Miracle-dz/UniFAR-FTUs huggingface dataset:
Constraints on Thermal X-Ray Radiation from SAX J1808.4–3658 and Implications for Neutron Star Neutrino Emission

Thermal X-ray radiation from neutron star soft X-ray transients in quiescence provides the strongest constraints on the cooling rates of neutron stars and thus on the interior composition and properties of matter in the cores of neutron stars. We analyze new (2006) and archival (2001) XMM-Newton observations of the accreting millisecond pulsar SAX J1808.4-3658 in quiescence, which provide the most stringent constraints to date. The X-ray spectrum of SAX J1808.4-3658 in the 2006 observation is consistent with a power law of photon index 1.83 ± 0.17, without requiring the presence of a blackbody-like component from a neutron star atmosphere. Our 2006 observation shows a slightly lower 0.5-10 keV X-ray luminosity, at a level of 68% of that inferred from the 2001 observation. Simultaneous fitting of all available XMM-Newton data allows a constraint on the quiescent neutron star (0.01-10 keV) luminosity of LNS < 1.1 × 1031 ergs s-1. This limit excludes some current models of neutrino emission mediated by pion condensates and provides further evidence of additional cooling processes, such as neutrino emission via direct Urca processes involving nucleons and/or hyperons, in the cores of massive neutron stars.
Simulated MRI Artifacts: Testing Machine Learning Failure Modes

Objective. Seven types of MRI artifacts, including acquisition and preprocessing errors, were simulated to test a machine learning brain tumor segmentation model for potential failure modes. Introduction. Real-world medical deployments of machine learning algorithms are less common than the number of medical research papers using machine learning. Part of the gap between the performance of models in research and deployment comes from a lack of hard test cases in the data used to train a model. Methods. These failure modes were simulated for a pretrained brain tumor segmentation model that utilizes standard MRI and used to evaluate the performance of the model under duress. These simulated MRI artifacts consisted of motion, susceptibility induced signal loss, aliasing, field inhomogeneity, sequence mislabeling, sequence misalignment, and skull stripping failures. Results. The artifact with the largest effect was the simplest, sequence mislabeling, though motion, field inhomogeneity, and sequence misalignment also caused significant performance decreases. The model was most susceptible to artifacts affecting the FLAIR (fluid attenuation inversion recovery) sequence. Conclusion. Overall, these simulated artifacts could be used to test other brain MRI models, but this approach could be used across medical imaging applications.
A Headless Tadpole Galaxy: The High Gas-phase Metallicity of the Ultra-diffuse Galaxy UGC 2162

The cosmological numerical simulations tell us that accretion of external metal-poor gas drives star formation (SF) in galaxy disks. One the best pieces of observational evidence supporting this prediction is the existence of low-metallicity star-forming regions in relatively high-metallicity host galaxies. The SF is thought to be fed by metal-poor gas recently accreted. Since the gas accretion is stochastic, there should be galaxies with all the properties of a host but without the low-metallicity starburst. These galaxies have not been identified yet. The exception may be UGC 2162, a nearby ultra-diffuse galaxy (UDG) that combines low surface brightness and relatively high metallicity. We confirm the high metallicity of UGC 2162 ( ) using spectra taken with the 10 m GTC telescope. UGC 2162 has the stellar mass, metallicity, and star formation rate surface density expected for a host galaxy in between outbursts. This fact suggests a physical connection between some UDGs and metal-poor galaxies, which may be the same type of object in a different phase of the SF cycle. UGC 2162 is a high-metallicity outlier of the mass–metallicity relation, a property shared by the few UDGs with known gas-phase metallicity.
Analysis of the arm spacing effect on symmetric and asymmetric Y-shape optical power splitters: plasmonic interactions between gold nanorings

