Miracle-dz/UniFAR-FTUs huggingface dataset:
Second language psychological speaking and listening needs: Scale development, symbiosis, and demographic differences

This study aimed to develop and validate two parallel scales to measure the psychological L2 speaking and listening needs of 863 English-as-a-foreign language (EFL) learners. The associations between three psychological needs (i.e., autonomy, competence, and relatedness) of L2 speaking and of L2 listening were examined to develop insights into oracy (i.e., integration of speaking and listening) in L2 communication. Subsequently, the impact of demographic variables was explored. The data, collected via a 5-point Likert-scale questionnaire, were analyzed through descriptive and correlation analysis, factor analysis, and ANOVA. Exploratory factor analysis was conducted to determine the factor structures, followed by confirmatory factor analysis for validation. Results demonstrated that the validity and reliability of the two developed scales were satisfactory. L2 speaking autonomy was significantly related to L2 listening autonomy, as were competence and relatedness. The three psychological needs of both L2 speaking and listening revealed varying patterns in terms of gender, major, university geographical context, schooling stage (first year to fourth year), and study-abroad experiences. The research findings reinforce the need for integration of L2 speaking and L2 listening when satisfying university students’ psychological needs, contribute to the research field with the measurement scales of psychological needs in L2 speaking and listening settings, and yield implications for teaching the two language skills integratedly.
Effective Organization Strive to Focus on the Behavioral Patterns of Their Employed

Effective organizations strive to focus on the behavioral patterns of their employees. They are designed to develop human behaviors that are best suited for the effectiveness of an organization. Organizational justice is one of the main key factor that invest in developing a positive behavior of the employees towards their organization as well as their colleagues that in turn add up to the effectiveness of an organization. This research extracts the theoretical support from equity theory of Adam smith, Justice judgmental Model theory of Leventhal, Social Exchange theory of George Homan and Social System theory of Chester Bernard. The study is intended to empirically assess the impacts of organizational justice on organizational effectiveness with a mediating role of organization citizenship behavior in higher education institutions of Pakistan. The researchers suggests that criteria of effectiveness in institutions is the same as that of an organization. Using positivists’ approach 313 questionnaires were distributed in academic staff of five different universities located in the federal territory of Islamabad. Collected data was analyzed both in descriptive and inferential manner with appropriate statistical tools through statistical package for social sciences software SPSS version 22. The mediating role of Organization Citizenship Behavior was checked through Baron and Kenny four step model for mediation. This research has contributed towards the theory as well as given a practical insight into the institutional effectiveness. In the research data is collected from the faculty members from of different universities namely, International Islamic University Islamabad, Quaid e Azam University Islamabad, COMSATS Islamabad, National University of Modern Languages NUML Islamabad, and National University of Computer and Emerging Sciences FAST Islamabad campus. The results of the research shows that organizational justice is an important aspect that contribute towards the organization citizenship behavior. Organization citizenship behavior is the fundamental contributor towards the Organizational Effectiveness in higher education institutions of Pakistan.
On the properties of the interstellar medium in extremely metal-poor blue compact dwarf galaxies GMOS-IFU spectroscopy and SDSS photometry of the double-knot galaxy HS 2236+1344

