Miracle-dz/UniFAR-FTUs huggingface dataset:
Aberration features in directional dark matter detection

The motion of the Earth around the Sun causes an annual change in the magnitude and direction of the arrival velocity of dark matter particles on Earth, in a way analogous to aberration of stellar light. In directional detectors, aberration of weakly interacting massive particles (WIMPs) modulates the pattern of nuclear recoil directions in a way that depends on the orbital velocity of the Earth and the local galactic distribution of WIMP velocities. Knowing the former, WIMP aberration can give information on the latter, besides being a curious way of confirming the revolution of the Earth and the extraterrestrial provenance of WIMPs. While observing the full aberration pattern requires extremely large exposures, we claim that the annual variation of the mean recoil direction or of the event counts over specific solid angles may be detectable with moderately large exposures. For example, integrated counts over Galactic hemispheres separated by planes perpendicular to Earth's orbit would modulate annually, resulting in Galactic Hemisphere Annual Modulations (GHAM) with amplitudes larger than the usual non-directional annual modulation.
The Galactic Center Molecular Cloud Survey. I. A Steep Linewidth-Size Relation & Suppression of Star Formation

The Central Molecular Zone (CMZ; inner $\sim{}200~\rm{}pc$) of the Milky Way is a star formation (SF) environment with very extreme physical properties. Exploration of SF in this region is important because (i) this region allows us to test models of star formation under exceptional conditions, and (ii) the CMZ clouds might be suitable to serve as templates to understand the physics of starburst galaxies in the nearby and the distant universe. For this reason we launched the Galactic Center Molecular Cloud Survey (GCMS), the first systematic study that resolves all major CMZ clouds at interferometer angular resolution (i.e., a few arc seconds). Here we present initial results based on observations with the Submillimeter Array (SMA) and the Atacama Pathfinder Experiment (APEX). Our study is complemented by dust emission data from the Herschel Space Telescope and a comprehensive literature survey of CMZ star formation activity. Our research reveals (i) an unusually steep linewidth-size relation, $\sigma(v)\propto{}r_{\rm{}eff}^{0.66\pm{}0.18}$, down to velocity dispersions $\sim{}0.6~\rm{}km\,s^{-1}$ at 0.1 pc scale. This scaling law potentially results from the decay of gas motions to transonic velocities in strong shocks. The data also show that, relative to dense gas in the solar neighborhood, (ii) star formation is suppressed by factors $\gtrsim{}10$ in individual CMZ clouds. This observation encourages exploration of processes that can suppress SF inside dense clouds for a significant period of time.
Positive Parity $D_s$ Mesons

We study the positive parity charmed strange mesons using lattice QCD, the only reliable ab initio method to study QCD at low energies. Especially the experimentally observed $$D_{s0}^*(2317)$$ and $$D_{s1}(2460)$$ have challenged theory for quite some time. The dynamical lattice QCD simulations are performed at two distinct pion masses, $$m_{\pi}$$ = 266 MeV and 156 MeV, using both $$\bar{c}s$$ as well as $DK$ and $D^*K$ scattering operators in the construction of the correlation matrix in order to take into the account threshold effects. While the $J^P = 0^+$ channel benefited most from the inclusion of scattering operators, it was also crucial for the case of the $$D_{s1}(2460)$$. Using the L\"uscher method, which relates the finite volume spectrum to the infinite volume scattering matrix, we were able to determine the near threshold behavior of the scattering amplitude. From it we extracted the binding momenta and the masses of the below-threshold bound states $$D_{s0}^*(2317)$$ and $$D_{s1}(2460)$$ by determining the pole positions of the scattering amplitudes. Our results compare well with experiment, resolving a long standing discrepancy between theory and experiment.
Decentralization, Budget Participation and Managerial Work Achievements

