Miracle-dz/UniFAR-FTUs huggingface dataset:
Quintessence, Cosmology, and Fanaroff-Riley Type IIb Radio Galaxies

Fanaroff-Riley type IIb (FR IIb) radio galaxies provide a modified standard yardstick that allows constraints to be placed on global cosmological parameters. This modified standard yardstick is analogous to the modified standard candle provided by Type Ia supernovae. The radio galaxy and supernova methods provide a measure of the coordinate distance to high-redshift sources, and the coordinate distance is a function of global cosmological parameters. A sample of 20 FR IIb radio galaxies with redshifts between 0 and 2 are compared with the parent population of 70 radio galaxies to determine the coordinate distance to each source. The coordinate-distance determinations are used to constrain the current mean mass-energy density of quintessence ΩQ, the equation of state of the quintessence w, and the current mean mass-energy density of nonrelativistic matter Ωm; zero space curvature is assumed. Radio galaxies alone indicate that the universe is currently accelerating in its expansion (with 84% confidence); most of the allowed parameter space falls within the accelerating universe region on the Ωm-w plane. This provides verification of the acceleration of the universe indicated by high-redshift supernovae and suggests that neither method is plagued by systematic errors. It is found that Ωm must be less than about 0.5 and the equation of state w of the quintessence must lie between -0.25 and -2.5 at about 90% confidence. Fits of the radio galaxy data constrain the model parameter β, which describes a relation between the beam power of the active galactic nucleus (AGN) and the total energy expelled through large-scale jets. It is shown that the empirically determined model parameter is consistent with models in which the outflow results from the electromagnetic extraction of rotational energy from the central compact object. A specific relation between the strength of the magnetic field near the AGN and the spin angular momentum per unit mass of the central compact object is predicted.
RESULTS FROM LONG-TERM OPTICAL MONITORING OF THE SOFT X-RAY TRANSIENT SAX J1810.8−2609

In this paper, we report the long-term optical observation of the faint soft X-ray transient SAX J1810.8−2609 from the Optical Gravitational Lensing Experiment (OGLE) and Microlensing Observations in Astrophysics (MOA). We have focused on the 2007 outburst, and also cross-correlated its optical light curves and quasi-simultaneous X-ray observations from RXTE/Swift. Both the optical and X-ray light curves of the 2007 outburst show multi-peak features. Quasi-simultaneous optical/X-ray luminosity shows that both the X-ray reprocessing and viscously thermal emission can explain the observed optical flux. There is a slight X-ray delay of 0.6 ± 0.3 days during the first peak, while the X-ray emission lags the optical emission by ∼2 days during the rebrightening stage, which suggests that X-ray reprocessing emission contributes significantly to the optical flux in the first peak, but the viscously heated disk origin dominates it during rebrightening. This implies variation of the physical environment of the outer disk, with even the source remaining in a low/hard state during the entire outburst. The ∼2 day X-ray lag indicates a small accretion disk in the system, and its optical counterpart was not detected by OGLE and MOA during quiescence, which constrained it to be fainter than MI = 7.5 mag. There is a suspected short-time optical flare detected at MJD = 52583.5 with no detected X-ray counterpart; this single flux increase implies a magnetic loop reconnection in the outer disk, as proposed by Zurita et al. The observations cover all stages of the outburst; however, due to the low sensitivity of RXTE/ASM, we cannot conclude whether it is an optical precursor at the initial rise of the outburst.
GAMMA-RAY BURSTS FROM MAGNETIZED COLLISIONALLY HEATED JETS