Aims. The main goal of this study is to carry out a spatially resolved investigation of the warm interstellar medium (ISM) in the extremely metal-poor blue compact dwarf (BCD) galaxy HS 2236+1344. Special emphasis is laid on analysis of the spatial distribution of chemical abundances, emission-line ratios, and the kinematics of the ISM, and to the recent star-forming (SF) activity in this galaxy. Methods. This study is based on optical integral field unit spectroscopy data from Gemini Multi-Object Spectrograph (GMOS) at the Gemini North telescope and archival Sloan Digital Sky Survey (SDSS) images. The galaxy was observed at medium spectral resolution over the spectral range from ∼4300 A to 7300 A. The data were obtained in two different positions across the galaxy, obtaining a total 4 �� × 8 �� field that encompasses most of its ISM. Results. Emission-line maps and broad-band images obtained in this study indicate that HS 2236+1344 hosts three giant H ii regions (GH iiRs). Our data also reveal some faint curved features in the BCD periphery that might be due to tidal perturbations or expanding ionized-gas shells. The ISM velocity field shows systematic gradients along the major axis of the BCD, with its southeastern and northwestern half differing by ∼80 km s −1 in their recessional velocity over the field of view. The Hα and Hβ equivalent-width distribution in the central part of HS 2236+1344 is consistent with a very young (∼3 Myr) burst. Our surface photometry analysis reveals an underlying low surface brightness component with moderately red colors, which suggest that the galaxy has undergone previous star formation. We derive an integrated oxygen abundance of 12 + log(O/H) = 7.53 ± 0.06 and a nitrogen-to-oxygen ratio of log(N/O) = −1.57 ± 0.19. Our results are consistent, within the uncertainties, with a homogeneous distribution of oxygen and nitrogen within the ISM of the galaxy. The high-ionization He ii λ4686 emission line is detected only in the central part of HS 2236+1344. Similar to many BCDs with He ii λ4686 emission, HS 2236+1344 shows no Wolf-Rayet (WR) bump.
Revised geometric estimates of the North Galactic Pole and the Sun's height above the Galactic mid-plane

Astronomers are entering an era of {\mu}as-level astrometry utilizing the 5-decade-old IAU Galactic coordinate system that was only originally defined to $\sim$0{\deg}. 1 accuracy, and where the dynamical centre of the Galaxy (Sgr A*) is located $\sim$0{\deg}. 07 from the origin. We calculate new independent estimates of the North Galactic Pole (NGP) using recent catalogues of Galactic disc tracer objects such as embedded and open clusters, infrared bubbles, dark clouds, and young massive stars. Using these catalogues, we provide two new estimates of the NGP. Solution 1 is an "unconstrained" NGP determined by the galactic tracer sources, which does not take into account the location of Sgr A*, and which lies 90{\deg}. 120$\,\pm\,$0{\deg}. 029 from Sgr A*, and Solution 2 is a "constrained" NGP which lies exactly 90{\deg} from Sgr A*. The "unconstrained" NGP has ICRS position: $\alpha_{NGP}$ = 192{\deg}. 729 $\,\pm\,$ 0{\deg}. 035, $\delta_{NGP}$ = 27{\deg}. 084 $\,\pm\,$ 0{\deg}. 023 and $\theta\,$ = 122{\deg}. 928 $\,\pm\,$ 0{\deg}. 016. The "constrained" NGP which lies exactly 90{\deg} away from Sgr A* has ICRS position: $\alpha_{NGP}$ = 192{\deg}. 728 $\,\pm\,$0{\deg}. 010, $\delta_{NGP}$ = 26{\deg}. 863 $\,\pm\,$ 0{\deg}. 019 and $\theta\,$ = 122{\deg}. 928 $\,\pm\,$ 0{\deg}. 016. The difference between the solutions is likely due to the Sun lying above the Galactic midplane. Considering the angular separation between Sgr A* and our unconstrained NGP, and if one adopts the recent estimate of the Galactocentric distance for the Sun of $R_{0}$ = 8.2$\,\pm\,$0.1 kpc, then we estimate that the Sun lies $z_{\odot}$ $\simeq$ 17$\,\pm\,$5 pc above the Galactic midplane. Our value of $z_{\odot}$ is consistent with the true median of 55 previous estimates published over the past century of the Sun's height above the Galactic mid-plane ($z_{\odot}$ $\simeq$ 17$\,\pm\,$2 pc).
Large solar-type magnetic reconnection model for magnetar giant flare

Abstract We construct a magnetic reconnection model for magnetar giant flare in the framework of solar flare/coronal mass ejection theory. As is the case with the solar flare, the explosive magnetic reconnection plays a crucial role in the energetics of the magnetar flare. A key physics controlling the energy transport in the system, on the other hand, is the radiative process unlike that in the solar flare. After the release of the magnetic energy via the magnetic reconnection, the radiative heat flux drives the baryonic evaporation. Our model can predict that the baryonic matter evaporated in the preflare stage would be the origin of the radio emitting ejecta observed in association with the giant flare on 2004 December 27 from SGR1806-20.
CGCG 292-057 - a radio galaxy with merger-modulated radio activity

