Miracle-dz/UniFAR-FTUs huggingface dataset:
Artificial Neural Network-Based Prediction of Death Anxiety in HIV-Positive Cases through Social Support and Distress Tolerance

Background: Distress tolerance has increasingly been used as an important construct to develop a novel insight into the onset and persistence of psychological traumas as well as prevention and treatment. Objectives: The present study investigated the relationship between social support and distress tolerance with death anxiety using artificial neural networks (ANN) in human immunodeficiency virus (HIV)-positive cases. Methods: The research method was descriptive-correlational. The statistical population included all the HIV-positive cases of Ahvaz in 2021. The convenience sampling method was employed to select 91 participants as the research sample. The research instruments included the Death Anxiety Scale (DAS), the Social Support Survey (SSS), and the Distress Tolerance Scale (DTS). The Pearson correlation coefficient, simultaneous regression, and ANN were used for data analysis. Results: The mean and standard deviation (SD) of death anxiety, social support, and distress tolerance were 9.07 ± 2.76, 63.78 ± 18.05, and 37.49 ± 12.91, respectively. The results showed a negative correlation between death anxiety, social support, and distress tolerance. Also, there was a significant negative relationship between social support and death anxiety (β = -0.31, P < 0.001). There was also a significant negative relationship between distress tolerance and death anxiety in HIV-positive cases (β = -0.53, P < 0.001). Conclusions: It is now more necessary than ever before to consider the effects of social support and distress tolerance on death anxiety in HIV-positive cases. Apparently, their death anxiety is affected by other factors and their interactive effects.
Circularly Polarized Broadside Beam Radiated From a Large, Low-Profile Metaloop Antenna

The area within a loop antenna can be used for inserting additional components (such as mounting hardware) if this does not cause the antenna characteristics to degrade. This article discusses a circularly polarized (CP) metaloop antenna that has a loop circumference of <inline-formula> <tex-math notation="LaTeX">${C} _{\mathrm {LOOP}}= 1 \lambda _{\text {g}}= n\lambda _{0}$ </tex-math></inline-formula> with <inline-formula> <tex-math notation="LaTeX">$n>1$ </tex-math></inline-formula>, thereby creating a large area within the loop, where <inline-formula> <tex-math notation="LaTeX">$\lambda _{\text {g}}$ </tex-math></inline-formula> (<inline-formula> <tex-math notation="LaTeX">$= 2~\pi /\beta $ </tex-math></inline-formula>) and <inline-formula> <tex-math notation="LaTeX">$\lambda _{0}$ </tex-math></inline-formula> (<inline-formula> <tex-math notation="LaTeX">$= 2~\pi /k_{0}$ </tex-math></inline-formula>) are the guide wavelength of the current on the loop and the free-space wavelength, respectively. Values for the propagation phase constant within the range of <inline-formula> <tex-math notation="LaTeX">$-1 < \beta /k_{0} < 0$ </tex-math></inline-formula> are used in this article. It is found that metaloop antennas for <inline-formula> <tex-math notation="LaTeX">$n = 3$ </tex-math></inline-formula>, 4, and 5 generate a CP broadside beam (axial beam) with gain bandwidths (GBWs) of approximately 6%, 5%, and 4%, respectively. The VSWR across the GBWs is less than two and the axial ratio is less than 3 dB. The radiation efficiencies for <inline-formula> <tex-math notation="LaTeX">$n=3$ </tex-math></inline-formula>, 4, and 5 are approximately 48%, 69%, and 83%, respectively. When a conducting disk (as a generalization for the presence of additional components) is inserted into these metaloop antennas, the antenna characteristics are not degraded until the disk and the metaloop are in close proximity (proximity coupling occurs).
MATHEMATICAL SELF-ESTEEM ABILITY OF JUNIOR HIGH SCHOOL STUDENTS IN PROJECT-BASED LEARNING

The main objective of this research is to study the achievement of their mathematical self-esteem, as a result of Project-based Learning (PBL) and Conventional Learning (CL). This research is conducted mathematical self-esteem to be possessed by students, but in reality shows their self-esteem are still low. This research used quasi experimental methods. The population of this study is students of State Junior High Schools in Bandung City, West Java Province. The sample comprises the students of grade VIII. One class as an experimental group that received PBL learning and another class as a control group that received CL learning. The instruments used in this study are Prior Mathematical Knowledge (PMK) worksheet and mathematical self-esteem scale. The results indicate that: (1) the achievement of mathematical self-esteem of the students who received PBL learning is better than the students who received CL learning; (2) there is no interaction effect between learning model and PMK on the achievement of students' mathematical self-esteem.
Structure and evolution of X-ray heated compact binaries.