Jets producing gamma-ray bursts (GRBs) are likely to carry a neutron component that drifts with respect to the proton component. The neutron–proton collisions strongly heat the jet and generate electron–positron pairs. We investigate radiation produced by this heating using a new numerical code. Our results confirm the recent claim that collisional heating generates the observed Band-type spectrum of GRBs. We extend the model to study the effects of magnetic fields on the emitted spectrum. We find that the spectrum peak remains near 1 MeV for the entire range of the magnetization parameter 0 < εB < 2 that is explored in our simulations. The low-energy part of the spectrum softens with increasing εB, and a visible soft excess appears in the keV band. The high-energy part of the spectrum extends well above the GeV range and can contribute to the prompt emission observed by Fermi/LAT. Overall, the radiation spectrum created by the collisional mechanism appears to agree with observations, with no fine tuning of parameters.
PARTICLE TRANSPORT IN YOUNG PULSAR WIND NEBULAE

The model for pulsar wind nebulae (PWNe) as a result of the magnetohydrodynamic (MHD) downstream flow from a shocked, relativistic pulsar wind has been successful in reproducing many features of the nebulae observed close to central pulsars. However, observations of well-studied young nebulae like the Crab Nebula, 3C 58, and G21.5–0.9 do not show the toroidal magnetic field on a larger scale that might be expected in the MHD flow model; in addition, the radial variation of spectral index due to synchrotron losses is smoother than expected in the MHD flow model. We find that pure diffusion models can reproduce the basic data on nebular size and spectral index variation for the Crab, 3C 58, and G21.5–0.9. Most of our models use an energy-independent diffusion coefficient; power-law variations of the coefficient with energy are degenerate with variation in the input particle energy distribution index in the steady state, transmitting boundary case. Energy-dependent diffusion is a possible reason for the smaller diffusion coefficient inferred for the Crab. Monte Carlo simulations of the particle transport allowing for advection and diffusion of particles suggest that diffusion dominates over much of the total nebular volume of the Crab. Advection dominates close to the pulsar and is likely to play a role in the X-ray half-light radius. The source of diffusion and mixing of particles is uncertain, but may be related to the Rayleigh–Taylor instability at the outer boundary of a young PWN or to instabilities in the toroidal magnetic field structure.
Reclust: an efficient clustering algorithm for mixed data based on reclustering and cluster validation

Clustering is a significant approach in data mining, which seeks to find groups or clusters of data. Both numeric and categorical features are frequently used to define the data in real-world applications. Several different clustering algorithms are proposed for the numerical and categorical datasets. In clustering algorithms, the quality of clustering results is evaluated using cluster validation. This paper proposes an efficient clustering algorithm for mixed numerical and categorical data using re-clustering and cluster validation. Initially, the mixed dataset is clustered with four traditional clustering algorithms like expectation-maximization (EM), hierarchical cluster (HC), k-means (KM), and self-organizing map (SOM). These four algorithms are validated, and the best algorithm is selected for re-clustering. It is an iterative process for improving the quality of cluster results. The incorrectly clustered data is iteratively re-clustered and evaluated based on the cluster validation. The performance of the proposed clustering method is evaluated with a real-time dataset in terms of purity, normalized mutual information, rand index, precision, and recall. The experimental results have shown that the proposed reclust algorithm achieves better performance compared to other clustering algorithms.
Component separation map-making for stochastic gravitational wave background

Superposition of unresolved sources of gravitational waves (GW) is expected to create a persistent background of stochastic gravitational wave background (SGWB). Different types of astrophysical and cosmological sources are however likely to be present in the background. We present an algorithm for separation of the components with distinct frequency spectral indices into individual sky-maps. To demonstrate the method, we simulate GW signals for different spectral indices and corresponding sky-maps, e.g., point sources like the Virgo cluster and extended ones like the Milky Way Galaxy, and apply our method to recover the injected maps.
On the origin of the fundamental metallicity relation and the scatter in galaxy scaling relations

We present a simple toy model to understand what sets the scatter in star formation and metallicity of galaxies at fixed mass. The scatter ultimately arises from the intrinsic scatter in the accretion rate, but may be substantially reduced depending on the timescale on which the accretion varies compared to the timescale on which the galaxy loses gas mass. This model naturally produces an anti-correlation between star formation and metallicity at a fixed mass, the basis of the fundamental metallicity relation. We show that observational constraints on the scatter in galaxy scaling relations can be translated into constraints on the galaxy-to-galaxy variation in the mass loading factor, and the timescales and magnitude of stochastic accretion onto star-forming galaxies. We find a remarkably small scatter in the mass loading factor, < 0.1 dex, and that the scatter in accretion rates is smaller than expected from N-body simulations.
Complete set of circuit equations for stabilizer quantum mechanics

