Miracle-dz/UniFAR-FTUs huggingface dataset:
Phases of supersymmetric O(N) theories

We perform a global renormalization group study of O(N) symmetric Wess-Zumino theories and their phases in three euclidean dimensions. At infinite N the theory is solved exactly. The phases and phase transitions are worked out for finite and infinite short-distance cutoffs. A distinctive new feature arises at strong coupling, where the effective superfield potential becomes multi-valued, signalled by divergences in the fermion-boson interaction. Our findings resolve the long-standing puzzle about the occurrence of degenerate O(N) symmetric phases. At finite N, we find a strongly-coupled fixed point in the local potential approximation and explain its impact on the phase transition. We also examine the possibility for a supersymmetric Bardeen-Moshe-Bander phenomenon, and relate our findings with the spontaneous breaking of supersymmetry in other models.
Practical Inference from Industrial Split-Plot Designs

In many industrial response surface experiments, some of the factors investigated are not reset independently. The resulting experimental design then is of the split-plot type, and the observations in the experiment are in many cases correlated. A proper analysis of the experimental data therefore is a mixed model analysis involving generalized least-squares estimation. Many people, however, analyze the data as if the experiment was completely randomized and estimate the model using ordinary least squares. The purposes of this article are to quantify the differences in conclusions reached from the two methods of analysis and to provide the reader with guidance for analyzing split-plot experiments in practice. The problem of determining the denominator degrees of freedom for significance tests in the mixed model analysis is discussed as well.
Investigation of Vortex Structures in Gas-Discharge Nonneutral Electron Plasma: II. Vortex Formation, Evolution and Dynamics

The results of experimental investigations of inhomogeneities of gas-discharge nonneutral electron plasma obtained by using the nonperturbing experimental methods [N.A. Kervalishvili, arXiv:1502.02516 [physics.plasm-ph] (2015)] have been presented. Inhomogeneities are the dense solitary vortex structures stretched along the magnetic field, the lifetime of which is much greater than the time of electron-neutral collisions. The processes of formation, evolution and dynamics of vortex structures were studied. The periodic sequence of these processes is described for different geometries of discharge device.
Massive stars at low metallicity - Evolution and surface abundances of O dwarfs in the SMC

We study the evolution, rotation, and surface abundances of O-type dwarfs in the Small Magellanic Cloud. We analyzed the UV and optical spectra of twenty-three objects and derived photospheric and wind properties. The observed binary fraction of the sample is ~ 26%, which is compatible with more systematic studies, if one considers that the actual binary fraction is potentially larger owing to low-luminosity companions and that the sample excluded obvious spectroscopic binaries. The location of the fastest rotators in the H-R diagram indicates that these could be several Myr old. The offset in the position of these fast rotators compared with the other stars confirms the predictions of evolutionary models that fast-rotating stars tend to evolve more vertically in the H-R diagram. Only one star of luminosity-class Vz, expected to best characterize extreme youth, is located on the ZAMS, the other two stars are more evolved. The distribution of nitrogen abundance of O and B stars suggests that the mechanisms responsible for the chemical enrichment of slowly rotating massive stars depends only weakly on the star's mass. We confirm that the group of slowly rotating N-rich stars is not reproduced by the evolutionary tracks. Our results call for stronger mixing in the models to explain the range of observed N abundances. All stars have an N/C ratio as a function of stellar luminosity that matches the predictions of the stellar evolution models well. More massive stars have a higher N/C ratio than the less massive stars. Faster rotators show on average a higher N/C ratio than slower rotators. The N/O versus N/C ratios agree qualitatively well with those of stellar evolution models. The only discrepant behavior is observed for the youngest two stars of the sample, which both show very strong signs of mixing, which is unexpected for their evolutionary status.
Little change in the sizes of the most massive galaxies since z = 1