We announce the discovery of a unique combination of features in a radio source identified with the merger galaxy CGCG 292−057. The radio galaxy both exhibits a highly complex, X-like structure and shows signs of recurrent activity in the form of double–double morphology. The outer lobes of CGCG 292−057 are characterized by low radio power, P1400 MHz≃ 2 × 1024 W Hz−1, placing this source below the FR II/FR I luminosity threshold, and are highly polarized (almost 20 per cent at 1400 MHz) as is typical of X-shaped radio sources. The host is a low-ionization nuclear emission-line region-type galaxy with a relatively low black hole mass and double-peaked narrow emission lines. These features make this galaxy a primary target for studies of merger-triggered radio activity.
Metals, dust and the cosmic microwave background: fragmentation of high-redshift star-forming clouds

We investigate the effects of the Cosmic Microwave Background (CMB) radiation field on the collapse of prestellar clouds. Using a semi-analytic model to follow the thermal evolution of clouds with varying initial metallicities and dust contents at different redshifts, we study self-consistently the response of the mean Jeans mass at cloud fragmentation to metal line-cooling, dust-cooling and the CMB. In the absence of dust grains, at redshifts z 6 10 moderate characteristic masses (of 10s of M⊙) are formed when the metallicity is 10 −4 Z⊙ 6 Z 6 10 −2.5 Z⊙; at higher metallicities, the CMB inhibits fragmentation and only very large masses (of � 100s of M⊙) are formed. These effects become even more dramatic at z > 10 and the fragmentation mass scales are always > 100s of M⊙, independent of the initial metallicity. When dust grains are present, sub-solar mass fragments are formed at any redshift for metallicities Z > 10 −6 Z⊙ because dust-cooling remains relatively insensitive to the presence of the CMB. When Z > 10 −3 Z⊙, heating of dust grains by the CMB at z > 5 favors the formation of larger masses, which become super-solar when Z > 10 −2 Z⊙ and z > 10. Finally, we discuss the implications of our result for the interpretation of the observed abundance patterns of very metal-poor stars in the galactic halo.
REVISITING THE SCALING RELATIONS OF BLACK HOLE MASSES AND HOST GALAXY PROPERTIES

New kinematic data and modeling efforts in the past few years have substantially expanded and revised dynamical measurements of black hole masses (M•) at the centers of nearby galaxies. Here we compile an updated sample of 72 black holes and their host galaxies, and present revised scaling relations between M• and stellar velocity dispersion (σ), V-band luminosity (L), and bulge stellar mass (Mbulge), for different galaxy subsamples. Our best-fitting power-law relations for the full galaxy sample are log10(M•) = 8.32 + 5.64log10(σ/200 km s−1), log10(M•) = 9.23 + 1.11log10(L/1011 L☉), and log10(M•) = 8.46 + 1.05log10(Mbulge/1011 M☉). A log-quadratic fit to the M•–σ relation with an additional term of β2 [log10(σ/200 km s−1)]2 gives β2 = 1.68 ± 1.82 and does not decrease the intrinsic scatter in M•. Including 92 additional upper limits on M• does not change the slope of the M•–σ relation. When the early- and late-type galaxies are fit separately, we obtain similar slopes of 5.20 and 5.06 for the M•–σ relation but significantly different intercepts—M• in early-type galaxies are about two times higher than in late types at a given sigma. Within early-type galaxies, our fits to M•(σ) give M• that is about two times higher in galaxies with central core profiles than those with central power-law profiles. Our M•–L and M•–Mbulge relations for early-type galaxies are similar to those from earlier compilations, and core and power-law galaxies yield similar L- and Mbulge-based predictions for M•. When the conventional quadrature method is used to determine the intrinsic scatter in M•, our data set shows weak evidence for increased scatter at Mbulge < 1011 M☉ or LV < 1010.3 L☉, while the scatter stays constant for 1011 < Mbulge < 1012.3 M☉ and 1010.3 < LV < 1011.5 L☉. A Bayesian analysis indicates that a larger sample of M• measurements would be needed to detect any statistically significant trend in the scatter with galaxy properties.
ON THE METALLICITY DISTRIBUTION OF THE PECULIAR GLOBULAR CLUSTER M22