In this paper, we investigated specific properties and features of several kinds of Y-splitters based on gold nanorings arrays which are surrounded by SiO 2 host substance, to be used at C-band spectrum (λ ~ 1550 nm). The comparison between two kinds of splitters shows that the symmetric splitter demonstrates better performance than the asymmetric splitter at given wavelength with high efficiency and transmittance (power ratio). Calculations proved that the transmitted power percentage was approximately ~47.5% in the well-organized splitter. It is shown that the offset distance plays an important role in the quality of the optical energy division and transmission through the plasmonic waveguide. The influence of increasing and decreasing in the offset distance was demonstrated numerically by snapshots. Hence, choosing and determining the appropriate value for the offset distance lead to the structure with lower losses and higher percentage in energy transmission. Ultimately, the optical behavior of an asymmetric nanostructure with unequal distances between the arms and the main array is investigated and its applications and possible purposes are introduced.
Optimization of Starburst99 for Intermediate-Age and Old Stellar Populations

We have incorporated the latest release of the Padova models into the evolutionary synthesis code Starburst99. The Padova tracks were extended to include the full asymptotic giant branch (AGB) evolution until the final thermal pulse over the mass range 0.9-5 M☉. With this addition, Starburst99 accounts for all stellar phases that contribute to the integrated light of a stellar population with arbitrary age from the extreme-ultraviolet to the near-infrared. AGB stars are important for ages between 0.1 and 2 Gyr, with their contribution increasing at longer wavelengths. We investigate similarities and differences between the model predictions by the Geneva and the Padova tracks. The differences are particularly pronounced at ages >1 Gyr, when incompleteness sets in for the Geneva models. We also perform detailed comparisons with the predictions of other major synthesis codes and find excellent agreement. Our synthesized optical colors are compared to observations of old, intermediate-age, and young populations. Excellent agreement is found for the old globular cluster system of NGC 5128 and for old and intermediate-age clusters in NGC 4038/4039. In contrast, the models fail for red supergiant-dominated populations with subsolar abundances. This failure can be traced back to incorrect red supergiant parameters in the stellar evolutionary tracks. Our models and the synthesis code are publicly available as version 5.0 of Starburst99 at http://www.stsci. edu/science/starburst99.
Measurement back action and spin noise spectroscopy in a charged cavity QED device in the strong coupling regime

We study theoretically the spin-induced and photon-induced fluctuations of optical signals from a singly-charged quantum dot-microcavity structure. We identify the respective contributions of the photon-polariton interactions, in the strong light-matter coupling regime, and of the quantum back-action induced by photon detection on the spin system. Strong spin projection by a single photon is shown to be achievable, allowing the initialization and measurement of a fully-polarized Larmor precession. The spectrum of second-order correlations is deduced, displaying information on both spin and quantum dot-cavity dynamics. The presented theory thus bridges the gap between the fields of spin noise spectroscopy and quantum optics.
Narrowing down the possible explanations of cosmic acceleration with geometric probes

Recent re-calibration of the Type Ia supernova (SNe Ia) magnitude-redshift relation combined with cosmic microwave background (CMB) and baryon acoustic oscillation (BAO) data have provided excellent constraints on the standard cosmological model. Here, we examine particular classes of alternative cosmologies, motivated by various physical mechanisms, e.g. scalar fields, modified gravity and phase transitions to test their consistency with observations of SNe Ia and the ratio of the angular diameter distances from the CMB and BAO. Using a model selection criterion for a relative comparison of the models (the Bayes Factor), we find moderate to strong evidence that the data prefer flat ΛCDM over models invoking a thawing behaviour of the quintessence scalar field. However, some exotic models like the growing neutrino mass cosmology and vacuum metamorphosis still present acceptable evidence values. The bimetric gravity model with only the linear interaction term as well as a simplified Galileon model can be ruled out by the combination of SNe Ia and CMB/BAO datasets whereas the model with linear and quadratic interaction terms has a comparable evidence value to standard ΛCDM. Thawing models are found to have significantly poorer evidence compared to flat ΛCDM cosmology under the assumption that the CMB compressed likelihood provides an adequate description for these non-standard cosmologies. We also present estimates for constraints from future data and find that geometric probes from oncoming surveys can put severe limits on non-standard cosmological models.
Short-Term Load Forecasting Model of Ameliorated CNN Based on Adaptive Mutation Fruit Fly Optimization Algorithm

