Miracle-dz/UniFAR-FTUs huggingface dataset:
Teacher collaboration: Significant influence on self-efficacy of secondary school teachers

Teacher collaboration is an aspect that needs to be given due attention in the educational institutions in order to sustain the improvement of teachers’ learning. This study was conducted to examine the influence of secondary school teacher’s collaboration on their self-efficacy. Research design was based on quantitative approach by cross-sectional survey. Data collection via questionnaires was performed to obtain demographic information of respondents, as well as data on teacher collaboration and self-efficacy. A number of 410 secondary school teachers in the northern part of peninsular Malaysia were involved in the study as survey respondents. The collected data was processed and analyzed using statistical package for the social sciences (SPSS) via frequency, mean, standard deviation, Pearson correlation and multiple regression analysis. The study found that the level of teacher collaboration and teachers’ self-efficacy among secondary school teachers is high. The findings also discovered that there was positive relationship between teacher collaboration and teachers’ self-efficacy. In addition, the dimension of teacher collaboration was found to have a significant influence on the teachers’ self-efficacy. Thus, the findings clearly indicated the importance of the collaboration practices between teachers in influencing the self-efficacy of teachers.
ON THE STAR FORMATION RATES IN MOLECULAR CLOUDS

In this paper, we investigate the level of star formation activity within nearby molecular clouds. We employ a uniform set of infrared extinction maps to provide accurate assessments of cloud mass and structure and compare these with inventories of young stellar objects within the clouds. We present evidence indicating that both the yield and rate of star formation can vary considerably in local clouds, independent of their mass and size. We find that the surface density structure of such clouds appears to be important in controlling both these factors. In particular, we find that the star formation rate (SFR) in molecular clouds is linearly proportional to the cloud mass (M0.8) above an extinction threshold of AK≈ 0.8 mag, corresponding to a gas surface density threshold of Σgas ≈ 116 M☉ pc2. We argue that this surface density threshold corresponds to a gas volume density threshold which we estimate to be n(H2) ≈ 104 cm−3. Specifically, we find SFR (M☉ yr−1) = 4.6 ± 2.6 × 10−8 M0.8 (M☉) for the clouds in our sample. This relation between the rate of star formation and the amount of dense gas in molecular clouds appears to be in excellent agreement with previous observations of both galactic and extragalactic star-forming activity. It is likely the underlying physical relationship or empirical law that most directly connects star formation activity with interstellar gas over many spatial scales within and between individual galaxies. These results suggest that the key to obtaining a predictive understanding of the SFRs in molecular clouds and galaxies is to understand those physical factors which give rise to the dense components of these clouds.
The polar wind of the fast rotating Be star Achernar. VINCI/VLTI interferometric observations of an

Be stars show evidence of mass loss and circumstellar envelopes (CSE), from UV resonance lines, near-IR excesses and the presence of episodic hydrogen emission lines. The geometry of these envelopes is still uncertain, though it is often assumed that they are formed by a disk around the stellar equator and a hot polar wind. We probe the close environment of the fast rotating Be star Achernar at angular scales of a few mas in the infrared, in order to constrain the geometry of a possible polar CSE. We obtained long-baseline interferometric observations of Achernar with the VINCI/VLTI beam combiner in the $H$ and $K$ bands, using various telescope configurations and baseline lengths with a large azimuthal coverage. The observed visibility measurements along the polar direction are significantly lower than the visibility function of the photosphere of the star alone, in particular at low spatial frequencies. This points at the presence of an asymmetric diffuse CSE elongated along the polar direction of the star. We fit to our data a simple model consisting of two components: a 2D elliptical Gaussian superimposed on a uniform ellipse representing the distorted photosphere of the fast rotating star. We clearly detect a CSE elongated along the polar axis of the star, as well as the rotational flattening of the stellar photosphere. The relative near-IR flux measured for the CSE compared to the stellar photosphere is 5\%. Its angular dimensions are loosely constrained by the available data$2.7 \pm 1.3$ mas and $17.6 \pm 4.9$ mas. This CSE could be linked to free-free emission from the radiative pressure driven wind originating from the hot polar caps of the star.
Spiropyran/Merocyanine Amphiphile in Various Solvents: A Joint Experimental–Theoretical Approach to Photophysical Properties and Self-Assembly