We find a sufficient set of equations between quantum circuits from which we can derive any other equation between stabilizer quantum circuits. To establish this result, we rely upon existing work on the completeness of the graphical ZX language for quantum processes. The complexity of the circuit equations, as opposed to the very intuitive reading of the much smaller number of ZX-equations, advocates the latter for performing computations with quantum circuits.
Project Overview of the Beijing–Arizona Sky Survey

The Beijing–Arizona Sky Survey (BASS) is a wide-field two-band photometric survey of the northern Galactic Cap using the 90Prime imager on the 2.3 m Bok telescope at Kitt Peak. It is a four-year collaboration between the National Astronomical Observatory of China and Steward Observatory, the University of Arizona, serving as one of the three imaging surveys to provide photometric input catalogs for target selection of the Dark Energy Spectroscopic Instrument (DESI) project. BASS will take up to 240 dark/gray nights to cover an area of about 5400 deg2 in the g and r bands. The 5σ limiting AB magnitudes for point sources in the two bands, corrected for the Galactic extinction, are 24.0 and 23.4 mag, respectively. BASS, together with other DESI imaging surveys, will provide unique science opportunities that cover a wide range of topics in both Galactic and extragalactic astronomy.
Added Value of Multi-slice CT Scan (320 Slice) in Evaluation of Cardiac Complications Post COVID-19 Infection

Background: The COVID-19 pandemic had affected population health throughout the world. Few studies had focused on post-COVID19 complications detection using multi-slice CT scans. Our trial aimed to assess the value of cardiac CT utility during the COVID-19 pandemic for the detection of cardiac complications and correlation with the severity scoring system for chest manifestations. Since the beginning of COVID-19 outbreak, cardiac computed tomography (CT) had a sudden increased value and use with a huge reduction in face-to-face patient care and elective diagnostic testing. This study started from May 2021 to April 2022 in a single cardiac CT centre. This prospective cohort trial was conducted on 40 patients proved to have COVID-19 infection by positive RT-PCR test for COVID-19 and/or CT chest manifestations. CT results were reviewed and compared to echocardiography and/or catheterization data. Results: In the CT severity score, the more severe score for COVID-19 infection was noted in cases with coronary artery occlusion and pulmonary embolic diseases. Meanwhile, the mild and moderate severity score groups developed myocarditis, pericarditis, and dilated cardiomyopathy, respectively, with statically significant differences with p-value= 0.007 for coronary artery disease (CAD) and 0.026 for pulmonary embolism. The significance of echocardiography examination was noted in cases with pericarditis and dilated cardiomyopathy, with p-value= 0.018 for pericarditis and 0.01 for dilated cardiomyopathy. Conclusions: MSCT is a very useful technique to for patients presenting with suspected post-COVID cardiac complications, in addition to severity scoring of chest involvement, also providing its correlation with the occurrence of cardiac complications.
Empathy as a Mediator of the Effect of Dark Triad Personality, Social Support, and Demographic Factors on Cyberbullying Behavior in SMAN 10 Depok Students