We study the effect of X-ray illumination of the secondary star in a close binary on its internal structure and on the evolution of the system. We take into account the fact that X-ray heating is non-spherical and show that this modifies the results obtained in models which assume spherically symmetric illumination. Our results suggest that the effects of X-ray heating have been largely overestimated in earlier papers. We also show that radiation-induced winds in LMXBs with orbital periods less than 10 hr cannot give mass transfer rates larger than about one tenth of the Eddington limit mass flux, making it unlikely that such self-sustained winds have a marked effect on LMXB evolution, contrary to the suggestion of Tavani (1991)
Semiparametric Estimation of Signaling Games

This paper studies an econometric modeling of a signaling game with two players where one player has one of two types. In particular, we develop an estimation strategy that identies the payos structure and the distribution of types from data of observed actions. We can achieve uniqueness of equilibrium using a renement, which enables us to identify the parameters of interest. In the game, we consider non-strategic public signals about the types. Because the mixing distribution of these signals is nonparametrically specified, we propose to estimate the model using a sieve conditional MLE. We achieve the consistency and the asymptotic normality of the structural parameters estimates. As an alternative, we allow for the possibility of multiple equilibria, without using an equilibrium selection rule. As a consequence, we adopt a set inference allowing for multiplicity of equilibria.
Search for sub-parsec massive binary black holes through line diagnosis

We investigate the spectral properties of an active black hole, member of a massive (10 7 – 10 9 M� ) sub-parsec black hole binary. We work under the hypothesis that the binary, surrounded by a circumbinary disc, has cleared a gap, and that accretion occurs on to the secondary black hole fed by material closer to the inner edge of the disc. Broad line emission clouds orbit around the active black hole and suffer erosion due to tidal truncation at the Roche Lobe surface, following gap opening and orbital decay. We consider three of the most prominent broad emission lines observed in the spectra of active galactic nuclei (AGNs), i.e. C IV ,M gII and Hβ, and compute the flux ratios between the lines of Mg II and C IV (FMg II/FC IV) and those of Mg II and Hβ (FMg II/FHβ). We find that close black hole binaries have FMg II/FC IV up to 1 order of magnitude smaller than single black holes. By contrast FMg II/FHβ may be significantly reduced only at the shortest separations. Peculiarly low values of line flux ratios together with large velocity offsets between the broad and narrow emission lines and/or periodic variability in the continuum (on time-scales years) would identify genuine sub-pc binary candidates.
Hilbert schemes of rational curves on Fano hypersurfaces

In this paper we try to further explore the linear model of the moduli of rational maps. Our attempt yields following results. Let $X\subset \mathbf P^n$ be a generic hypersurface of degree $h$. Let $R_d(X, h)$ denote the open set of the Hilbert scheme parameterizing irreducible rational curves of degree $d$ on $X$. We obtain that (1) If $4\leq h\leq n-1$, $R_d(X, h)$ is an integral, local complete intersection of dimension \begin{equation} (n+1-h)d+n-4. \end{equation} (2) If furthermore $(h^2-n)d+h\leq 0$ and $h\geq 4$, in addition to part (1), $R_d(X, h)$ is also rationally connected.
The VISTA Carina Nebula Survey II. Spatial distribution of the infrared-excess-selected young stellar population