This joint experimental-theoretical work focuses on molecular and photophysical properties of the spiropyran-containing amphiphilic molecule in organic and aqueous solutions. Being dissolved in tested organic solvents, the system demonstrates positive photochromism, i.e., upon UV stimulus the colorless spiropyran form is transformed into colorful merocyanine isomer. However, the aqueous solution of the amphiphile possesses a negative photochromism: the orange-red merocyanine form becomes thermodynamically more stable in water, and both UV and vis stimuli lead to the partial or complete photobleaching of the solution. The explanation of this phenomenon is given on the basis of density functional theory calculations and classical modeling including thermodynamic integration. The simulations reveal that stabilization of merocyanine in water proceeds with the energy of ca. 70 kJ mol−1, and that the Helmholtz free energy of hydration of merocyanine form is 100 kJ mol−1 lower as compared to the behavior of SP isomer in water. The explanation of such a difference lies in the molecular properties of the merocyanine: after ring-opening reaction this molecule transforms into a zwitterionic form, as evidenced by the electrostatic potential plotted around the opened form. The presence of three charged groups on the periphery of a flat conjugated backbone stimulates the self-assembly of merocyanine molecules in water, ending up with the formation of elongated associates with stack-like building blocks, as shown in molecular dynamics simulations of the aqueous solution with the concentration above critical micelle concentration. Our quantitative evaluation of the hydrophilicity switching in spiropyran/merocyanine containing surfactants may prompt the search for new systems, including colloidal and polymeric ones, aiming at remote tuning of their morphology, which could give new promising shapes and patterns for the needs of modern nanotechnology.
Electric-field control and adiabatic evolution of shallow donor impurities in silicon

We present a tight-binding study of donor impurities in Si, demonstrating the adequacy of this approach for this problem by comparison with Kohn-Luttinger effective mass theory and experimental results. We consider the response of the system to an applied electric field: donors near a barrier material and in the presence of a uniform electric field may undergo two different ionization regimes according to the distance of the impurity to the Si/barrier interface. We show that for impurities ∼5 nm below the barrier, adiabatic ionization is possible within switching times of the order of one picosecond, while for impurities ∼ 10 nm or more below the barrier, no adiabatic ionization may be carried out by an external uniform electric field. Our results are discussed in connection with proposed Si:P quantum computer architectures.
Maximal incompatibility of locally classical behavior and global causal order in multiparty scenarios

Quantum theory in a global space-time gives rise to non-local correlations, which cannot be explained causally in a satisfactory way; this motivates the study of theories with reduced global assumptions. Oreshkov, Costa, and Brukner (2012) proposed a framework in which quantum theory is valid locally but where, at the same time, no global space-time, i.e., predefined causal order, is assumed beyond the absence of logical paradoxes. It was shown for the two-party case, however, that a global causal order always emerges in the classical limit. Quite naturally, it has been conjectured that the same also holds in the multi-party setting. We show that counter to this belief, classical correlations locally compatible with classical probability theory exist that allow for deterministic signaling between three or more parties incompatible with any predefined causal order.
A TALE OF A RICH CLUSTER AT z ∼ 0.8 AS SEEN BY THE STAR FORMATION HISTORIES OF ITS EARLY-TYPE GALAXIES