Recent reports suggest that elliptical galaxies have increased their size dramatically over the last ~8 Gyr. This result points to a major rethink of the processes dominating the late-time evolution of galaxies. In this paper we present the first estimates for the scale sizes of brightest cluster galaxies (BCGs) in the redshift range 0.8 <z <1.3 from an analysis of deep Hubble Space Telescope imaging, comparing to a well-matched local sample taken from the Local Cluster Substructure Survey at z~ 0.2. For a small sample of five high-redshift BCGs we measure half-light radii ranging from 14 to 53kpc using de Vaucuoleurs profile fits, with an average determined from stacking of 32.1 ± 2.5kpc compared to a value 43.2 ± 1.0kpc for the low-redshift comparison sample. This implies that the scale sizes of BCGs at z= 1 are ≃30 per cent smaller than at z= 0.25. Analyses comparing either Sersic or Petrosian radii also indicate little or no evolution between the two samples. The detection of only modest evolution at most out to z= 1 argues against BCGs having undergone the large increase in size reported for massive galaxies since z= 2 and in fact the scale-size evolution of BCGs appears closer to that reported for radio galaxies over a similar epoch. We conclude that this lack of size evolution, particularly when coupled with recent results on the lack of BCG stellar mass evolution, demonstrates that major merging is not an important process in the late-time evolution of these systems. The homogeneity and maturity of BCGs at z= 1 continues to challenge galaxy evolution models.
The maximum asymptotic bias of outlier identifiers

In their paper, Davies and Gather (1993) formalized the task of outlier identification, considering also certain performance criteria for outlier identifiers. One of those Criteria, the maximum asymptotic bias, is carried over here to multivariate outlier identifiers. We show how this term depends on the respective biases of estimators which are used to construct the identifier. It turns out that the use of high breakdown robust estimators is not sufficient to achieve outlier identifiers with bounded maximum asymptotic bias.
Constructing regularized cosmic propagators

We present a new scheme for the general computation of cosmic propagators that allow to interpolate between standard perturbative results at low-k and their expected large-k resummed behavior. This scheme is applicable to any multi-point propagator and allows the matching of perturbative low-k calculations to any number of loops to their large-k behavior, and can potentially be applied in case of non-standard cosmological scenarios such as those with non-Gaussian initial conditions. The validity of our proposal is checked against previous prescriptions and measurements in numerical simulations showing a remarkably good agreement. Such a generic prescription for multi-point propagators provides the necessary building blocks for the computation of polyspectra in the context of the so-called Gamma-expansion introduced by Bernardeau et al. (2008). As a concrete application we present a consistent calculation of the matter bispectrum at one-loop order.
Teacher Performance Analysis in Terms of Job Satisfaction and Commitment

The problem of teacher performance is an important problem that must be addressed immediately. Factors The main cause in terms of lack of job satisfaction and commitment. This study aims to prove that job satisfaction and commitment have an effect either partially or simultaneously on performance. And to prove which of the job satisfaction and commitment have a dominant effect on the performance of teachers in SMA PGRI 1 Lumajang, East Java, Indonesia. This research uses multiple linear regression method and then the data results are processed with the help of the SPSS program and hypothesis testing. The results showed that job satisfaction and commitment to performance. The higher the job satisfaction, the higher the performance. Likewise with commitment, the higher the commitment to work, the higher the performance. The uniqueness of this research is the main supporting factor in improving performance, namely job satisfaction. In improving teacher performance, what must be considered is the teacher's job satisfaction factor.
The Influence of Academic Supervision Activities, School Culture, Infrastructure, on the Quality of Learning Processes and Outcomes at Madrasah Aliyah

The lack of optimal quality of education in madrasahs causes the public image of madrasas to remain poor. The public view of Madrasahs is associated with second-choice educational institutions, not developed, slums, and other negative images about madrasas, therefore, the desire of the community (parents) to continue their children's studies in madrasahs is very lacking. For the quality of learning in madrasah to increase, the head of the madrasah must always improve the effectiveness of the implementation of academic supervision, improve good school culture, and prepare educational facilities. The results of the pre-survey on the quality of learning at Madrasah Aliyah in South Lampung District, the initial data obtained on the quality of the learning process are as follows: (1) there are still many teachers using less varied learning methods; (2) teachers rarely make use of and use instructional media; (3) learning activities do not activate students, where teachers are more active in learning; (4) the evaluation activities carried out by the teacher were more on the cognitive aspects; (5) learning activities carried out by the teacher do not optimize the development of all potential students; and (6) student learning outcomes are rarely followed up, the information is merely to find out the extent of the learning outcomes of students (students).
A universal scaling for short and long gamma-ray bursts: EX,iso - Eγ,iso - Epk

