Miracle-dz/UniFAR-FTUs huggingface dataset:
Wide binary companions to massive stars and their use in constraining natal kicks

The origin of ultra-wide massive binaries (orbital separations $10^3-2\times 10^5$~AU) and their properties are not well characterized nor understood. Here we use the second Gaia data release to search for wide astrometric companions to Galactic O-B5 stars which share similar parallax and proper motion with the primaries. Using the data we characterize the frequency and properties of such binaries. We find an ultra-wide multiplicity fraction of $4.4\pm0.5$ per cent, to our completeness limit (up to $\approx 17$~mag; down to G-stars at distances of 0.3-2~kpc, excluding stars in clusters). The secondary mass-function is generally consistent with a Kroupa initial stellar function; if extrapolated to lower mass companion stars we then might expect a wide-binary fraction of $\sim 27\pm5\%$. In addition we use these data as a verification sample to test the existence of ultra-wide binaries among neutron stars (NSs) and black holes (BHs). We propose that the discovery of such binary can provide unique constraints on the weakest natal kicks possible for NSs/BHs. If a compact object is formed in an ultra-wide binary and receives a very-low natal kick, such a binary should survive as a common proper motion pair. We therefore use Gaia data to search for ultra-wide companions to pulsars (normal and millisecond ones) and X-ray binaries. We find no reliable pairs. Future data could potentially provide stringent constraints through this method.
Accuracy of Machine Learning Classification Models for the Prediction of Type 2 Diabetes Mellitus: A Systematic Survey and Meta-Analysis Approach

Highlights We reviewed soft-computing and statistical learning methods for predicting type 2 diabetes mellitus. We searched for papers published between 2010 and 2021 on three academic search engines, obtaining 34 relevant documents for the final meta-analysis. We analyzed the data extracted, compared the results and models, discussed their performance, and highlighted the issues related to T2DM. Finally, the decision trees model has the best prediction performances, with excellent accuracy compared to other soft-computing models in this systematic meta-analysis. Abstract Soft-computing and statistical learning models have gained substantial momentum in predicting type 2 diabetes mellitus (T2DM) disease. This paper reviews recent soft-computing and statistical learning models in T2DM using a meta-analysis approach. We searched for papers using soft-computing and statistical learning models focused on T2DM published between 2010 and 2021 on three different search engines. Of 1215 studies identified, 34 with 136952 patients met our inclusion criteria. The pooled algorithm’s performance was able to predict T2DM with an overall accuracy of 0.86 (95% confidence interval [CI] of [0.82, 0.89]). The classification of diabetes prediction was significantly greater in models with a screening and diagnosis (pooled proportion [95% CI] = 0.91 [0.74, 0.97]) when compared to models with nephropathy (pooled proportion = 0.48 [0.76, 0.89] to 0.88 [0.83, 0.91]). For the prediction of T2DM, the decision trees (DT) models had a pooled accuracy of 0.88 [95% CI: 0.82, 0.92], and the neural network (NN) models had a pooled accuracy of 0.85 [95% CI: 0.79, 0.89]. Meta-regression did not provide any statistically significant findings for the heterogeneous accuracy in studies with different diabetes predictions, sample sizes, and impact factors. Additionally, ML models showed high accuracy for the prediction of T2DM. The predictive accuracy of ML algorithms in T2DM is promising, mainly through DT and NN models. However, there is heterogeneity among ML models. We compared the results and models and concluded that this evidence might help clinicians interpret data and implement optimum models for their dataset for T2DM prediction.
High-Speed Optical Spectroscopy of a Cataclysmic Variable Wind: BZ Camelopardalis