We present a detailed stellar population analysis for a sample of 24 early-type galaxies (ETGs) belonging to the rich cluster RX J0152.7-1357 at z = 0.83. We have derived the age, metallicity, abundance pattern, and star formation history (SFH) for each galaxy individually to further characterize this intermediate-z reference cluster. We then study how these stellar population parameters depend on the local environment. This provides a better understanding on the formation timescales and subsequent evolution of the substructures in this cluster. We have also explored the evolutionary link between z ∼ 0.8 ETGs and those in the local universe by comparing the trends that the stellar population parameters followed with galaxy velocity dispersion at each epoch. We find that the ETGs in Coma are consistent with being the (passively evolving) descendants of the ETG population in RX J10152.7-1357. Furthermore, our results favor a downsizing picture, where the subclumps centers were formed first. These central parts contain the most massive galaxies, which formed the bulk of their stars in a short, burst-like event at high z. On the contrary, the cluster outskirts are populated with less-massive, smaller galaxies that show a wider variety of SFHs. In general, they present extended star formation episodes over cosmic time, which seems to be related to their posterior incorporation into the cluster around 4 Gyr after the initial event of formation.
On the stability of solitary waves with decaying oscillatory tails

In dispersive wave systems with dispersion relations such that the phase speed attains an extremum at a finite wavenumber, a rich variety of solitary waves that feature decaying oscillatory tails is known to arise. Here we use the fifth–order Korteweg–de Vries (KdV) equation, a model for small–amplitude gravity–capillary waves on water of finite depth when the Bond number is close to ⅓ to examine the stability of the two symmetric solitary–wave solution branches that bifurcate at the minimum phase speed. In the vicinity of the bifurcation point, these solitary waves take the form of modulated wave packets with envelopes that can be approximated by the same soliton solution of the nonlinear Schrodinger (NLS) equation, suggesting that both branches would be stable in the small–amplitude limit. It is shown, however, that the branch of the so–called elevation waves is unstable while the branch of depression waves is stable, consistent with numerical results. The coupling between the carrier oscillations and their envelope, an effect beyond all orders of the expansion underlying the NLS equation, is essential to this behaviour: the dimensionless growth rates of the instability modes found for elevation waves are exponentially small with respect to the solitary–wave steepness. The asymptotic procedure followed here would be useful in discussing the stability of solitary waves with decaying oscillatory tails in other settings as well, and details are worked out for a nonlinear beam equation and a modified fifth–order KdV equation.
The Influence of Ability, Work Discipline, and Work Motivation on Employee Performance (Study on Honorary Employees at the Department of Transportation of the City of Binjai)

This research was conducted to find the effect of ability, work discipline, and work motivation on the performance of honorary employees at the Department of Transportation of Binjai City. The population in this research amounted to 45 honorary employees. The number of samples also took as many as 45 honorary employees as respondents. The sampling technique used was saturated sampling. This research used primary data in the type of quantitative data collected through questionnaires and processed using the SPSS 24.0 application. The research was conducted from September 2021 - February 2022. The analytical technique used was using multiple linear regression models. The results showed that the ability, work discipline, and work motivation both partially and simultaneously had a positive and significant effect on the performance of honorary employees at the Department of Transportation of Binjai City. The most dominant variable affecting the performance of honorary employees was the work motivation variable with the largest tcount of 3,715. In addition, 87.8% of employee performance can be explained and obtained from ability, work discipline, and work motivation, while the rest was obtained from other factors. Employee performance has a very strong relationship to ability, work discipline, and work motivation.
A Comprehensive Review of Map-Matching Techniques: Empirical Analysis, Taxonomy, and Emerging Research Trends

The map matching method gets simpler with higher precision positioning systems, but because the positioning framework is still not sufficiently precise or too costly for marginal map matching in practice, it is still a hot research domain. Several researchers have worked on map-matching methods and reported their finding of in-depth studies of domain. This literature review provides extensive information on the above map-matching methods related to digital maps with respect to convergence and outline the problems, information sources, as well as future demands identified by industry/society. It focuses on past research work approaches, implementations, capabilities, and their weaknesses using linear search and citation chaining. Finally, this work concludes with recommendations of the future direction of research and ideas to develop new algorithms for advanced applications.
The Institution's Knowledge: Congressional Staff Experience and Committee Productivity