Abstract In order to improve the accuracy and calculating speed of load forecasting for the strong nonlinear problem of short-term load, this article proposes a Short-term Load Forecasting Model of Ameliorated CNN Based on Adaptive Mutation Fruit Fly Optimization Algorithm. This method integrates the Extreme Learning Machine (ELM) algorithm into the Convolutional Neural Network (CNN): replace the fully connected layer in the original CNN network with ELM to form a CNN-ELM network. The purpose is to improve the calculation accuracy. An Adaptive Mutation Fruit Fly Optimization Algorithm (AMFOA) was proposed to reduce the probability that the Fruit Fly Optimization Algorithm (FOA) would easily fall into a local optimal value. And then AMFOA is used to optimize the parameters in CNN-ELM network. The above model is used to predict the grid load of a certain area in northern China. Compared with other prediction algorithms, it is proved that the model proposed in this article has higher prediction accuracy and also proved that the model has higher calculation speed than other models.
On the role of the measurement apparatus in quantum measurements

We study the extent to which the outcomes of a quantum measurement can be manipulated by changing the state of the measurement apparatus. The measurement process is modeled as decoherence induced by the experimenter, to gain knowledge about a particular system. The measurement apparatus is assumed to contain a large number of degrees of freedom, and the measurement outcomes are obtained by looking at the long interaction time limit. We study two cases which show contrasting behaviour. With a fixed axis coupling, the measurement is performed along the pointer basis with a high degree of robustness, for a wide variety of bath states. In a second model with Heisenberg interactions, the measurement outcomes can be altered considerably by changing the state of the bath.
Serum Lipid Variation in Patients with Dengue Virus Infection and Associated Risks of Cardio Vascular Disorder

Background: Dengue virus (DENV) is a most prevalent arbovirus with about 100 million infections worldwide every year. It is endemic in the subtropical and tropical areas in the world, an emerging public health threat. Serum lipidome is a key player in the immune system response of the patient for the period of dengue fever. This study was aimed to assess the lipids deviations in serum of patients with dengue fever. Materials and Methods: Three For this case-control study blood samples of N=65 dengue patients of age ≥18 year were collected from the Mayo Hospital, Lahore. Whereas samples of 45 healthy individuals were collected from the University of the Punjab, Lahore. Blood samples from subjects were collected to analyze serum lipidome. Results: Significantly (P < 0.001) increased serum triglyceride, total cholesterol, low density lipoprotein, and very low-density lipoprotein while a significant (P < 0.001) reduction in high density lipoprotein was observed in the dengue patient’s serum in contrast to the control. Conclusion: We can conclude that DENV infection can contribute to dyslipidemia with subsequent cardiovascular disorder symptoms. Therefore, patients infected with DENV should monitor their serum lipid profiles to deal with DENV induced effects to the cardiovascular physiology.
Structural, Surface Morphology and Optical Properties of Bi2O3 Thin Film Prepared By Reactive Pulse Laser Deposition.

In the present work, bismuth oxide Nanostructure thin film was prepared using reactive pulse laser deposition method. Optical, structural and surface morphology properties was carried out and the result insure the formation of polycrystalline Bi2O3 thin film with energy gap of (2.5) eV . The Atomic Force Microscopic Image show a Nano crystalline structure with average grain size of about (75.42 nm) .
Performance Prediction and Working Fluid Active Design of Organic Rankine Cycle Based on Molecular Structure