BZ Camelopardalis is the first cataclysmic variable star with an accretion disk wind evident in its optical spectrum. The wind was found by Thorstensen, who discovered intermittent P Cygni profiles occurring simultaneously in He I λ5876 and Hα. We have since obtained spectra with 0.4 Å pixel-1 dispersion and 60 s time resolution. We find a much faster and more rapidly variable wind than the radiatively accelerated ones of OB stars, Wolf-Rayet stars, or luminous blue variables. Instead of showing blob ejection, the whole wind of BZ Cam appears to turn on and off. We use this to measure the acceleration law of a CV wind for the first time. The velocity increases linearly with time, attaining blue edge velocities near -3000 km s-1, and absorption velocities near -1700 km s-1, in 6 to 8 minutes after starting near rest. We also find a subsequent linear deceleration to nearly rest in 30–40 minutes, perhaps an effect of dilution as the wind expands. No periodicity from rotational outflow is obvious. This wind is erratic and incessantly variable, and perhaps bipolar and face-on, but not highly collimated. The P Cygni absorption events trace out sawtooth waves, occurring within 30 to 40 white dwarf radii from the disk. This is the approximate size of the disk, as well as the disk/wind transition region recently postulated by Knigge & Drew. We estimate a distance of 830 ± 160 pc and an orbital inclination i such that 12° ≲ i < 40°.
TIDAL EVOLUTION OF THE SPIN–ORBIT ANGLE IN EXOPLANETARY SYSTEMS

The angle between the stellar spin and the planetary orbit axes (the spin–orbit angle) is supposed to carry valuable information concerning the initial condition of planetary formation and subsequent migration history. Indeed, current observations of the Rossiter–McLaughlin effect have revealed a wide range of spin–orbit misalignments for transiting exoplanets. We examine in detail the tidal evolution of a simple system comprising a Sun-like star and a hot Jupiter adopting the equilibrium tide and the inertial wave dissipation effects simultaneously. We find that the combined tidal model works as a very efficient realignment mechanism; it predicts three distinct states of the spin–orbit angle (i.e., parallel, polar, and antiparallel orbits) for a while, but the latter two states eventually approach the parallel spin–orbit configuration. The intermediate spin–orbit angles as measured in recent observations are difficult to obtain. Therefore the current model cannot reproduce the observed broad distribution of the spin–orbit angles, at least in its simple form. This indicates that the observed diversity of the spin–orbit angles may emerge from more complicated interactions with outer planets and/or may be the consequence of the primordial misalignment between the protoplanetary disk and the stellar spin, which requires future detailed studies.
Comparative Evaluation of Surface Roughness and Wettability of an Alkasite with Nano Bulk-Fill and Nanofilled Resin Composite Restorative Materials: In vitro Study

Context: Surface characteristics of resin-based composites (RBCs) can change with polishing and over time. Aim: The aim of the study was to compare the surface roughness and wettability of three different posterior RBCs after polishing and the change in these surface characteristics over time, after aqueous aging. Settings and Design: Experimental in vitro study. Materials and Methods: Eleven disc-shaped RBC specimens were fabricated. The RBCs used were, alkasite composite, bulk-fill nanocomposite, conventional nanofilled composite. All the specimens underwent polishing with Soflex Diamond Polishing System and then analyzed for roughness and wettability at baseline and after aqueous aging for 3 months with the help of an atomic force microscope and a contact angle goniometer respectively. Statistical Analysis: One-way ANOVA and Tamhane test were used for the multiple comparisons. Results: Alkasite composite showed significantly higher surface roughness (P = 0.028 and P < 0.001, respectively) and lower wettability (P = 0.023 and P = 0.020, respectively) than conventional nanofilled composite at baseline and 3 months. Surface roughness of alkasite composite was also significantly higher than bulk-fill nanocomposite (P = 0.009 and P < 0.001, respectively) at both the time points. Conclusions: Alkasite has higher surface roughness in comparison to conventional nanocomposite and bulk-fill nanocomposite and lower wettability than conventional nanocomposite after polishing and aqueous aging over a 3-month period. In terms of surface characteristics, alkasite composite may be advantageous in preventing initial plaque adhesion to the material surface, but the lower surface roughness of nano-filled composites may be more advantageous in terms of plaque retention prevention.
Asymptotically flat black holes and gravitational waves in three-dimensional massive gravity