Research on decentralization and budget participation on managerial performance lately is a field of research that many have debates, thus attracting the interest of researchers to conduct further studies of the influence. The population in this study is the manager of the Company's manufacturing industry with sampling purposive sampling techniques. The analysis tool to test the hypothesis using simple regression analysis.Research generates Decentralization positive and significant impact on Managerial Performance. meaning that the higher the decentralization of the motivation of the manager with the unmet need for self-actualization. Participation Budget negative and significant effect on Managerial Performance. This means that in the preparation of the budget involved some employees may of them have properties that are less concerned about the budget so that less cooperative.
Flow-Induced Vibrations of Two Flexible Tubes in Cross Flow

Abstract To further investigate fluid-structure–interaction problems that occur in the nuclear field such as the behavior of pressurized water reactor fuel rods, steam generator tubes, and other heat exchanger tubes, the flow-induced vibrations of two flexible tubes in tandem, side-by-side, and in staggered arrangements are investigated. First, a three-dimensional numerical model for fluid-structure interaction of flexible tubes in cross flow is developed. It is a three-dimensional fully coupled approach with solving the fluid flow and the structure vibration simultaneously. Second, results are presented in the form of force coefficients, dynamic response, trajectories, and wake vortex pattern. The effects of pitch ratio, tube arrangement, and flow velocity on the vibration response and the flow field characteristic are investigated. Critical pitch and critical velocity are obtained successfully. The critical velocity depends heavily on pitch ratio. Under the same pitch ratio and velocity, the side-by-side tubes have the maximum value of fluid force and vibration amplitude, followed by the staggered tubes the and tandem tubes in sequence. The trajectory and wake vortex pattern are highly dependent on tube arrangement, pitch ratio, and flow velocity.
On the contribution of classical novae to the $^{26}$Al content of the Galaxy

A comparative analysis of the various scenarios proposed to xplain the26Al content of the galaxy, as observed through its characterisitc γ-ray line at 1.8 MeV, is presented. We include some suggestions about how theoretical yields should be handled, ac counting for the influence of the initial metallicity of the corresponding star, which depends not on ly its mass but also on its location in the galaxy. A code of chemical evolution of the galaxy is us ed to derive the temporal evolution of metallicity along the galaxy, the necessary tool to deter mine the initial metallicity of any stellar source of26Al. The contribution of each scenario (AGB stars, massive st ars and classical novae) and its range of uncertainty are described.
The effect of organizational culture transformation and talent management on organizational effectiveness mediated by job satisfaction

This study aims to determine the effect of Organizational Culture Transformation and Talent Management on Organizational Effectiveness mediated by Work. This research is based on organizational effectiveness in companies that have changed strategy due to encouragement from external industry factors so that organizational culture and talent management need to be carried out which are expected to increase organizational effectiveness. organization. The sample in this study was taken using a data collection method called purposive sampling. The sample used was 80 respondents. Data analysis using PLS (Partial Least Square) analysis technique through SmartPLS software. In addition, to test the hypothesis and the seventh, a trial was conducted to test the mediating/intervention variable in the hypothesis. The results showed that organizational culture transformation had a positive but not significant effect on organizational effectiveness. Furthermore, talent management has a positive and significant effect on organizational effectiveness. The results also show that the transformation of organizational culture and talent management has a positive but not significant effect on organizational effectiveness through job satisfaction owned by employees of PT. XYZ.
SUPERNOVAE AND AGN DRIVEN GALACTIC OUTFLOWS

