Miracle-dz/UniFAR-FTUs huggingface dataset:
Nonparametric Predictive Inference for Reproducibility of Basic Nonparametric Tests

Reproducibility of tests is an important characteristic of the practical relevance of test outcomes. Recently, there has been substantial interest in the reproducibility probability (RP), where not only its estimation but also its actual definition and interpretation are not uniquely determined in the classical frequentist statistics framework. Nonparametric predictive inference (NPI) is a frequentist statistics approach that makes few assumptions, enabled by the use of lower and upper probabilities to quantify uncertainty, and that explicitly focuses on future observations. The explicitly predictive nature of NPI provides a natural formulation for inferences on RP. In this article, we introduce the NPI approach to RP for some basic nonparametric tests.
A cross cultural investigation of individuals’ acceptance of Smart Home Technology: The role of needs satisfaction

Smart Home Technology manufacturers currently face significant issues with regard to the acceptance and intention to use their products. Evidence suggests that specific products have the lion’s share of the smart home market, and fully integrated smart home set-ups are still rare. The aim of this study was to investigate the acceptance of Smart Home Technology by administering the Technology Acceptance Model and applying Self Determination Theory with a sample of British (N = 284) and Spanish (N= 209) technology users. Results showed that perceived ease of use and perceived usefulness act as mediators of the effect of need satisfaction on respondents’ behavioural intention to use Smart Home Technology. Except for relatedness satisfaction, there were no gender effects; however, we found important differences between the British and Spanish participants, which are discussed in terms of cultural differences in the degree to which need satisfaction is important to participants.
Modeling the 3C 120 Radio Jet from 1 to 30 Milliarcseconds

In this paper we use the predicted spatial development of helical structures along an expanding jet to model observed structures and motions in the 3C 120 jet. New results of VLBI imaging of the parsec-scale radio jet in 3C 120 at 5 GHz are examined along with older long-term monitoring results at 5 GHz and older results obtained at 22 and 43 GHz. The high-frequency observations provide detailed information on motions and structure from 0.5 to 10 mas from the core and the lower frequency observations from 1 to 30 mas from the core. Proper motions of helical components associated with the pattern and of other components that move through the pattern provide estimates of flow and helical pattern speeds. Theoretical modeling of the motion and appearance of the helical pattern allows determination of sound speeds as a function of the jet viewing angle. The jet sound speed declines although probably not as fast as adiabatically. At a 12° viewing angle the most likely scenario involves a decline in jet sound speed from c/3 < aj < c/ at ~0.5 mas from the core to 0.1c < aj < 0.25c at ~25 mas from the core accompanied by some acceleration in the jet flow from Lorentz factor γ ≲ 5 to γ ≳ 7. The sound speed in the cocoon medium around the jet is less well determined but is less than the sound speed in the jet probably by a factor of 1.5-5. A largest possible viewing angle of 15° implies a jet sound speed at the upper limit of these estimates and somewhat higher flow Lorentz factors. However, jet morphology argues against viewing angles larger than 12°. At smaller viewing angles the jet sound speed is lower, and at a 6° viewing angle the jet sound speed is about a factor of 2 less, but the flow Lorentz factor is comparable. The decline in radio intensity is on the order of what would be associated with isothermal jet expansion. Knot-interknot intensity variations are greater than would be expected from adiabatic compressions associated with the helical twist, and we infer the presence of a shock along the leading edge of the helical twist in addition to shock or density structures flowing through the helical pattern. Our results imply that the macroscopic heating of the expanding jet fluid is less than the microscopic energization of the synchrotron radiating relativistic electrons.
Free flexural vibration of functionally graded size-dependent nanoplates