In our previous study, we showed that the peculiar globular cluster (GC) M22 contains two distinct stellar populations, namely the Ca-w and Ca-s groups, which have different physical properties, chemical compositions, spatial distributions, and kinematics. We proposed that M22 was most likely formed via a merger of two GCs with heterogeneous metallicities in a dwarf galaxy environment and then later accreted to our Galaxy. In their recent study, Mucciarelli et al. claimed that M22 is a normal monometallic globular cluster without any perceptible metallicity spread among the two groups of stars, which challenges our results and those of others. We devise new strategies for the local thermodynamic equilibrium abundance analysis of red giant branch stars in GCs and show that there exists a spread in the iron abundance distribution in M22.
Perturbative stability along the supersymmetric directions of the landscape

We consider the perturbative stability of non-supersymmetric configurations in 𝒩=1 supergravity models with a spectator sector not involved in supersymmetry breaking. Motivated by the supergravity description of complex structure moduli in Large Volume Compactifications of type IIB-superstrings, we concentrate on models where the interactions are consistent with the supersymmetric truncation of the spectator fields, and we describe their couplings by a random ensemble of generic supergravity theories. We characterise the mass spectrum of the spectator fields in terms of the statistical parameters of the ensemble and the geometry of the scalar manifold. Our results show that the non-generic couplings between the spectator and the supersymmetry breaking sectors can stabilise all the tachyons which typically appear in the spectator sector before including the supersymmetry breaking effects, and we find large regions of the parameter space where the supersymmetric sector remains stable with probability close to one. We discuss these results about the stability of the supersymmetric sector in two physically relevant situations: non-supersymmetric Minkowski vacua, and slow-roll inflation driven by the supersymmetry breaking sector. For the class of models we consider, we have reproduced the regimes in which the KKLT and Large Volume Scenarios stabilise all supersymmetric moduli. We have also identified a new regime in which the supersymmetric sector is stabilised at a very robust type of dS minimum without invoking a large mass hierarchy.
Implementation of Mean of Maximum on Cigarette Smoke Control in a Room

Home automation is an IoT technology that has the ability to communicate between devices. This technology requires a method for making the decision process. Fuzzy logic method is a solution to this problem. Fuzzy Logic is a method that functions to replicate and run human knowledge to control a system. In fuzzy logic algorithm, there are three main processes, which are fuzzification, inference, and defuzzification. Defuzzification process requires a method to obtain the value of crisp solutions. One of the many methods is Mean of Maximum (MoM). MoM is an algorithm that calculates the average of fuzzy conclusions or outputs that have the highest degree. In this research, we apply the MoM method in the defuzzification process to build a smoke emission control system in a room using an exhaust fan. Wemos D1 mini is used as a controller and processor in the system. And using telegram chatbot for communication media between users and the system. There are 27 rules in this system with 100% functionality. This research topic is very useful to keep the air clean and fresh in the room and avoid the dangers of cigarette smoke that can damage health.
Motor Imagery and Sport Performance: A Systematic Review on the PETTLEP Model

The aim of this review is to critically analyze the evidence provided throughout the years regarding the application of motor imagery (MI) in sport performance, focusing on the PETTLEP approach. Among the different MI approaches, in fact, the PETTLEP model takes into account many different domains for increasing the performance of athletes. These domains include physical features, the environment, task-related aspects, timing, learning, emotion, and perspective.
The Theoretical Model of Decision-Making Behaviour Geospatial Analysis Using Data Obtained from the Games of Chess