We present analytical solutions for winds from galaxies with a Navarro–Frank–White (NFW) dark matter halo. We consider winds driven by energy and mass injection from multiple supernovae (SNe), as well as momentum injection due to radiation from a central black hole. We find that the wind dynamics depends on three velocity scales: (1) describes the effect of starburst activity, with as energy and mass injection rate in a central region of radius R; (2) v• ∼ (GM•/2R)1/2 for the effect of a central black hole of mass M• on gas at distance R; and (3) , which is closely related to the circular speed (vc) for an NFW halo, where rs is the halo scale radius and is a function of the halo concentration parameter. Our generalized formalism, in which we treat both energy and momentum injection from starbursts and radiation from the central active galactic nucleus (AGN), allows us to estimate the wind terminal speed to be (4v2⋆ + 6(Γ − 1)v•2 − 4v2s)1/2, where Γ is the ratio of force due to radiation pressure to gravity of the central black hole. Our dynamical model also predicts the following: (1) winds from quiescent star-forming galaxies cannot escape from 1011.5 M☉ ⩽ Mh ⩽ 1012.5 M☉ galaxies; (2) circumgalactic gas at large distances from galaxies should be present for galaxies in this mass range; (3) for an escaping wind, the wind speed in low- to intermediate-mass galaxies is ∼400–1000 km s−1, consistent with observed X-ray temperatures; and (4) winds from massive galaxies with AGNs at Eddington limit have speeds ≳ 1000 km s−1. We also find that the ratio [2v2⋆ − (1 − Γ)v•2]/v2c dictates the amount of gas lost through winds. Used in conjunction with an appropriate relation between M• and Mh and an appropriate opacity of dust grains in infrared (K band), this ratio has the attractive property of being minimum at a certain halo mass scale (Mh ∼ 1012–1012.5 M☉) that signifies the crossover of AGN domination in outflow properties from starburst activity at lower masses. We find that stellar mass for massive galaxies scales as M⋆∝M0.26h, and for low-mass galaxies, M⋆∝M5/3h.
Continuous-wave backward frequency doubling in periodically poled lithium niobate

We report on backward second-harmonic-generation in bulk periodically poled congruent lithium niobate with a 3.2 μm period. A tunable continuous-wave Ti:sapphire laser allowed us exciting two resonant quasi-phase-matching orders in the backward configuration. The resonances were also resolved by temperature tuning and interpolated with standard theory to extract relevant information on the sample.
MOBA Games in EFL Educational Settings For Intercultural Language Teaching

This paper unveils the relative merits of multiplayer online battle arena (MOBA) games in EFL educational settings for educational purposes, particularly rechecking the influence of League of Legends (LoL) on the EFL learners’ ICC. We have used Byram’s (1997) Model as a framework of assessment for thematic analysis, and both the Cultural Intelligence Scale (CQS), modified by Gozzoli and Gazzaroli (2018) and the Assessment of Intercultural Competence of Chinese College Students (AIC-CCS) by Wu et al. (2013) to ensure a consistent questionnaire. Our participants were 75 Algerian EFL learners (Males=86,7%, Females= 13,3%) from different educational levels, aged 20.08 (SD= 2.99). The results indicate a need to design a more convenient MOBA game as a replace for LoL, as well as adopting a flexible assessment continuous guidance to ensure appropriate ICC instruction.
Discovery of an overlapping cluster in the Abell 1674 field with Suzaku

We present the results of a Suzaku observation of Abell 1674, an optically very rich (richness class 3) cluster cataloged as z = 0.1066. We discover the He-like Fe K-shell line from the central region for the first time, and find that the X-ray spectrum yields a high redshift of 0.215^{+0.007}_{-0.006}. On the other hand, the spectrum of the southwestern region is fitted with a redshift of 0.11 \pm 0.02 by the He-like Fe L-shell lines, consistent with the optically determined value. The gas temperature, metal abundance, and core radius of the X-ray emission in the central region are 3.8 \pm 0.2 keV, 0.20 \pm 0.05 Z_solar and 450 \pm 40 kpc, respectively, while those in the southwestern region are 2.0 \pm 0.2 keV, 0.41^{+0.17}_{-0.13} Z_solar and 220^{+90}_{-70} kpc, respectively. These parameters are typical for clusters. We thus conclude that Abell 1674 consists of two independent clusters, A1674-C at z ~0.22 and A1674-SW at z ~0.11, overlapping along the line of sight. The X-ray luminosities of A1674-C within r = 2 Mpc is 15.9 \pm 0.6 \times 10^{43} erg s^{-1} in the 0.1-2.4 keV energy band, while that for A1674-SW is 1.25 \pm 0.07 \times 10^{43} erg s^{-1}. Both are consistent with those expected from the L-T relation of clusters within a factor of 2. This is another support for our conclusion.
Nearring Ideals, Graphs and Cliques