In this paper, the linear free flexural vibration behaviour of functionally graded (FG) size-dependent nanoplates are investigated using the finite element method. The field variables are approximated by non-uniform rational B-splines. The size-dependent FG nanoplate is investigated by using Eringen's differential form of nonlocal elasticity theory. The material properties are assumed to vary only in the thickness direction and the effective properties for FG nanoplate are computed using Mori-Tanaka homogenization scheme. The accuracy of the present formulation is tested considering the problems for which solutions are available. A detailed numerical study is carried out to examine the effect of material gradient index, the characteristic internal length, the plate thickness, the plate aspect ratio and the boundary conditions on the global response of FG nanoplate.
Fragmentation Phase Transition in Atomic Clusters IV -- Liquid-gas transition in finite metal clusters and in the bulk --

Within the micro-canonical ensemble it is well possible to identify phase-transitions in small systems. The consequences for the understanding of phase transitions in general are discussed by studying three realistic examples. We present micro-canonical calculations of the fragmentation phase transition in Na-, K-, and Fe- clusters of N = 200 to 3000 atoms at a constant pressure of 1 atm. The transition is clearly of ﬁrst order with a back-bending micro-canonical caloric curve T P ( E, V ( E, P )) = ∂S ( E, V ( E, P )) /∂E | P . From the Maxwell construction of β P ( E/N, P ) = 1 /T P one can simultaneously determine the transition temperature T tr , the speciﬁc latent heat q lat , and the speciﬁc entropy-loss ∆ s surf linked to the creation of intra-phase surfaces. T tr ∆ s surf ∗ N/ (4 πr 2 ws N 2 / 3 eff ) = γ gives the surface tension γ . Here is the combined surface area of all fragments with a mass m i ≥ 2 and multiplicity N i . All these characteristic parameters are for ∼ 1000 atoms similar to their experimentally known bulk values. This ﬁnding shows clearly that within micro-canonical thermodynamics phase transitions can unambiguously be determined without invoking the thermodynamic limit . However, one has carefully to distinguish observables which are deﬁned for each phase-space point , like the values of the conserved quantities, from thermodynamic quantities like temperature, pressure, chemical potential, and also the concept of pure phases, which refer to the volume of the energy shell of the N-body phase-space and thus do not refer to a single phase-space point. At the same time we present here the ﬁrst successful microscopic calculation of the surface tension in liquid sodium, potassium, and iron at a constant pressure of 1 atm.
Topics on Hydrodynamic Model of Nucleus-Nucleus Collisions

A survey is given on the applications of hydrodynamic model of nucleus-nucleus collisons, focusing especially on i) the resolution of hydrodynamic equations for arbitrary configurations, by using the smoothed-particle hydrodynamic approach; ii) effects of the event-by-event fluctuation of the initial conditions on the observables; iii) decoupling criteria; iv) analytical solutions; and others.
Scattering-produced (sub)millimetre polarization in inclined discs: optical depth effects, near–far side asymmetry and dust settling

Disk polarization at (sub)millimeter wavelengths is being revolutionized by ALMA observationally, but its origin remains uncertain. Dust scattering was recently recognized as a potential contributor to polarization, although its basic properties have yet to be thoroughly explored. Here, we quantify the effects of optical depth on the scattering-induced polarization in inclined disks through a combination of analytical illustration, approximate semi-analytical modeling using formal solution to the radiative transfer equation, and Monte Carlo simulations. We find that the near-side of the disk is significantly brighter in polarized intensity than the far-side, provided that the disk is optically thick and that the scattering grains have yet to settle to the midplane. This asymmetry is the consequence of a simple geometric effect: the near-side of the disk surface is viewed more edge-on than the far-side. It is a robust signature that may be used to distinguish the scattering-induced polarization from that by other mechanisms, such as aligned grains. The asymmetry is weaker for a geometrically thinner dust disk. As such, it opens an exciting new window on dust settling. We find anecdotal evidence from dust continuum imaging of edge-on disks that large grains are not yet settled in the youngest (Class 0) disks, but become more so in older disks. This trend is corroborated by the polarization data in inclined disks showing that younger disks have more pronounced near-far side asymmetry and thus less grain settling. If confirmed, the trend would have far-reaching implications for grain evolution and, ultimately, the formation of planetesimals and planets.
CO luminosity–FWHM correlation of low- and high-redshift galaxies and its possible cosmological utilization