This study examines empathy as a mediator of the dark triad personality, social support, and demographic factors on cyberbullying behavior in SMAN 10 Depok students. The study was conducted on 428 students of SMAN 10 with purposive sampling technique. The measuring tools used in this study are Tudkuea's Cyberbullying Scale, The Short Dark Triad (SD3), The Interpersonal Reactivity Index (IRI), and the Multidimensional Scale of Perceived Social Support (MSPSS). Data analysis using Path Analyze with MPlus 7.4 software. Based on the results of the analysis of the research data, a fit model was found so that it can be concluded that the theoretical model of Empathy as a mediator of the influence of dark triad personality, social support & demographic factors on cyberbullying behavior fits with empirical data. This means that Empathy acts as a mediator of the influence of dark triad personality, social support & demographic factors on cyberbullying behavior. Then the results of research data analysis related to direct influence reported that there was a significant effect of Machiavellianism and gender directly on cyberbullying, while narcissism, psychopathy, family support, peers support, and significant others had no significant effect on cyberbullying. In addition, the results of the hypothesis test also reported that there was a direct significant effect of narcissism, peers support and gender on Empathy, while there was no significant effect of psychopathic machiavellianism, family support and significant other (teachers) directly on Empathy.
Polyomino Models of Surface Supramolecular Assembly: Design Constraints and Structural Selectivity

We examine emergent properties of 2D supramolecular networks, using enumeration of configurations formed by interacting dominoes on square lattices as a simple model system. Possible ground states are identified using a convex hull construction in the interaction parameters for nearest-neighbour bonds. We demonstrate how this construction can be used to design interaction parameters which lead to networks with specific properties, including chirality and highly degenerate ground states. We then introduce kinetics as simple local rearrangements. By partitioning the configuration space into smaller sets which satisfy different topological constraints, we can design configurations which are kinetically trapped. By considering heat capacity curves along directions through the convex hull, we also demonstrate design of interacting domino configurations to create tilings robust against temperature induced phase transitions. We discuss extension of this design construction to more complex molecular shapes.
The Effectiveness of Lazarus Multimodal Approach on Psychological Distress, Working Memory, and Anxiety in Patients With Multiple Sclerosis

Background: Multiple sclerosis (MS) is considered a chronic disease in which physical and mental disorders are common among these patients. This study aimed to evaluate the effectiveness of the Lazarus multimodal approach intervention on psychological distress, working memory, and anxiety in patients with MS. Methods: A quasi-experimental research method with pre-test, post-test, and follow-up and a control group was used in this study. The statistical population of the study included the patients who were members of the "MS Patient Support Society" in Tehran who had been referred to this center during January and March 2017. The sample consisted of 32 people selected by the convenience sampling method from the members of the MS community. The data were obtained through the Kessler psychological distress scale (K10), the Wechsler’s Working Memory Index, and the Beck Anxiety Inventory. The experimental group underwent the Lazarus multimodal approach in ten 90-minute sessions of two sessions per week for one and a half months. The control group received no intervention. The follow-up was performed three months after the post-test. The repeated measurement method and SPSS 22 were used to analyze the data. Results: The findings showed that the Lazarus multimodal approach had a significant effect on decreasing anxiety (P<0.001), psychological distress (P<0.001), and increasing working memory (P<0.001). Conclusion: It can be concluded that Lazarus’ multimodal approach was effective on anxiety, psychological distress, and working memory and can be employed to reduce psychological problems in patients with MS.
COMPARISONS OF COSMOLOGICAL MAGNETOHYDRODYNAMIC GALAXY CLUSTER SIMULATIONS TO RADIO OBSERVATIONS

Radio observations of galaxy clusters show that there are μG magnetic fields permeating the intracluster medium (ICM), but it is hard to accurately constrain the strength and structure of the magnetic fields without the help of advanced computer simulations. We present qualitative comparisons of synthetic Very Large Array observations of simulated galaxy clusters to radio observations of Faraday rotation measure (RM) and radio halos. The cluster formation is modeled using adaptive mesh refinement magnetohydrodynamic simulations with the assumption that the initial magnetic fields are injected into the ICM by active galactic nuclei (AGNs) at high redshift. In addition to simulated clusters in Xu et al., we present a new simulation with magnetic field injections from multiple AGNs. We find that the cluster with multiple injection sources is magnetized to a similar level as in previous simulations with a single AGN. The RM profiles from simulated clusters, both |RM| and the dispersion of RM (σRM), are consistent at a first order with the radial distribution from observations. The correlations between the σRM and X-ray surface brightness from simulations are in a broad agreement with the observations, although there is an indication that the simulated clusters could be slightly overdense and less magnetized with respect to those in the observed sample. In addition, the simulated radio halos agree with the observed correlations between the radio power versus the cluster X-ray luminosity and between the radio power versus the radio halo size. These studies show that the cluster-wide magnetic fields that originate from AGNs and are then amplified by the ICM turbulence match observations of magnetic fields in galaxy clusters.
Effect of Alkali-Treatment on Physico-Chemical Properties of Typha Angustata Stem Fiber and Its Composites