In this paper, we dene the notion of fuzzy graph of a nearring N with respect to a level ideal t denoted by (N;;;t ). The primary aim of this notion is to depict graphically the fuzzy character which is concealed algebraically in the examples of 3-prime fuzzy ideals of a nearring N. We nd that if N is a zero-symmetric nearring and is 3prime fuzzy ideal of N, then (N;;;t ) has a special type of symmetry. We call this symmetry as the ideal symmetry of (N;;;t ). We nd the conditions under which the ideal symmetry of (N;;;t ) implies is a 3-prime fuzzy ideal of N. Finally, we obtain a result which nds all the fuzzy cliques of (N;;;t ) whenever is 3-prime and N is zerosymmetric.
COLD FRONTS AND GAS SLOSHING IN GALAXY CLUSTERS WITH ANISOTROPIC THERMAL CONDUCTION

Cold fronts in cluster cool cores should be erased on short timescales by thermal conduction, unless protected by magnetic fields that are “draped” parallel to the front surfaces, suppressing conduction perpendicular to the sloshing fronts. We present a series of MHD simulations of cold front formation in the core of a galaxy cluster with anisotropic thermal conduction, exploring a parameter space of conduction strengths parallel and perpendicular to the field lines. Including conduction has a strong effect on the temperature distribution of the core and the appearance of the cold fronts. Though magnetic field lines are draping parallel to the front surfaces, preventing conduction directly across them, the temperature jumps across the fronts are nevertheless reduced. The geometry of the field is such that the cold gas below the front surfaces can be connected to hotter regions outside via field lines along directions perpendicular to the plane of the sloshing motions and along sections of the front that are not perfectly draped. This results in the heating of this gas below the front on a timescale of a Gyr, but the sharpness of the density and temperature jumps may nevertheless be preserved. By modifying the gas density distribution below the front, conduction may indirectly aid in suppressing Kelvin–Helmholtz instabilities. If conduction along the field lines is unsuppressed, we find that the characteristic sharp jumps seen in Chandra observations of cold front clusters do not form. Therefore, the presence of cold fronts in hot clusters is in contradiction with our simulations with full Spitzer conduction. This suggests that the presence of cold fronts in hot clusters could be used to place upper limits on conduction in the bulk of the intracluster medium. Finally, the combination of sloshing and anisotropic thermal conduction can result in a larger flux of heat to the core than either process in isolation. While still not sufficient to prevent a cooling catastrophe in the very central (r ∼ 5 kpc) regions of the cool core (where something else is required, such as active galactic nucleus feedback), it reduces significantly the mass of gas that experiences a cooling catastrophe outside those small radii.
A Spectroscopic Search for High Mass X-ray Binaries in M31

We present new optical spectroscopy of 20 candidate counterparts of 17 X-ray sources in the direction of the M31 disc. By comparing the X-ray catalogue from the XMMNewton survey of M31 with star catalogues from the Local Group Galaxy Survey, we chose counterpart candidates based on optical colour and X-ray hardness. We have discovered 17 counterpart candidates with spectra containing stellar features. Eight of these are early-type stars of O or B type in M31, with hard X-ray spectra, making them good HMXB candidates. Three of these eight exhibit emission lines, which we consider to be the strongest HMXB candidates. In addition, our spectra reveal two likely Galactic cataclysmic variables, one foreground M star, two probable LMXBs related to M31 globular clusters, one emission line region with an embedded Wolf-Rayet star, and one newly-discovered supernova remnant. Finally, two of the sources have stellar spectra with no features indicative of association with an X-ray source.
Dark influences III. Structural characterization of minor mergers of dwarf galaxies with dark satellites

In the current concordance cosmology small halos are expected to be completely dark and can significantly perturb low-mass galaxies during minor merger interactions. These interactions may well contribute to the diversity of the dwarf galaxy population. Dwarf galaxies in the field are often observed to have peculiarities in their structure, morphology, and kinematics, as well as strong bursts of star formation without apparent cause. We aim to characterize the signatures of minor mergers of dwarf galaxies with dark satellites to aid their observational identification. We explore and quantify a variety of structural, morphological, and kinematic indicators of merging dwarf galaxies and their remnants using a suite of hydrodynamical simulations. The most sensitive indicators of mergers with dark satellites are large asymmetries in the gaseous and stellar distributions, enhanced central surface brightness and starbursts, and velocity offsets and misalignments between the cold gas and stellar components. In general, merging systems span a wide range of values of the most commonly used indicators, while isolated objects tend to have more confined values. Interestingly, we find in our simulations that a significantly off-centered burst of star formation can pinpoint the location of the dark satellite. Observational systems with such characteristics are perhaps the most promising for unveiling the presence of the hitherto, missing satellites.
The Divergence in Demographic Factors of Technical and Vocational Education (TVE) Teacher Commitment