Working fluid selection is crucial for organic Rankine cycles (ORC). In this study, the relationship between molecular structure and ORC performance was established based on the quantitative structure–property relationship (QSPR) and working fluid parameterized model (WFPM), from which an ORC working fluid was actively designed. First, the QSPR model with four properties, namely, critical temperature (Tc), boiling point (Tb), critical pressure (pc), and isobaric heat capacity (cp0), was built. Second, the evaporation enthalpy (hvap), evaporation entropy (svap), and thermal efficiency (η) were estimated by WFPM, and the results were compared with those using REFPROP to verify the calculation accuracy of the “QSPR+WFPM” coupling model. The average absolute relative deviations of evaporation enthalpy and entropy are below 8.44%. The maximum relative error of thermal efficiency is 6%. Then, the thermodynamic performance limit of ORC and corresponding thermophysical properties of the ideal working fluid were calculated at typical geothermal source conditions. Finally, the active design of the working fluid was conducted with the ideal working fluid Tc and pc as the target. The research shows that C3H4F2 and C4H3F5 are optimal working fluids at 473.15 and 523.15 K heat sources, respectively.
Growth and feedback from the first black holes

Regardless of their initial seed mass, any active galactic nuclei observed at redshifts z > 6 must have grown by several orders of magnitude from their seeds. In this chapter, we will discuss the physical processes and latest research on black hole growth and associated feedback after seed formation. Fueling is initially slowed down by radiative feedback from the black hole itself and supernova explosions from nearby stars. Its growth however accelerates once the host galaxy grows past a critical mass.
KAON ELECTROPRODUCTION OFF PROTON

The elementary reaction of kaon exclusive electroproduction on protons has been studied ina broad kinematical range. Data for the calculation of the form factor of the kaon have been taken atdifferent values of the invariant center of mass energy W in the range W=1.8, 1.85, 1.98, 2.08 (GeV), forone value of the transferred 4-momentum Q2=2.35 (GeV/c)2. In this analysis, we calculated σL and σT byusing the Rosenbluth separation. Then the electromagnetic kaon form factor was calculated by Chew-Low extrapolation.
Star Formation Activity Beyond the Outer Arm. I. WISE-selected Candidate Star-forming Regions

The outer Galaxy beyond the Outer Arm provides a good opportunity to study star formation in an environment significantly different from that in the solar neighborhood. However, star-forming regions in the outer Galaxy have never been comprehensively studied or cataloged because of the difficulties in detecting them at such large distances. We studied 33 known young star-forming regions associated with 13 molecular clouds at RG ≥ 13.5 kpc in the outer Galaxy with data from the Wide-field Infrared Survey Explorer (WISE) mid-infrared all-sky survey. From their color distribution, we developed a simple identification criterion of star-forming regions in the outer Galaxy with the WISE color. We applied the criterion to all the WISE sources in the molecular clouds in the outer Galaxy at RG ≥ 13.5 kpc detected with the Five College Radio Astronomy Observatory (FCRAO) 12CO survey of the outer Galaxy, of which the survey region is 102. °49 ≤ l ≤ 141. °54, −3. °03 ≤ b ≤ 5. °41, and successfully identified 711 new candidate star-forming regions in 240 molecular clouds. The large number of samples enables us to perform the statistical study of star formation properties in the outer Galaxy for the first time. This study is crucial to investigate the fundamental star formation properties, including star formation rate, star formation efficiency, and initial mass function, in a primordial environment such as the early phase of the Galaxy formation.
Unraveling the Complex Structure of AGN-driven Outflows. III. The Outflow Size–Luminosity Relation