The comprehensive statistical analysis of Swift X-ray light curves, collecting data from six years of operation, revealed the existence of a universal scaling among the isotropic energy emitted in the rest-frame 1 - 104 keV energy band during the prompt emission (), the peak of the prompt emission energy spectrum (Epk) and the X-ray energy emitted in the 0.3–10 keV observed energy band (EX, iso). In this paper, we show that this three-parameter correlation is robust and does not depend on our definition of EX, iso. It is shared by long, short and low-energetic gamma-ray bursts (GRBs), and thus reflects the existence of some properties which are shared by the GRB class as a whole. A more intuitive way to express the three-parameter correlation is in the form of a two-parameter correlation between the GRB efficiency and Epk. We speculate that the physical origin of such a relation is connected with the outflow Lorentz factor.
Thermodynamics of histories for the one-dimensional contact process

The dynamical activity K(t) of a stochastic process is the number of times it changes configuration up to time t. It was recently argued that (spin) glasses are at a first-order dynamical transition where histories of low and high activity coexist. We study this transition in the one-dimensional contact process by weighting its histories with exp(sK(t)). We determine the phase diagram and the critical exponents of this model using a recently developed approach to the thermodynamics of histories that is based on the density matrix renormalization group. We find that for every value of the infection rate, there is a phase transition at a critical value of s. Near the absorbing state phase transition of the contact process, the generating function of the activity shows a scaling behaviour similar to that of the free energy in an equilibrium system near criticality.
Polymer quantization of the Einstein-Rosen wormhole throat

We present a polymer quantization of spherically symmetric Einstein gravity in which the polymerized variable is the area of the Einstein-Rosen wormhole throat. In the classical polymer theory, the singularity is replaced by a bounce at a radius that depends on the polymerization scale. In the polymer quantum theory, we show numerically that the area spectrum is evenly spaced and in agreement with a Bohr-Sommerfeld semiclassical estimate, and this spectrum is not qualitatively sensitive to issues of factor ordering or boundary conditions except in the lowest few eigenvalues. In the limit of small polymerization scale we recover, within the numerical accuracy, the area spectrum obtained from a Schr\"odinger quantization of the wormhole throat dynamics. The prospects of recovering from the polymer throat theory a full quantum-corrected spacetime are discussed.
An Outdoor Support Insulator Surface Defects Segmentation Approach via Image Adversarial Reconstruction in High-Speed Railway Traction Substation

As a result of high-voltage electricity and outdoor environment in high-speed railway traction substation, insulator surface defects are inevitable. However, most of the current unsupervised learning visual detection methods can only achieve patch-level defects detection. To achieve the goal of defects pixel-level segmentation, a universal three-step outdoor support insulators surface defects segmentation framework is proposed to segment insulators surface defects in this article. In this framework, outdoor support insulators are first located using the robust SCRDet network, which can locate the insulators accurately toward various angles. Then, a resolution-improved insulator reconstruction network (RIIR-Net) is proposed to reconstruct resolution-improved nondefect insulators. Finally, defective areas of insulators, such as missing, porcelain drop, and flashover, can be segmented via the proposed coarse-to-fine defects decision strategy, which can postprocess the residual map between the original defective insulator and the reconstructed nondefect insulator to effectively filter noise and segment defects based on decision rules of color feature, area, and HuMoment. Experiments on dataset collected from the Heishan traction substation demonstrate that the newly designed RIIR-Net can indeed improve the quality of reconstructed normal insulators, and the proposed framework can accurately achieve the task of outdoor support insulators defects pixel-level segmentation, including but not limited to missing, porcelain drop, and flashover.
Probing quiet Sun magnetism using MURaM simulations and Hinode/SP results: support for a local dynamo