Teacher commitment is needed for the development and sustainability of the national education system. Therefore, the purpose of this study is to determine the level of TVE teachers’ commitme nt and to differentiate it based on gender, marital status, and level of education. Plus, the study also identifies the relationship of TVE teachers’ commitment with the selected demographic factor. The sample included 130 secondary school TVE teachers. Gender, marital status, age, years of service, and level of education were the demographic factors that this study focused on. For teacher commitment, the instrument used is a 16-item of 5-point Likert scale Teacher Commitment Scale with four dimensions. Respondents filled out an online survey using a Google Form. The data were analyzed by following descriptive and inferential statistics with SPSS version 25. The result showed that TVE teacher commitment is at a high level and there is no difference in TVE teacher commitment with gender, marital status, and level of education. However, there is a weak and significant relationship between TVE teacher commitment and marital status. As a result of the study, the researcher encourages policymakers to take measures to sustain the level of commitment of TVE teachers.
MID-INFRARED EXTINCTION MAPPING OF INFRARED DARK CLOUDS. II. THE STRUCTURE OF MASSIVE STARLESS CORES AND CLUMPS

We develop the mid-infrared extinction (MIREX) mapping technique of Butler & Tan (Paper I), presenting a new method to correct for the Galactic foreground emission based on observed saturation in independent cores. Using Spitzer GLIMPSE 8 μm images, this allows us to accurately probe mass surface densities, Σ, up to ≃ 0.5 g cm−2 with 2″ resolution and mitigate one of the main sources of uncertainty associated with Galactic MIREX mapping. We then characterize the structure of 42 massive starless and early-stage cores and their surrounding clumps, selected from 10 infrared dark clouds, measuring Σcl(r) from the core/clump centers. We first assess the properties of the core/clump at a scale where the total enclosed mass as projected on the sky is Mcl = 60 M☉. We find that these objects have a mean radius of Rcl ≃ 0.1 pc, mean and, if fitted by a power-law (PL) density profile , a mean value of kρ, cl = 1.1. If we assume a core is embedded in each clump and subtract the surrounding clump envelope to derive the core properties, then we find a mean core density PL index of kρ, c = 1.6. We repeat this analysis as a function of radius and derive the best-fitting PL plus uniform clump envelope model for each of the 42 core/clumps. The cores have typical masses of Mc ∼ 100 M☉ and , and are embedded in clumps with comparable mass surface densities. We also consider Bonnor–Ebert density models, but these do not fit the observed Σ profiles as well as PLs. We conclude that massive starless cores exist and are well described by singular polytropic spheres. Their relatively low values of Σ and the fact that they are IR dark may imply that their fragmentation is inhibited by magnetic fields rather than radiative heating. Comparing to massive star-forming cores and clumps, there is tentative evidence for an evolution toward higher densities and steeper density profiles as star formation proceeds.
4D light - field modeling and rendering

A cassette housing has an inlet and accommodates in its interior a turntable provided with a tape-engaging hub. The turntable is rotatable about a normally upright axis in one direction to take tape up on the hub, and in the opposite direction to pay tape out from the hub. A pair of guide baffles guides the tape for travel between the inlet and the hub. An articulated band of curved band sections surrounds the hub over a portion of arc and rests freely slidably on the turntable so that when the same is rotated in take-up direction the articulated band contracts about the hub to urge tape on the same against the hub, whereas when the turntable is rotated in the pay-out direction the articulated band expands about the hub to recede outwardly from it so as to permit unobstructed paying-out of the tape.