Different classes of exact solutions for the BHT massive gravity theory are constructed and analyzed. We focus in the special case of the purely quadratic Lagrangian, whose field equations are irreducibly of fourth order and are known to admit asymptotically locally flat black holes endowed with gravitational hair. The first class corresponds to a Kerr-Schild deformation of Minkowski spacetime along a covariantly constant null vector. As in the case of General Relativity, the field equations linearize so that the solution can be easily shown to be described by four arbitrary functions of a single null coordinate. These solutions can be regarded as a new sort of pp-waves. The second class is obtained from a deformation of the static asymptotically locally flat black hole, that goes along the spacelike (angular) Killing vector. Remarkably, although the deformation is not of Kerr-Schild type, the field equations also linearize, and hence the generic solution can be readily integrated. It is neither static nor spherically symmetric, being described by two integration constants and two arbitrary functions of the angular coordinate. In the static case it describes "black flowers" whose event horizons break the spherical symmetry. The generic time-dependent solution appears to describe a graviton that moves away from a black flower. Despite the asymptotic behaviour of these solutions at null infinity is relaxed with respect to the one for General Relativity, the asymptotic symmetries coincide. However, the algebra of the conserved charges corresponds to BMS$_{3}$, but devoid of central extensions. The "dynamical black flowers" are shown to possess a finite energy. The surface integrals that define the global charges also turn out to be useful in the description of the thermodynamics of solutions with event horizons.
Degenerate Plebanski sector and spin foam quantization

We show that the degenerate sector of Spin(4) Plebanski formulation of four-dimensional gravity is exactly solvable and describes covariantly embedded SU(2) BF theory. This fact ensures that its spin foam quantization is given by the SU(2) Crane–Yetter model and allows to test various approaches of imposing the simplicity constraints. Our analysis strongly suggests that restricting representations and intertwiners in the state sum for Spin(4) BF theory is not sufficient to get the correct vertex amplitude. Instead, for a general theory of Plebanski type, we propose a quantization procedure which is by construction equivalent to the canonical path integral quantization and, being applied to our model, reproduces the SU(2) Crane–Yetter state sum. A characteristic feature of this procedure is the use of secondary second class constraints on an equal footing with the primary simplicity constraints, which leads to a new formula for the vertex amplitude.
Rigorous limits on the interaction strength in quantum field theory

We derive model-independent, universal upper bounds on the operator product expansion coefficients in unitary 4-dimensional conformal field theories. The method uses the conformal block decomposition and the crossing symmetry constraint of the 4-point function. In particular, the operator product expansion coefficient of three identical dimension d scalar primaries is found to be bounded by {approx_equal}10(d-1) for 1<d<1.7. This puts strong limits on unparticle self-interaction cross sections at the LHC.
Differences in the Morphological Characteristics and Body Composition between Elite Montenegrin Kata and Kumite Karatekas

Elite karatekas should have specific morphological characteristics suitable for their specializations. This study aimed to determine the differences in morphological characteristics and body composition of elite Montenegrin karate athletes according to different specializations. This study consisted of a total of 16 male karate athletes divided according to specialization in kata (form or movement pattern) and kumite (fighting) disciplines. The subject sample included healthy, black belt karate senior athletes, with no prior injuries divided into kata (n-6, 19.83±4.71 years) and kumite (n-10, 20.4±5.21 years) athletes. Morphological characteristics and body composition were evaluated by a battery of 11 variables: body height (BH), body mass (BM), triceps skinfold (TS), biceps skinfold (BiS), back skinfold (BS), abdominal skinfold (AS), upper leg skinfold (UlS), lower leg skinfold (LlS), body mass index (BMI), fat percentage (FP), and muscle mass percentages (MP). The differences in morphological characteristics and the composition of the body between kata and kumite karatekas were determined by using a statistical procedure with a t-test for small independent samples. It was determined that the kumite had a higher body height, and body weight, as well as a higher percentage of muscle mass than kata karatekas. In other parameters concerning the distribution of subcutaneous adipose tissue, as well as the percentage of body fat, there was no difference between the groups. The results suggest that there is some difference in morphological characteristics between kata and kumite karatekas, but for more complete conclusions an analysis should be performed on a larger sample of high-level karate athletes.
THE ABSENCE OF COLD DUST AND THE MINERALOGY AND ORIGIN OF THE WARM DUST ENCIRCLING BD +20 307

Spitzer Space Telescope photometry and spectroscopy of BD +20 307 show that all of the dust around this remarkable Gyr-old spectroscopic binary arises within 1 AU. No additional cold dust is needed to fit the infrared excess. Peaks in the 10 and 20 μm spectrum are well fit with small silicates that should be removed on a timescale of years from the system. This is the dustiest star known for its age, which is ≳1 Gyr. The dust cannot arise from a steady-state collisional cascade. A catastrophic collision of two rocky, planetary-scale bodies in the terrestrial zone is the most likely source for this warm dust because it does not require a reservoir of planetesimals in the outer system.
BLOOD TIES: THE REAL NATURE OF THE LMC BINARY GLOBULAR CLUSTERS NGC 2136 AND NGC 2137