A linear correlation has been proposed between the CO luminosity ($\rm{L}^{\prime}_{\rm{CO}}$) and full-width at half maximum (FWHM) for high-redshift (z > 1) submillimeter galaxies. However, the controversy concerning the $\rm{L}^{\prime}_{\rm{CO}}$-FWHM correlation seems to have been caused by the use of heterogeneous samples (e.g., different transition lines) and/or data with large measurement uncertainties. In order to avoid the uncertainty caused by using different rotational transitions, in this work we make an extensive effort to select only CO($J = 1-0$) data from the literature. We separate these wide-ranging redshift data into two samples : the low-redshift (z 1) samples. The samples are corrected for lensing magnification factors if gravitational-lensing effects appeared in the observations. The correlation analysis shows that there exists significant $\rm{L}^{\prime}_{\rm{CO}}$-FWHM correlations for both the low-redshift and high-redshift samples. A comparison of the low- and high-redshift $\rm{L}^{\prime}_{\rm{CO}}$-FWHM correlations does not show strong evolution with redshift. Assuming that there is no evolution, we can use this relation to determine the model independent distances of high-redshift galaxies. We then constrain cosmological models with the calibrated high-redshift CO data and the sample of Type Ia supernovae in the Union 2.1 compilation. In the constraint for wCDM with our samples, the derived values are w_{0} = -1.02 {\pm} 0.17, {\Omega}_{m0} = 0.30{\pm}0.02, and H_{0} = 70.00 {\pm}0.60 km\,s^{-1}\,Mpc^{-1}.
Shear and vorticity in the spherical collapse of dark matter haloes

Traditionally the spherical collapse of objects is studied with respect to a uniform background density, yielding the critical over-density $\delta_\mathrm{c}$ as key ingredient to the mass function of virialized objects. Here we investigate the shear and rotation acting on a peak in a Gaussian random field. By assuming that collapsing objects mainly form at those peaks, we use this shear and rotation as external effects changing the dynamics of the spherical collapse, which is described by the Raychaudhuri equation. We therefore assume that the shear and rotation have no additional dynamics on top of their cosmological evolution and thus only appear as inhomogeneities in the differential equation.
Upward Bipolar Lightning Flashes Originated From the Connection of Recoil Leaders With Intracloud Lightning

The present work shows high‐speed videos of two upward flashes that started with positive upward leaders and, instead of being followed by negative subsequent return strokes, they were followed by positive subsequent return strokes. In both cases, after the positive leaders developed, recoil leaders (RL) appeared in their decayed branches as would be usual in negative upward lightning flashes. However, in these flashes the negative end of a recoil leader connected to a positive leader of an intracloud (IC) flash nearby. The connection initiated a downward positive leader that re‐ionized the decayed channel of the upward flash all the way to the tower giving origin to a positive subsequent return stroke. This work shows that RL do play an important role in the occurrence of bipolar upward flashes and their interaction with IC flashes can provide explanations for all types of bipolar upward flashes initiated by upward positive leaders.
Comparison of hard X-ray spectra of luminous radio galaxies and their radio-quiet counterparts

We study the differences in X-ray properties of luminous radio galaxies and their radio-quiet counterparts. In order to avoid biases associated with the dependence of X-ray properties on the black hole mass and Eddington ratio, the radio-loud and radio-quiet objects are selected to cover similar ranges of these parameters. Our studies are based on the X-ray data from the Swift/BAT catalogue. We confirm previous results that radio galaxies are on average X-ray-louder than radio-quiet AGNs, but find that their spectral slopes are very similar. This suggests that in radio-loud and radio-quiet AGNs the hard X-rays are produced in the same region and by the same mechanism. We argue that this region can be associated with the hot, geometrically thick, central portion of the accretion flow, where production of hard X-rays is likely to be dominated by Comptonization of the optical/UV radiation of the truncated 'cold' accretion disc by hot electrons. The larger X-ray luminosities in radio-loud AGNs may result from larger radiative efficiencies of the innermost portions of the accretion flows around faster rotating black holes.
Large Wood in Small Channels: A 20‐Year Study of Budgets and Piece Mobility in Two Redwood Streams