Context. Owing to the limited spatial resolution and the weak polarization signal coming from the quietest regions on the Sun, the organization of the magnetic field on the smallest scales is largely unknown. Aims. We obtain information about the magnetic flux present in the quiet Sun by comparing radiative MHD simulations with observations, with particular emphasis on the role of surface dynamo action. Methods. We synthesized Stokes profiles on the basis of the MHD simulation results. The profiles are degraded by taking the properties of the spectropolarimeter (SP) into account onboard the Hinode satellite. We used simulation runs with different magnetic Reynolds numbers (R m ) and observations at different heliocentric angles with different levels of noise. Results. Simulations with an imposed mixed-polarity field and R m below the threshold for dynamo action reproduce the observed vertical flux density, but do not display a high enough horizontal flux density. Surface dynamo simulations at the highest R m feasible at the moment yield a ratio of the horizontal and vertical flux density consistent with observational results, but the overall amplitudes are too low. Based on the properties of the local dynamo simulations, a tentative scaling of the magnetic field strength by a factor 2-3 reproduces the signal observed in the internetwork regions. Conclusions. We find agreement with observations at different heliocentric angles. The mean field strength in internetwork implied by our analysis is roughly 170 G at the optical depth unity. Our study shows that surface dynamo could be responsible for most of the magnetic flux in the quiet Sun outside the network, given that the extrapolation to higher R m is valid.
Improvement of surface wave methods for constructing subsurface S-wave velocity structures

Improvement of surface wave methods for constructing subsurface S-wave velocity structures by Tatsunori Ikeda Chair: Toshifumi Matsuoka Seismic surface waves are guided waves propagating on the surface of the earth. Although surface waves have a long history in seismological studies, the use of surface waves has not been common in geophysical explorations. In a reflection or refraction seismic survey, surface waves are regarded as noise to be eliminated. Recently, however, a seismic exploration method using surface waves has been dramatically developed mainly for engineering purposes. The surface wave method is attractive because it is non-destructive, low cost, and simple compared to other seismic methods. By the surface wave method, subsurface S-wave velocity structures can be efficiently estimated from dispersion of surface waves. Since S-wave velocity structures down to several tens of meters play an important role for evaluating local ground-motion amplification, the surface wave method is one of the most important geophysical methods to be established for earthquake-prone countries such as Japan. The surface wave method utilizes velocity dispersion of surface waves, which can be extracted from both passive and active seismic data by surface wave analysis. Since surface waves can be theoretically modeled for horizontally layered structures, S-wave
Nonlocal halo bias with and without massive neutrinos

Understanding the biasing between the clustering properties of halos and the underlying dark matter distribution is important for extracting cosmological information from ongoing and upcoming galaxy surveys. While on sufficiently larges scales the halo overdensity is a local function of the mass density fluctuations, on smaller scales the gravitational evolution generates non-local terms in the halo density field. We characterize the magnitude of these contributions at third-order in perturbation theory by identifying the coefficients of the non-local invariant operators, and extend our calculation to include non-local (Lagrangian) terms induced by a peak constraint. We apply our results to describe the scale-dependence of halo bias in cosmologies with massive neutrinos. The inclusion of gravity-induced non-local terms and, especially, a Lagrangian $k^2$-contribution is essential to reproduce the numerical data accurately. We use the peak-background split to derive the numerical values of the various bias coefficients from the excursion set peak mass function. For neutrino masses in the range $0\leq \sum_i m_{\nu_i} \leq 0.6$ eV, we are able to fit the data with a precision of a few percents up to $k=0.3\, h {\rm \,Mpc^{-1}}$ without any free parameter.
THE H i MASS DENSITY IN GALACTIC HALOS, WINDS, AND COLD ACCRETION AS TRACED BY Mg ii ABSORPTION