We performed a deep wide-field (6.76 deg^2) near-infrared survey with the VISTA telescope that covers the entire extent of the Carina nebula complex (CNC). The point-source catalog created from these data contains around four million individual objects down to masses of 0.1 M_sun. We present a statistical study of the large-scale spatial distribution and an investigation of the clustering properties of infrared-excesses objects, which are used to trace disk-bearing young stellar objects (YSOs). We find that a (J - H) versus (Ks - [4.5]) color-color diagram is well suited to tracing the population of YSO-candidates (cYSOs) by their infrared excess. We identify 8781 sources with strong infrared excess, which we consider as cYSOs. This sample is used to investigate the spatial distribution of the cYSOs with a nearest-neighbor analysis. The surface density distribution of cYSOs agrees well with the shape of the clouds as seen in our Herschel far-infrared survey. The strong decline in the surface density of excess sources outside the area of the clouds supports the hypothesis that our excess-selected sample consists predominantly of cYSOs with a low level of background contamination. This analysis allows us to identify 14 groups of cYSOs outside the central area. Our results suggest that the total population of cYSOs in the CNC comprises about 164000 objects, with a substantial fraction (~35%) located in the northern, still not well studied parts. Our cluster analysis suggests that roughly half of the cYSOs constitute a non-clustered, dispersed population.
A simultaneous 3.5 and 1.3 mm polarimetric survey of active galactic nuclei in the northern sky

Short millimeter observations of radio-loud AGN offer the opportunity to study the physics of their inner relativistic jets, from where the bulk millimeter emission is radiated. Millimeter jets are significantly less affected by Faraday rotation and depolarization than in radio. Also, the millimeter emission is dominated by the innermost jet regions, that are invisible in radio owing to synchrotron opacity. We present the first dual frequency simultaneous 86GHz and 229GHz polarimetric survey of all four Stokes parameters of a large sample of 211 radio loud active galactic nuclei, designed to be flux limited at 1Jy at 86GHz. The observations were most of them made in mid August 2010 using the XPOL polarimeter on the IRAM 30 m millimeter radio telescope. Linear polarization detections above 3 sigma median level of ~1.0% are reported for 183 sources at 86GHz, and for 23 sources at 229GHz, where the median 3 sigma level is ~6.0%. We show a clear excess of the linear polarization degree detected at 229GHz with regard to that at 86GHz by a factor of ~1.6, thus implying a progressively better ordered magnetic field for blazar jet regions located progressively upstream in the jet. We show that the linear polarization angle, both at 86 and 229GHz, and the jet structural position angle for both quasars and BL Lacs do not show a clear preference to align in either parallel or perpendicular directions. Our variability study with regard to the 86GHz data from our previous survey points out a large degree variation of total flux and linear polarization in time scales of years by median factors of ~1.5 in total flux, and ~1.7 in linear polarization degree -maximum variations by factors up to 6.3, and ~5, respectively-, with 86% of sources showing linear polarization angles evenly distributed with regard to our previous measurements.
Evolution of central dark matter of early-type galaxies up to z ∼ 0.8

We investigate the evolution of dark and luminous matter in the central regions of early-type galaxies (ETGs) up to z � 0.8. We use a spectroscopically selected sample of 154 cluster and field galaxies from the EDisCS survey, covering a wide range in redshifts (z �0.4–0.8), stellar masses (logM⋆/M⊙ � 10.5–11.5 dex) and velocity dispersions (σ⋆ � 100–300 km/s). We obtain central dark matter (DM) fractions by determining the dynamical masses from Jeans modelling of galaxy aperture velocity dispersions and the M⋆ from galaxy colours, and compare the results with local samples. We discuss how the correlations of central DM with galaxy size (i.e. the effective radius, Re), M⋆ and σ⋆ evolve as a function of redshift, finding clear indications that local galaxies are, on average, more DM dominated than their counterparts at larger redshift. This DM fraction evolution with z can be only partially interpreted as a consequence of the size–redshift evolution. We discuss our results within galaxy formation scenarios, and conclude that the growth in size and DM content which we measure within the last 7 Gyr is incompatible with passive evolution, while it is well reproduced in the multiple minor merger scenario. We also discuss the impact of the IMF on our DM inferences and argue that this can be non-universal with the lookback time. In particular, we find the Salpeter IMF can be better accommodated by low redshift systems, while producing stellar masses at high–z which are unphysically larger than the estimated dynamical masses (particularly for lower-σ⋆ systems).
Optical Polarimetry of the Inner Crab Nebula and Pulsar