Large wood (LW) influences geomorphic and ecological processes. However, most field data sets describing LW dynamics are conducted over the span of only a few years. We present a unique long‐term data set from northern California, USA of LW volumes, inputs, and transport in two small headwater streams, the North Fork (NF) and South Fork (SF) of Caspar Creek. We used data collected approximately every 2 years from 1998 to 2018 to assess how LW budgets change over time between catchments, what factors influence inputs from standing trees to the streams, and controls on LW piece mobility. We find that the SF, which experienced stream‐side logging and instream wood removal in the 1970s, continued to have lower LW volumes (range of 101–153 m3 km−1 over the 20‐year period) compared to the NF (range of 297–313 m3 km−1), which experienced logging in the 1980s but with buffer strips left near the channel. If current trends continue, it will likely take ∼100–200 years from the time of logging for the SF to reach NF instream wood volumes. We show that windstorms combined with precipitation events, very high winds, and hillslope steepness are strongly associated with LW piece inputs from standing trees. LW moves infrequently in the channel, with piece characteristics, the number of wood pieces per meter surrounding an LW piece, and discharge metrics influencing LW entrainment and displacement lengths. Our data set provides strong support to previously identified controls on LW dynamics in streams while also capturing variability over a 20‐year period.
Energy and angular distributions of neutrons from 90 MeV proton and 140 MeV alpha-particle bombardment of nuclei

We measured neutron time-of-flight spectra from 90 MeV protons and 140 MeV alpha particles bombarding thin targets of Al, Ni, Zr, and Bi at laboratory angles between 20/sup 0/ and 135/sup 0/. The low-energy (5 to 45 MeV) portions of the spectra were measured with 5 cm diameter by 5 cm deep NE-213 counters at 1 m flight paths with n-. gamma. pulse-shape discrimination. The high-energy (35 to 150 MeV) portions of the spectra were measured with 12.7 cm diameter by 10.2 cm deep NE-102 counters at flight paths of 2.0 to 5.0 m. The proton-induced measured neutron spectra reveal three distinct energy regions: a low-energy evaporation region, a high-energy region dominated by the quasifree scattering process, and an intermediate-energy region dominated by multistep, preequilibrium processes. In the latter two regions, the spectra show strong angular dependence. The alpha-particle induced neutron spectra show these same distinct energy regions plus an exponential falloff above the beam energy per nucleon. The neutron spectra are compared with earlier proton spectra produced also by 90 MeV protons and 140 MeV alpha particles. It is observed that the high-energy portions of the forward-angle neutron and proton cross sections are in ratios consistent with the idea thatmore » single nucleon-nucleon scattering dominates. For the heavy-mass targets, the low-energy evaporation regions show neutron yields larger than proton yields. The proton-to-neutron ratios observed in the high-energy continua are interpreted with a quasifree calculation fitted simultaneously to the proton and the neutron spectra. Preequilibrium calculations with the exciton model and the hybrid model reproduce the shape of the experimental angle-integrated energy spectra down to lower energies than the quasifree calculations. The exciton model calculations underestimate the magnitudes of the cross sections, while the hybrid model provides better absolute agreement. « less
Association Between Serum Midkine Level and Gastric Precancerous Lesion in Patients with Gastritis