The game of chess offers a conducive setting to explore basic cognitive processes, including decision-making. The game exercises analytical cause-and-effect thinking skills regardless of the level of play. Moreover, chess portals provide information on the chess games played and serve as a vast database. The numbers of games played thus have the potential to be analyzed comprehensively, including for purposes other than analyzing chess matches only. The primary objective of this study is to develop a methodology for using information obtained from chess games for geospatial social analysis. The assumption is that the methodology will allow for general geographical variation in personality inference in the future, relying on big data from chess databases. Future large-scale studies of the geographical differentiation of personality traits using the developed methodology may be applicable in a number of ways. The results can be used wherever cross-sectional social analyses are needed in the context of personality traits (decision-making) to better understand their geographical background. In turn, the geographical distribution of these traits is accompanied by a range of important social, educational, health, political and economic implications.
Prognostic Ability of Tumor Budding Outperforms Poorly Differentiated Clusters in Gastric Cancer

Simple Summary Small clusters of tumor cells at the invasion front of the tumor, known as “tumor budding” and larger clusters of cells, known as “poorly differentiated clusters”, are well known histological parameters to assess the outcome of colorectal cancer. However, their prognostic value for gastric cancer is less well investigated and controversial based on the studies conducted so far. In our retrospective study, we investigated the prognostic power of these two entities in a large cohort of gastric cancer patients. Our results demonstrate that tumor budding is an independent prognostic factor determining overall survival in gastric cancer, especially in intestinal type adenocarcinomas. In addition, budding can also predict the risk of lymph node metastases. However, although the trend is similar for poorly differentiated clusters, their predictive value is lower and they have not been shown to be an independent prognostic factor of survival in gastric cancer. Abstract The prognostic value of histological phenomena tumor budding (TB) and poorly differentiated clusters (PDCs) have been less studied in gastric cancer (GAC) and the data provided so far are controversial. In our study, 290 surgically resected GAC cases were evaluated for TB according to the criteria of International Tumor Budding Consensus Conference (ITBCC) and PDC, and both parameters were scored on a three-grade scale as described for colorectal cancer previously (0: Grade0, 1–4: Grade1, 5–9: Grade2 and ≥10: Grade3) and classified as low (Grade0–2) and high (Grade3) TB/PDC. High TB/PDC was associated with diffuse-type morphology, higher pT status, incomplete surgical resection, poor tumor differentiation and perineural and lymphovascular invasion. Multivariable survival analyses have shown an independent prognostic role of high TB with poorer overall survival in the total cohort (p = 0.014) and in intestinal-type adenocarcinomas (p = 0.005). Multivariable model revealed high TB as an independent predictor for lymph node metastasis in both the total cohort (p = 0.019) and in the intestinal type adenocarcinomas (p = 0.038). In contrast to tumor budding, no significant association was found between PDC and the occurrence of lymph node metastasis and tumor stage and even survival. In conclusion, tumor budding is an independent prognostic factor of survival in gastric cancer, especially in intestinal-type adenocarcinomas.
Effects of Support Ratio on the Perception of Illusory Contours, Brightness Enhancement, and Depth Stratification in Illusory Figures

For the stimulus inducing illusory figures support ratio is defined as the ratio of the diameter of an inducing element to the separation distance between the centers of the two nearest inducing elements. Shipley and Kellman (1992) reported that perceived magnitude of illusory contours for the stimuli of equal support ratio did not differ from the other even though the stimuli differed from one another in retinal size at support ratios of 0.5 and 0.8 and that it was larger for larger retinal size of the stimulus at support ratio of 0.3. This result suggests that perceived magnitude of illusory contours is scale invariant at higher support ratios and that it depends on retinal size of the stimulus at lower support ratios. In the present study we investigated the effects of retinal size of the stimulus of fixed support ratio on perceived magnitude of illusory contours, brightness enhancement, and depth stratification in illusory figures using families of congruent figures as stimuli. We found that perceived magnitude of them was independent of retinal size of the stimulus of fixed support ratio of 0.80 and that it was larger for larger retinal size of the stimulus at support ratios of 0.20 and 0.40. These results suggest that not only illusory contour formation but also illusory surface formation are scale invariant at higher support ratios and that they are facilitated by larger retinal size of the stimulus at lower support ratios. are closed region and are far more complex entities than the former (Gurnsey, Poirier, & Gascon, 1996).