Time-resolved polarisation measurements of pulsars oer an unique insight into the geometry of their emission regions. Such measurements provide observational constraints on the dierent models proposed for the pulsar emission mechanisms. Optical polarisation data of the Crab Nebula was obtained from the HST archive. The dataset consists of a series of observations of the nebula taken with the HST/ACS. We produced polarisation vector maps of the inner nebula and measured, for the rst time, the degree of linear polarisation (P.D.) and the position angle (P.A.) of the pulsar’s integrated pulse beam, and of its nearby synchrotron knot. This yielded P:D: = 5:2 0:3% and P:A: = 105:1 1:6 for the pulsar, and P:D: = 59:0 1:9% and P:A: = 124:7 1:0 for the synchrotron knot. This is the rst high-spatial resolution multi-epoch study of the polarisation of the inner nebula and pulsar. None of the main features in the nebula show evidence of signicant polarisation evolution in the period covered by these observations. The results for the pulsar are consistent with those obtained by S lowikowska et al. (2009) using the high-time resolution photo-polarimeter OPTIMA, once the DC component has been subtracted. Our results clearly prove that the knot is the main source of the DC component.
C18O DEPLETION IN STARLESS CORES IN TAURUS

We present here findings for C18O depletion in eight starless cores in Taurus: TMC-2, L1498, L1512, L1489, L1517B, L1521E, L1495A-S, and L1544. We compare observations of the C18O J = 2–1 transition taken with the ALMA prototype receiver on the Heinrich Hertz Submillimeter Telescope to results of radiative transfer modeling using RATRAN. We use temperature and density profiles calculated from dust continuum radiative transfer models to model the C18O emission. We present modeling of three cores, TMC-2, L1489, and L1495A-S, which have not been modeled before, and compare our results for the five cores with published models. We find that all of the cores but one, L1521E, are substantially depleted. We also find that varying the temperature profiles of these model cores has a discernable effect, and varying the central density has an even larger effect. We find no trends with depletion radius or depletion fraction with the density or temperature of these cores, suggesting that the physical structure alone is insufficient to fully constrain evolutionary state. We are able to place tighter constraints on the radius at which C18O is depleted than the absolute fraction of depletion. As the timeline of chemical depletion depends sensitively on the fraction of depletion, this difficulty in constraining depletion fraction makes comparison with other timescales, such as the free-fall timescale, very difficult.
Collaborative Contrastive Learning-Based Generative Model for Image Inpainting

The critical challenge of image inpainting is to infer reasonable semantics and textures for a corrupted image. Typical methods for image inpainting are built upon some prior knowledge to synthesize the complete image. One potential limitation is that those methods often remain undesired blurriness or semantic mistakes in the synthesized image while handling images with large corrupted areas. In this paper, we propose a Collaborative Contrastive Learning-based Generative Model (C2LGM), which learns the content consistency in the same image to ensure that the inferred content of corrupted areas is reasonable compared to the known content by pixel-level reconstruction and high-level semantic reasoning. C2LGM leverages the encoder-decoder based framework to directly learn the mapping from the corrupted image to the intact image and perform the pixel-level reconstruction. To perform semantic reasoning, our C2LGM introduces a Collaborative Contrastive Learning (C2L) mechanism that learns high-level semantic consistency between inferred and known content. Specifically, C2L mechanism introduces the high-frequency edge maps to participate in the process of typical contrastive learning and enables the deep model to ensure the semantic reasonableness between high-frequency structures and pixel-level content by pushing the representations of inferred content and known content close and keeping unrelated semantic content away in the latent feature space. Moreover, C2LGM also directly absorbs the prior knowledge of structural information from the proposed structural spatial attention module, and leverages the texture distribution sampling to improve the quality of synthesized content. As a result, our C2LGM achieves a 0.42 dB improvement over competing methods in terms of the PSNR metric while coping with a $40\thicksim 50$ % corruption ratio in the Places2 dataset. Extensive experiments on three benchmark datasets, including Paris Street View, CelebA-HQ, and Places2, demonstrate the advantages of our proposed C2LGM over other state-of-the-art methods for image inpainting both qualitatively and quantitatively.
Determination of the Most Appropriate Covariance Structure for Data with Missing Observations in Repeated Measures Design