Background: Gastric cancer is the fifth most common malignancy and the third highest cancer-related mortality worldwide after lung and colorectal cancers. The gastric carcinogenesis is started with precancerous lesion. Prompt diagnosis and management of gastric precancerous lesion may prevent disease progression. Midkine is a growth factor associated with various cancers and proposed as a marker for detecting gastric precancerous lesion. Objective: The aim of the study is to determine the association between serum midkine level and gastric precancerous lesion in patients with gastritis. Methods: A cross sectional study was conducted at Haji Adam Malik general hospital. Subjects were obtained by consecutive sampling. Inclusion criteria were patients aged 18 years or older, diagnosed with gastritis from gastroscopy and histopathology results, and willing to cooperate in the study. Each subjects underwent interview and endoscopic examination. Serum midkine level was determined using enzyme-linked immunosorbent assay (ELISA) method. Chi square, receiver operating characteristic (ROC) curve, and logistic regression tests were applied. Results: A total of 160 subjects were enrolled with 29.4% had gastric precancerous lesion. Serum midkine level was associated with gastric premalignant lesion. Cut off point for serum midkine level was 252 pg/mL with area under the curve of 0.816 (p<0.001). It’s sensitivity, specificity, and accuracy in diagnosing gastric precancerous lesion were 74.5%, 71.7%, and 72.5%, respectively. Helicobacter pylori infection, high serum midkine level, heavy alcohol drinker, and family history of gastric cancer were risk factors for gastric precancerous lesion. Conclusion: Serum midkine level is associated with gastric premalignant lesion in patients with gastritis and has good diagnostic values.
Spatial separation of rotating binary Bose-Einstein condensates by tuning the dipolar interactions

We are pointing out relevant anisotropic effects, related to spatial separation, miscibility and mass-symmetry, due to dipole-dipole interactions in rotating binary dipolar Bose-Einstein condensates, by considering symmetric ($^{164}$Dy-$^{162}$Dy) and asymmetric ($^{168}$Er-$^{164}$Dy, $^{164}$Dy-$^{87}$Rb) dipolar mixtures. The binary mixtures are kept in strong pancake-shaped trap, modeled by an effective two-dimensional coupled Gross-Pitaevskii equation. The anisotropy of the dipolar interactions, on miscibility and vortex-lattice structures, is studied by tuning the polarization angle of the dipoles $\varphi$, which can enhance the attractive part of the dipole-dipole interaction (DDI) for both inter- and intra-species. Within this procedure of changing to attractive the DDI, a clear spatial separation is verified in the densities at some critical polarization angle. The spatial separations, being angular for symmetric mixtures and radial for asymmetric ones, are verified for repulsive contact interactions when the inter- to intra-species ratio $\delta$ is larger than one, implying the system is less miscible. The corresponding result for the critical polarization angle as a function of $\delta$ is shown in the particular dipolar symmetric case. A striking outcome of the present study is the observed sensibility of the vortex-pattern binary distributions due to the mass-asymmetry. This is exemplified by the symmetric dipolar mixture, where the two isotopes are of the same species.
Pressure Profiles of Distant Galaxy Clusters in the Planck Catalogue

Successive releases of Planck data have demonstrated the strength of the Sunyaev–Zeldovich (SZ) effect in detecting hot baryons out to the galaxy cluster peripheries. To infer the hot gas pressure structure from nearby galaxy clusters to more distant objects, we developed a parametric method that models the spectral energy distribution and spatial anisotropies of both the Galactic thermal dust (GTD) and the cosmic microwave background (CMB), which are combined with the cluster SZ and dust signals. Taking advantage of the best angular resolution of the High Frequency Instrument channels (5 arcmin) and using X-ray priors in the innermost cluster regions that are not resolved with Planck, this modeling allowed us to analyze a sample of 61 nearby members of the Planck Catalogue of SZ sources ( , ) using the full mission data, as well as to examine a distant sample of 23 clusters ( , ) that have been recently followed-up with XMM-Newton and Chandra observations. We find that (i) the average shape of the mass-scaled pressure profiles agrees with results obtained by the Planck Collaboration in the nearby cluster sample, and that (ii) no sign of evolution is discernible between averaged pressure profiles of the low- and high-redshift cluster samples. In line with theoretical predictions for these halo masses and redshift ranges, the dispersion of individual profiles relative to a self-similar shape stays well below 10% inside r500 but increases in the cluster outskirts.