We have used a sample of high-resolution spectra obtained with the multi-fiber facility FLAMES at the Very Large Telescope of the European Southern Observatory to derive the kinematical and chemical properties of the two young Large Magellanic Cloud (LMC) globular clusters NGC 2136 and NGC 2137. These two clusters represent a typical example of LMC cluster pair suspected to be bound in a binary system: indeed, the cluster centers of gravity have an angular separation of less than 1.4 arcmin in the sky. The spectral analysis of seven giants in NGC 2136 and four in NGC 2137 reveals that the two clusters share very similar systemic radial velocities, namely, Vr = 271.5 ± 0.4 km s−1 (σ = 1.0 km s−1) and Vr = 270.6 ± 0.5 km s−1 (σ = 0.9 km s−1) for NGC 2136 and NGC 2137, respectively, and they have also indistinguishable abundance patterns. The iron content is [Fe/H] = −0.40 ± 0.01 dex (σ = 0.03 dex) for NGC 2136 and −0.39 ± 0.01 dex (σ = 0.01 dex) for NGC 2137, while the [α/Fe] ratios are roughly solar in both clusters. These findings suggest that the two clusters are gravitationally bound and that they formed from the fragmentation of the same molecular cloud that was chemically homogeneous. This is the first firm confirmation of the binary nature of an LMC cluster pair. The most likely fate of this system is to merge into a single structure in a timescale comparable with its orbital period.
The large area KX quasar catalogue – I. Analysis of the photometric redshift selection and the complete quasar catalogue

The results of a large area, ∼600 deg2, K-band flux-limited spectroscopic survey for luminous quasars are presented. The survey utilizes the UKIRT Infrared Deep Sky Survey (UKIDSS) Large Area Survey (LAS) in regions of sky within the Sloan Digital Sky Survey (SDSS) footprint. The K-band excess (KX) of all quasars with respect to Galactic stars is exploited in combination with a photometric redshift/classification scheme to identify quasar candidates for spectroscopic follow-up observations. The data contained within this investigation will be able to provide new constraints on the fraction of luminous quasars reddened by dust with E(B − V) ≤ 0.5 mag. The spectroscopic sample is defined using the K-band, 14.0 ≤ K ≤ 16.6, and SDSS i-band limits of i = 19.5, 19.7 and 22.0 over sky areas of 287, 150 and 196 deg2, respectively. The survey includes >3200 known quasars from the SDSS and more than 250 additional confirmed quasars from the KX selection. A well-defined subsample of quasars in the redshift interval 1.0 ≤ z ≤ 3.5 includes 1152 objects from the SDSS and 172 additional KX-selected quasars. The quasar selection is >95 per cent complete with respect to known SDSS quasars and >95 per cent efficient, largely independent of redshift and i-band magnitude. The properties of the new KX-selected quasars confirm the known redshift-dependent effectiveness of the SDSS quasar selection and provide a sample of luminous quasars experiencing intermediate levels of extinction by dust. The catalogue represents an important step towards the assembly of a well-defined sample of luminous quasars that may be used to investigate the properties of quasars experiencing intermediate levels of dust extinction within their host galaxies or due intervening absorption line systems.
Systane iLux Thermal Pulsation System in the Treatment of Meibomian Gland Dysfunction: A Post-Hoc Analysis of a 12-Month, Randomized, Multicenter Study