Kantitatif bir ozellik bakimindan ayni deneme unitesinden farkli zaman periyotlarinda alinan ardisikolcumlere, tekrarlanan olcum denir. Iki faktorlu (muamele ve zaman) tekrarlanan olcumlu denemelerde, kuresellikvarsayiminin saglanmadigi durumda Repeated ANOVA (klasik yaklasim) yerine MIXED modelinin kullanilmasi,eksik/tam gozlemli verilerde cesitli kovaryans yapilarinin tanimlanmasina (CS, UN, AR (1), TOEPLITZ vs) olanaksaglamaktadir. Bu calismanin amaclari, tekrarlanan olcumlu denemeler icin kullanilan MIXED modellemekapsaminda, eksik gozlemler iceren mevcut veri setleri icin konu ile ilgili bazi varsayimlarin istatistikselgecerliligini (dogrulugunu) degerlendirmek ve bu veri setleri icin secilmis uygun kovaryans yapisinin secilmesikonusunda bilgi sahibi olmaktir. Bu amaclara ulasmak icin hayvancilik alaninda bir veri seti temin edilmistir. En iyikovaryans yapisi; AIC, BIC ve AICC uyum iyiligi olcutlerine gore secilmistir.Sonucta, bu calisma, tekrarlanan olcumlu denemelerde, kuresellik varsayiminin saglanmamasi durumundaMIXED model kullaniminin, eksik/tam gozlem iceren veri setleri icin ideal kovaryans yapilarini tanimlamada iyi birsecenek oldugunu acikca gostermistir.
The definition of environment and its relation to the quenching of galaxies at z = 1–2 in a hierarchical Universe

A well calibrated method to describe the environment of galaxies at all redshifts is essential for the study of structure formation. Such a calibration should include well understood correlations with halo mass, and the possibility to identify galaxies which dominate their potential well (centrals), and their satellites. Focusing on z = 1 and 2 we propose a method of environmental calibration which can be applied to the next generation of low to medium resolution spectroscopic surveys. Using an up-to-date semi-analytic model of galaxy formation, we measure the local density of galaxies in fixed apertures on different scales. There is a clear correlation of density with halo mass for satellite galaxies, while a significant population of low mass centrals is found at high densities in the neighbourhood of massive haloes. In this case the density simply traces the mass of the most massive halo within the aperture. To identify central and satellite galaxies, we apply an observationally motivated stellar mass rank method which is both highly pure and complete, especially in the more massive haloes where such a division is most meaningful. Finally we examine a test case for the recovery of environmental trends: the passive fraction of galaxies and its dependence on stellar and halo mass for centrals and satellites. With careful calibration, observationally defined quantities do a good job of recovering known trends in the model. This result stands even with reduced redshift accuracy, provided the sample is deep enough to preserve a wide dynamic range of density.
High Energy Effects of Noncommutative Spacetime Geometry

In this paper, we endeavour to obtain a modified form of the Foldy-Wouthuysen and Cini-Toushek transformations by resorting to the noncommutative nature of space-time geometry, starting from the Klein-Gordon equation. Also, we obtain a shift in the energy levels due to noncommutativity and from these results a limit for the Lorentz factor in the ultra-relativistic case has been derived in conformity with observations
Cosmic Microwave Background Acoustic Peak Locations

The Planck collaboration has measured the temperature and polarization of the cosmic microwave background well enough to determine the locations of eight peaks in the temperature (TT) power spectrum, five peaks in the polarization (EE) power spectrum and 12 extrema in the cross (TE) power spectrum. The relative locations of these extrema give a striking, and beautiful, demonstration of what we expect from acoustic oscillations in the plasma; e.g. that EE peaks fall half way between TT peaks. We expect this because the temperature map is predominantly sourced by temperature variations in the last scattering surface, while the polarization map is predominantly sourced by gradients in the velocity field, and the harmonic oscillations have temperature and velocity 90 deg out of phase. However, there are large differences in expectations for extrema locations from simple analytic models versus numerical calculations. Here, we quantitatively explore the origin of these differences in gravitational potential transients, neutrino free-streaming, the breakdown of tight coupling, the shape of the primordial power spectrum, details of the geometric projection from three to two dimensions, and the thickness of the last scattering surface. We also compare the peak locations determined from Planck measurements to expectations under the Λ cold dark matter model. Taking into account how the peak locations were determined, we find them to be in agreement.