Congressional staff have often been called the “invisible force” behind members of Congress, earning themselves the title of “unelected lawmakers. ” in this paper, i explore the link between united states senate committees’ level of productivity and the experience of their staff. utilizing publicly reported data on senate staff experience and a new measure of committee productivity i find that a committee’s average years of staff experience is a significant predictor of committee legislative effectiveness. i find, however, that greater levels of staff experience only increase committee effectiveness when assessing the experience of senior or highranking staff. as nonsenior staff experience increases, however, committees become less effective. these findings suggest that when making hiring decisions, senate chairs and ranking members should prioritize years of experience in their senior staff while foregoing experienced general and administrative staff in order to achieve greater levels of committee productivity.
The impact of rotation on turbulent tidal friction in stellar and planetary convective regions

Context. Turbulent friction in convective regions in stars and planets is one of the key physical mechanisms that drive the dissipation of the kinetic energy of tidal flows in their interiors and the evolution of their systems. This friction acts both on the equilibrium/non-wave-like tide and on tidal inertial waves in these layers. Aims. It is thus necessary to obtain a robust prescription for this friction. In the current state-of-the-art, it is modelled by a turbulent eddy-viscosity coefficient, based on mixing-length theory, applied to tide velocities. However, none of the current prescriptions take into account the action of rotation that can strongly affect turbulent convection. Therefore, a new prescription that takes this into account must be derived. Methods. We use theoretical scaling laws for convective velocities and characteristic lengthscales in rotating stars and planets that have been recently confirmed by 3D high-resolution non-linear Cartesian numerical simulations to derive the new prescription. A corresponding local model of tidal waves is used to understand the consequences for the linear tidal dissipation. Finally, new grids of rotating stellar models and published values of planetary convective Rossby numbers are used to discuss astrophysical consequences. Results. The action of rotation on convection deeply modifies the turbulent friction applied on tides. In the regime of rapid rotation (with a convective Rossby number below 0.25), the eddy-viscosity may be decreased by several orders of magnitude. It may lead to a loss of efficiency of the viscous dissipation of the equilibrium tide and to a more efficient complex and resonant dissipation of tidal inertial waves in the bulk of convective regions. Conclusions. To understand the complete evolution of planetary systems, tidal friction in rapid rotators such as young low-mass stars, giant and Earth-like planets must be evaluated. Therefore, we need a completely coupled treatment of the tidal evolution of star-planet systems and multiple stars, and of the rotational evolution of their components with a coherent treatment of the variations of tidal flows, and of their dissipation as a function of rotation.
INFRARED OBSERVATIONS OF THE QUINTUPLET PROPER MEMBERS USING SOFIA/FORCAST AND GEMINI/TReCS

Since their discovery, the Quintuplet proper members (QPMs) have been somewhat mysterious in nature. Originally dubbed the “cocoon stars” due to their cool featureless spectra, high-resolution near-infrared imaging observations have shown that at least two of the objects exhibit “pinwheel” nebulae consistent with binary systems with a carbon-rich Wolf–Rayet star and O/B companion. In this paper, we present 19.7, 25.2, 31.5, and 37.1 μm observations of the QPMs (with an angular resolution of 3.2″–3.8″) taken with the Faint Object Infrared Camera for the SOFIA Telescope (FORCAST) in conjunction with high-resolution (∼0.1″–0.2″) images at 8.8 and 11.7 μm from the Thermal-Region Camera Spectrograph (TReCS). DUSTY models of the thermal dust emission of two of the four detected QPMs, Q2 and Q3, are fitted by radial density profiles that are consistent with constant mass-loss rates ( ). For the two remaining sources, Q1 and Q9, extended structures (∼1″) are detected around these objects in high-resolution imaging data. Based on the fitted dust masses, Q9 has an unusually large dust reservoir ( ) compared to typical dusty Wolf–Rayet stars, which suggests that it may have recently undergone an episode of enhanced mass loss.
EXPANDING SHELL AND STAR FORMATION IN THE INFRARED DUST BUBBLE N6

