polytropic index, which retains informations about the thermal distribution of the gas, shows a slight linear positive evolution with the redshift and the concentration of the dark matter distribution. A prevalence of non-cool-core, disturbed systems, as we observe at higher redshifts, can explain such behaviours.
Lattice study of conformal behavior in SU(3) Yang-Mills theories

Using lattice simulations, we study the extent of the conformal window for an SU(3) gauge theory with N{sub f} Dirac fermions in the fundamental representation. We extend our recently reported work, describing the general framework and the lattice simulations in more detail. We find that the theory is conformal in the infrared for N{sub f}=12, governed by an infrared fixed point, whereas the N{sub f}=8 theory exhibits confinement and chiral symmetry breaking. We therefore conclude that the low end of the conformal window N{sub f}{sup c} lies in the range 8{<=}N{sub f}{sup c}{<=}12. We discuss open questions and the potential relevance of the present work to physics beyond the standard model.
Influence of Different Immunostimulants on Growth, Serological Response and Histological Changes of Newcastle Disease Virus-vaccinated Chicks

Newcastle disease (ND) vaccination was targeted to reduce mortality, viral load in the environment, and eradication of positive cases. Many immunostimulants have been used to improve the immune response of vaccinated chickens. The current study was designed to compare the effect of different immunostimulants on immune response of NDV vaccinated chicks. A total of 150 one-day old Cobb chicks were divided into 5 equal groups. Group 1 was lifted as non-vaccinated negative control, whereas other groups were vaccinated against NDV. The used immune stimulants under test were given to groups 3, 4, and 5 as follows N. sativa 6%, curcumin1%, and orego sol. respectively at 7 th day old continuously till the end of experiment. The results showed high antibody titers, low mortality rates and better body performance in the groups treated with these immunostimulants than the other groups. However, chicks treated with N. sativa showed renal water cyst formation compared with other groups. In conclusion, application of immunostimulants can stimulate the immune response and reduce the pathogenicity of ND in chickens.