Energetic gas outflows driven by active galactic nuclei (AGNs) are considered as one of the mechanisms by which supermassive black holes affect their host galaxies. To probe the impact of AGN-driven outflows, it is essential to quantify the size of the region under the influence of such outflows. In the third of a series of papers, we present the spatially resolved kinematics of ionized gas for three additional Type 2 AGNs based on Gemini Multi-Object Spectrograph (GMOS) integral field spectroscopy. Along with the six AGNs presented in our previous works and the 14 AGNs with available GMOS-integral field unit data, we construct a sample of 23 luminous Type 2 AGNs at z < 0.2, and kinematically measure the size of ionized gas outflows by tracing the radial decrease of the velocity dispersion of the [O iii] λ5007 emission line. The kinematically measured outflow size ranges from 0.60 to ∼7.45 kpc, depending on AGN luminosity. We find that the size of the photoionized region is larger than the kinematically measured outflow size, while the flux-weighted photoionization size is significantly smaller. Thus, using photoionization size as a proxy for outflow size leads to overestimation or underestimation, and introduces large uncertainties of the mass outflow rate and the energy output rate. We report an outflow size–luminosity relation with a slope of 0.28 ± 0.03, which is shallower than the slope of the correlation between the photoionization size and luminosity.
Nature of Kinetic Scale Turbulence in the Earth's Magnetosheath

We present a combined observational and theoretical analysis to investigate the nature of plasma turbulence at kinetic scales in the Earth’s magnetosheath. In the first decade of the kinetic range, just below the ion gyroscale, the turbulence was found to be similar to that in the upstream solar wind: predominantly anisotropic, low-frequency and kinetic Alfvén in nature. A key difference, however, is that the magnetosheath ions are typically much hotter than the electrons, , which, together with , leads to a change in behavior in the second decade, close to electron scales. The turbulence here is characterized by an increased magnetic compressibility, following a mode we term the inertial kinetic Alfvén wave, and a steeper spectrum of magnetic fluctuations, consistent with the prediction that we obtain from a set of nonlinear equations. This regime of plasma turbulence may also be relevant for other astrophysical environments with , such as the solar corona, hot accretion flows, and regions downstream of collisionless shocks.
Inertial force, Hawking Temperature and Quantum Statistics

To explore the mechanism for the entropic force proposal in Entropic Gravity, we propose a specific thermodynamic process for states thermalized in local Hawking Temperature. We find when Casini's version of the Bekenstein bound is saturated, the thermodynamic force derived in the entanglement first law matches the local inertial force for the Schwarzschild solution, except for a negligible statistics-dependent factor. We argue the gravity viewed by static observers may have observable effects emerged from quantum statistics. The successful detailed calculation in this simple model inspires and is in support of the further development in our following research arXiv:2004.14059.
Distance, Energy, and Variability of Quasar Outflows: Two HST/COS Epochs of LBQS 1206+1052

We analyze new HST/COS spectra for two quasar absorption outflows seen in the quasi-stellar object LBQS 1206+1052. These data cover, for the first time, absorption troughs from S iv, Si ii, and P v. From the ratio of the S iv* to S iv column densities, we measure the electron number density of the higher-velocity (−1400 km s−1, v1400) outflow to be cm−3 and constrain the lower-velocity (−730 km s−1, v700) outflow to log(ne) > 5.3 cm−3. The ne associated with the higher-velocity outflow is an order of magnitude larger than reported in prior work. We find that the previous measurement was unreliable since it was based on density-sensitive absorption troughs that were likely saturated. Using photoionization models, we determine the best χ2-minimization fit for the ionization parameter and hydrogen column density of the higher-velocity outflow: log( and log( cm−2, respectively. We calculate from UH and ne a distance of pc from the central source to the outflow. Using an SED attenuated by the v700 outflow yields a two-phase photoionization solution for the v1400 outflow, separated by a . Otherwise, the resultant distance, mass flux, and kinetic luminosity are similar to the unattenuated case. However, the attenuated analysis has significant uncertainties due to a lack of constraints on the v700 outflow in 2017.
Quantum Spin Nematic States in Bose–Einstein Condensates

We review some recent results on discrete symmetries and topological order in spinor Bose–Einstein condensates (BECs) of 23Na. For spin one bosons with two-body scatterings dominated by a total spin equal to two channel, the BECs are in quantum spin nematic states at a low density limit. We study spin correlations in condensates at different limits and analyze hidden symmetries using a non-perturbative approach developed recently. Furthermore we investigate the influence of hidden Z2 symmetries and U(1) quantum orders in symmetry partially restored states, particularly the effects on topological excitations.