We have carried out a multiwavelength study of the infrared dust bubble N6 to extensively investigate the molecular environs and star-forming activities therein. Mapping observations in 12CO J = 1–0 and 13CO J = 1–0 performed with the Purple Mountain Observatory 13.7 m telescope have revealed four velocity components. Comparison between distributions of each component and the infrared emission suggests that three components are correlated with N6. There are 10 molecular clumps detected. Among them, five have reliable detections in both 12CO and 13CO and have similar LTE and non-LTE masses ranging from 200 to higher than 5000 M☉. With larger gas masses than virial masses, these five clumps are gravitationally unstable and have the potential to collapse to form new stars. The other five clumps are only reliably detected in 12CO and have relatively small masses. Five clumps are located on the border of the ring structure, and four of them are elongated along the shell. This is well in agreement with the collect-and-collapse scenario. The detected velocity gradient reveals that the ring structure is still under expansion owing to stellar winds from the exciting star(s). Furthermore, 99 young stellar objects (YSOs) have been identified based on their infrared colors. A group of YSOs reside inside the ring, indicating active star formation in N6. Although no confirmative features of triggered star formation are detected, the bubble and the enclosed H ii region have profoundly reconstructed the natal cloud and altered the dynamics therein.
On redundancy and untestability in sequential circuits

This research addresses the problems of identifying redundancy and untestability in synchronous sequential circuits. The widespread misconceptions about redundancy are revealed and examples are provided to illustrate the differences between untestability and redundancy in sequential circuits. Existing techniques to identify sequential redundancy are discussed, and it is shown that some of these methods are based on incorrect theoretical results. Specifically, it is shown that untestable faults in balanced pipeline circuits and in circuits with fault-free global reset mechanisms are not necessarily redundant, and that a constant function does not always indicate a redundancy. It is also shown that adding a global reset mechanism or retiming synchronous circuitry may introduce redundancies. The first efficient algorithm (FIRES) to identify sequential redundancy, that is practical for large circuits is presented. No global reset is assumed and no state transition information is required. The concept of a c-cycle redundancy as a generalization of the conventional notion of sequential redundancy is introduced. FIRES is based on the result that a fault which requires a conflict as a necessary condition for its detection is c-cycle redundant. FIRES has provably polynomial-time complexity, but is not guaranteed to identify all redundancies in a circuit. Experimental results on benchmark circuits indicate that FIRES finds a large number of redundancies. When a sequential test generator targets a sequentially redundant fault, the most it can do is prove it as untestable. It is shown that, in general, the redundant faults identified by FIRES are not easy targets for state-of-the-art sequential test generators. Another algorithm, FUNI, to find untestable faults using illegal states is also introduced. FUNI uses the illegal states identified by a recently proposed algorithm, FILL, and finds untestable faults for which these illegal states are necessary for detection. FUNI identifies untestable faults without using the exhaustive search involved in ATG. Results show that FUNI finds a large number of untestable faults up to several orders of magnitude faster than an ATG algorithm that targeted the faults identified by FUNI. Also, many untestable faults identified by FUNI were aborted by the test generator.
Large grains can grow in circumstellar discs

Abstract We perform coagulation & fragmentation simulations to understand grain growth in T Tauri & brown dwarf discs. We present a physically-motivated approach using a probability distribution function for the collision velocities and separating the deterministic & stochastic velocities. We find growth to larger sizes compared to other models. Furthermore, if brown dwarf discs are scaled-down versions of T Tauri discs (in terms of stellar & disc mass, and disc radius), growth at the same location with respect to the outer edge occurs to similar sizes in both discs.