It is well established that Mg ii absorption lines detected in background quasar spectra arise from gas structures associated with foreground galaxies. The degree to which galaxy evolution is driven by the gas cycling through halos is highly uncertain because their gas mass density is poorly constrained. Fitting the Mg ii equivalent width (W) distribution with a Schechter function and applying the N(H i)–W correlation of Ménard & Chelouche, we computed Ω(H i)Mg ii ≡ Ω(H i)halo = 1.41+0.75−0.44 × 10−4 for 0.4 ⩽ z ⩽ 1.4. We exclude damped Lyα's (DLAs) from our calculations so that Ω(H i)halo comprises accreting and/or outflowing halo gas not locked up in cold neutral clouds. We deduce that the cosmic H i gas mass density fraction in galactic halos traced by Mg ii absorption is Ω(H i)halo/Ω(H i)DLA ≃ 15% and Ω(H i)halo/Ωb ≃ 0.3%. Citing several lines of evidence, we propose that infall/accretion material is sampled by small W whereas outflow/winds are sampled by large W, and find that Ω(H i)infall is consistent with Ω(H i)outflow for bifurcation at W = 1.23+0.15− 0.28 Å; cold accretion would then comprise no more than ∼7% of the total H i mass density. We discuss evidence that (1) the total H i mass cycling through halos remains fairly constant with cosmic time and that the accretion of H i gas sustains galaxy winds, and (2) evolution in the cosmic star formation rate depends primarily on the rate at which cool H i gas cycles through halos.
SEGUE 3: AN OLD, EXTREMELY LOW LUMINOSITY STAR CLUSTER IN THE MILKY WAY's HALO

We investigate the kinematic and photometric properties of the Segue 3 Milky Way companion using Keck/DEIMOS spectroscopy and Magellan/IMACS g- and r-band imaging. Using maximum likelihood methods to analyze the photometry, we study the structure and stellar population of Segue 3. We find that the half-light radius of Segue 3 is 26″ ± 5″ (2.1 ± 0.4 pc, for a distance of 17 kpc) and the absolute magnitude is a mere MV = 0.0 ± 0.8 mag, making Segue 3 the least luminous old stellar system known. We find Segue 3 to be consistent with a single stellar population, with an age of 12.0+1.5− 0.4 Gyr and an [Fe/H] of −1.7+0.07− 0.27. Line-of-sight velocities from the spectra are combined with the photometry to determine a sample of 32 stars which are likely associated with Segue 3. The member stars within three half-light radii have a velocity dispersion of 1.2 ± 2.6 km s−1. Photometry of the members indicates that the stellar population has a spread in [Fe/H] of ≲ 0.3 dex. These facts, together with the small physical size of Segue 3, imply the object is likely an old, faint stellar cluster which contains no significant dark matter. We find tentative evidence for stellar mass loss in Segue 3 through the 11 candidate member stars outside of three half-light radii, as expected from dynamical arguments. Interpretation of the data outside of three half-light radii is complicated by the object's spatial coincidence with a previously known halo substructure, which may enhance contamination of our member sample.
Gauged Hopfions

We discuss the $U(1)$ gauged version of the 3+1 dimensional Faddeev-Skyrme model supplemented by the Maxwell term. We show that there exist axially symmetric static solutions coupled to the non-integer toroidal flux of magnetic field, which revert to the usual Hopfions ${\cal A}_{m,n}$ of lower degrees $Q=mn$ in the limit of the gauge coupling constant vanishing. The masses of the static gauged Hopfions are found to be less than the corresponding masses of the usual ungauged solitons ${\cal A}_{1,1}$ and ${\cal A}_{2,1}$ respectively, they become lighter as gauge coupling increases. The dependence of the solutions on the gauge coupling is investigated. We find that in the strong coupling regime the gauged Hopfion carries two magnetic fluxes, which are quantized in units of $2\pi$, carrying $n$ and $m$ quanta respectively. The first flux encircles the position curve and the second one is directed along the symmetry axis. Effective quantization of the field in the gauge sector may allow us to reconsider the usual arguments concerning the lower topological bound in the Faddeev-Skyrme-Maxwell model.