Purpose This study aimed to demonstrate the effectiveness of Systane iLux, a thermal pulsation device, in patients with MGD, over 12 months post-single treatment. Methods This is a post-hoc analysis of a previous prospective, assessor-masked, parallel-group, multicenter study (NCT03956225) that compared the effectiveness and safety of iLux with LipiFlow in subjects with MGD. The original study included subjects with meibomian gland score (MGS) ≤12 in lower eyelids, Impact of Dry Eye on Everyday Life-Symptom Bother (IDEEL-SB) module score >16, and non-invasive tear break-up time (NITBUT) <10 seconds. Subjects were randomized (1:1) to receive a single bilateral treatment of iLux or LipiFlow. In this post-hoc analysis, mean changes in MGS, NITBUT (first break-up; seconds), IDEEL-SB module score, and corneal staining, from baseline to 12 months were analyzed post-single treatment with iLux. Results Data from 119 patients (n=238 eyes) treated with iLux were analyzed. The mean±SD age of the subjects was 58.4±13.4 years, with majority being female (79.0%). MGS (mean±SD) for both eyes improved significantly from baseline to 12 months (OD [baseline: 6.9±3.69; month 12: 22.8±11.31; change: 15.9±11.57, p<0.0001]; OS [baseline: 6.4±3.66; month 12: 23.0±11.33; change: 16.7±11.40, p<0.0001]). Similarly, significant improvements were observed in NITBUT (OD [baseline: 5.2±1.97; month 12: 7.0±3.68; change: 1.9±3.69, p<0.0001]; OS [baseline: 5.6±1.96; month 12: 7.9±4.58; change: 2.3±4.59, p<0.0001]) and IDEEL-SB score (p<0.0001). Corneal staining reduced significantly from baseline to 12 months (OD [baseline: 2.1±2.96; month 12: 0.7±1.56; change: −1.4±2.65, p<0.0001]; OS [baseline: 2.1±2.94; month 12: 0.7±1.44; change: −1.4±2.75, p<0.0001]). Improvements in MGS, NITBUT, IDEEL-SB module score, and corneal staining were seen as early as week 2, and at months 1, 3, 6, and 9 (all p<0.001). Conclusion A single treatment with iLux significantly improved clinical parameters of MGS, NITBUT, and corneal staining, and patient-reported symptom assessment with IDEEL-SB in patients with MGD over 12 months.
Crystal growth and magnetic structure of 
MnBi2Te4

Millimeter-sized MnBi$_2$Te$_4$ single crystals are grown out of Bi-Te flux and characterized by measuring magnetic and transport properties, scanning tunneling microscope (STM) and spectroscopy (STS). The magnetic structure of MnBi$_2$Te$_4$ below T$_N$ is determined by powder and single crystal neutron diffraction measurements. Below T$_N$=24\,K, Mn$^{2+}$ moments order ferromagnetically in the \textit{ab} plane but antiferromagnetically along the crystallographic \textit{c} axis. The ordered moment is 4.04(13) $\mu_{B}$/Mn at 10\,K and aligned along the crystallographic \textit{c}-axis. The electrical resistivity drops upon cooling across T$_N$ or when going across the metamagnetic transition in increasing fields below T$_N$. A critical scattering effect was observed in the vicinity of T$_N$ in the temperature dependence of thermal conductivity. However, A linear temperature dependence was observed for thermopower in the temperature range 2K-300K without any anomaly around T$_N$. These indicate that the magnetic order in Mn-Te layer has negligible effect on the electronic band structure, which makes possible the realization of proposed topological properties in MnBi$_2$Te$_4$ after fine tuning of the electronic band structure.
Interstellar dimethyl ether gas-phase formation: a quantum chemistry and kinetics study

Dimethyl ether is one of the most abundant interstellar complex organic molecules. Yet its formation route remains elusive. In this work, we have performed electronic structure and kinetics calculations to derive the rate coefficients for two ion-molecule reactions recently proposed as a gas-phase formation route of dimethyl ether in interstellar objects, namely CH$_3$OH + CH$_3$OH$_2^+$ $\rightarrow$ (CH$_3$)$_2$OH$^+$ + H$_2$O followed by (CH$_3$)$_2$OH$^+$ + NH$_3$ $\rightarrow$ CH$_3$OCH$_3$ + NH$_4^+$. A comparison with previous experimental rate coefficients for the reaction CH$_3$OH + CH$_3$OH$_2^+$ sustains the accuracy of the present calculations and allow a more reliable extrapolation at the low temperatures of interest in interstellar objects (10-100 K). The rate coefficient for the reaction (CH$_3$)$_2$OH$^+$ + NH$_3$ is, instead, provided for the first time ever. The rate coefficients derived in this work essentially confirm the prediction by Taquet et al. (2016) concerning dimethyl ether formation in hot cores/corinos. Nevertheless, this formation route cannot be efficient in cold objects (like prestellar cores) where dimethyl ether is also detected, because ammonia has a very low abundance in those environments.