ABSTRACT Recognizing the importance of using plant fibers in polymeric composites and the no availability of data on fine structure, physico-chemical, morphological and others properties of Typha Angustata stem fibers, a study was undertaken with the objective of determining some of these properties. In this work, untreated and treated Typha stem fibers by NaOH treatment have been extracted and characterized to evaluate and compare their surface condition as well as their chemical composition, their fine structure and their mechanical properties. Typha stem treated fibers (TSTFs) have presented best results with an alpha-cellulose content of 51.3%, a density of 1460 kg/m3, an average tensile strength equal to 9.42cN/tex and a diameter of 208.12 µm. Also, Crystallinity Index (CI) of TSTFs was 57.4%. Unsaturated polyester matrix was reinforced with TSTFs and mechanical properties were undergone. Results show that TSTFs could be used for sustainable fiber-reinforced polymer composites with an enhancement in flexural and tensile tests for 12.6% TSTFs ratio.
Squeezer-based pulsed optomechanical interface

We prove feasibility of high-fidelity pulsed optomechanical interface based on all-optical presqueezing of non-Gaussian quantum states of light before they enter the optomechanical system. We demonstrate that feasible presqueezing of optical states effectively increases the low noise transfer of them to mechanical oscillator. It allows one to surpass the limit necessary to transfer highly nonclassical states with negative Wigner function. In particular, we verify that with this help single photon states of light can be efficiently turned to single phonon states of mechanical oscillator, keeping the negativity of the Wigner function. It opens the possibility to merge quantum optomechanics with the recent methods of quantum optics.
Spectrum of a jet-emitting disc: application to the microquasar XTE J1118+480

Under the framework of the magnetized accretion ejection structures, we analyse the energy balance properties, and study the spectral energy distributions (SEDs) of the jet-emitting disc (JED) model for black hole X-ray transients. Various radiative processes are considered, i.e. synchrotron, bremsstrahlung, and their Comptonizations, and external Comptonization of radiation from the outer thin disc. With these cooling terms taken into account, we solve the thermal equilibrium equation self-consistently and find three solutions, of which the cold and the hot solutions are stable. Subsequently, we investigate the theoretical SEDs for these two stable solutions. We find the hot JED model can naturally explain the spectra of the Galactic microquasars in their hard states. As an example, we apply this model to the case of XTE J1118+480.
Position reconstruction in LUX

The (x, y) position reconstruction method used in the analysis of the complete exposure of the Large Underground Xenon (LUX) experiment is presented. The algorithm is based on a statistical test that makes use of an iterative method to recover the photomultiplier tube (PMT) light response directly from the calibration data. The light response functions make use of a two dimensional functional form to account for the photons reflected on the inner walls of the detector. To increase the resolution for small pulses, a photon counting technique was employed to describe the response of the PMTs. The reconstruction was assessed with calibration data including 83mKr (releasing a total energy of 41.5 keV) and 3H (β− with Q = 18.6 keV) decays, and a deuterium-deuterium (D-D) neutron beam (2.45 MeV) . Within the detector's fiducial volume, the reconstruction has achieved an (x, y) position uncertainty of σ = 0.82 cm and σ = 0.17 cm for events of only 200 and 4,000 detected electroluminescence photons respectively. Such signals are associated with electron recoils of energies ∼0.25 keV and ∼10 keV, respectively. The reconstructed position of the smallest events with a single electron emitted from the liquid surface (22 detected photons) has a horizontal (x, y) uncertainty of 2.13 cm.