Miracle-dz/UniFAR-FTUs huggingface dataset:
The Roles of Vitamins in Diabetic Retinopathy: A Narrative Review

There have been attempts to evaluate the roles of vitamins for the prevention or treatment of eye conditions, such as glaucoma, age-related macular degeneration, and diabetic retinopathy (DR). Regarding DR, two main groups of studies can be identified. The first group focuses on the association between serum levels of an individual vitamin and DR. Many studies have found that lower serum levels of vitamins, particularly vitamin D, are significantly associated with the development, or severity, of DR, while some studies have not supported this trend. The second group evaluates dietary vitamin intakes and DR. A small, randomized placebo-controlled trial did not show any benefit of vitamin E intake on improving the area of retinal hemorrhage or diabetic macular edema at 12 months. A pilot study of patients with mild-to-moderate non-proliferative DR received tablets of combined vitamins B6, B9, and B12 for 6 months and significant improvement in retinal sensitivity and retinal thickness resulted. Two large prospective cohorts showed that high dietary intake of vitamin B6, and fruit rich in vitamin C and E, could significantly lower the risk of DR by 50% after an eight-year follow-up. Properly designed, randomized controlled trials are needed to support the results.
A closer look at the cosmological implications of the ΛHDE model

In a previous paper, we proposed a heterotic dark energy model, called Λ holographic dark energy (ΛHDE), in which dark energy is composed of two components: cosmological constant (CC) and HDE. The aim of this work is to give a more comprehensive and systematic investigation on the cosmological implications of the ΛHDE model. First, we make use of the current observations to constrain the ΛHDE model, and compare its cosmology-fit results with the results of the Λ cold dark matter (ΛCDM) and the HDE model. Then, by combining a qualitative theoretical analysis with a quantitative numerical study, we discuss the impact of considering curvature on the cosmic evolutions of fractional HDE density Ω_hde and fractional CC density Ω_Λ, as well as on the ultimate cosmic fate. Finally, we explore the effects of adopting different types of observational data. We find that: (1) the current observational data cannot distinguish the ΛHDE model from the ΛCDM and the HDE model; this indicates that dark energy (DE) may contain multiple components. (2) The asymptotic solution of Ω_hde and the corresponding cosmic fate in a flat universe can be extended to the case of a non-flat universe; moreover, compared with the case of a flat universe, considering curvature will make HDE closer to a phantom DE. (3) Compared with Joint Light-curve Analysis (JLA) data set, Supernova Legacy Survey three-years (SNLS3) data more favour a phantom type HDE; in contrast, using other types of observational data have no significant impact on the cosmic evolutions of the ΛHDE model.
Commute based learning: Integrating literature across transportation, education, and i-o psychology

Though commuting is often seen as a source of stress, commuters may take advantage of travel time to pursue learning and developmental goals—a concept we refer to as Commute-Based Learning (CBL). We draw on self-regulation and learning and development theories to define CBL in terms of its context, content, and process and present the findings of a systematic review of multitasking activities in the transportation literature. This review demonstrates that (a) travel-based activities related to learning are increasingly prevalent, (b) people enjoy being productive during their commutes, and (c) commute mode and environmental characteristics impact multitasking and evaluations of the commute itself. We then integrate these review findings with psychological theories to propose a framework specifying the predictors of CBL, its benefits, and drawbacks, and the commute mode's moderating influence. These efforts yield several practical implications and future research directions to increase CBL's potential benefits while reducing potential harm. Plain Language Summary Although commuting can often be a source of stress, commuters may also take advantage of travel time to pursue learning and developmental goals—a concept we refer to as Commute-Based Learning (CBL). To emphasize the potential benefits and pitfalls of CBL, we draw on learning and development, self-regulation, multiple-goal pursuit, and multiple resource theories to define CBL in terms of its context (where it occurs), content (what it includes), and process (how it is done). Next, we present the findings of a systematic review ofresearch on multitasking activities in the transportation literature to gather evidence of the learning activities that commuters may pursue.This review demonstrates that (a) travel-based activities related to learning are increasingly prevalent, (b) people enjoy being productive during their commutes, and (c)commute mode and environmental characteristics impact multitasking and evaluations of the commute itself. We then integrate these findings from the transportation literature with psychological theories to propose a framework specifying the predictors of CBL (individual and organizational), its benefits (expertise, need satisfaction and well-being) and drawbacks (depletion, reduced safety), and the critical role of commute mode as a moderator of these relationships. Our definition and framework of CBL inform practical implications for improving the benefits of learning during the commute, while mitigating its potential drawbacks. We also present suggested directions for future multidisciplinary research. We hope this review provides insight into the state of the literature on commute-based learning and a clear research agenda for advancement in this broadly important, yet underdeveloped area.
TRANSIT AND ECLIPSE ANALYSES OF THE EXOPLANET HD 149026b USING BLISS MAPPING

The dayside of HD 149026b is near the edge of detectability by the Spitzer Space Telescope. We report on 11 secondary-eclipse events at 3.6, 4.5, 3 × 5.8, 4 × 8.0, and 2 × 16 μm plus three primary-transit events at 8.0 μm. The eclipse depths from jointly fit models at each wavelength are 0.040% ± 0.003% at 3.6 μm, 0.034% ± 0.006% at 4.5 μm, 0.044% ± 0.010% at 5.8 μm, 0.052% ± 0.006% at 8.0 μm, and 0.085% ± 0.032% at 16 μm. Multiple observations at the longer wavelengths improved eclipse-depth signal-to-noise ratios by up to a factor of two and improved estimates of the planet-to-star radius ratio (Rp/R⋆ = 0.0518 ± 0.0006). We also identify no significant deviations from a circular orbit and, using this model, report an improved period of 2.8758916 ± 0.0000014 days. Chemical-equilibrium models find no indication of a temperature inversion in the dayside atmosphere of HD 149026b. Our best-fit model favors large amounts of CO and CO2, moderate heat redistribution (f = 0.5), and a strongly enhanced metallicity. These analyses use BiLinearly-Interpolated Subpixel Sensitivity (BLISS) mapping, a new technique to model two position-dependent systematics (intrapixel variability and pixelation) by mapping the pixel surface at high resolution. BLISS mapping outperforms previous methods in both speed and goodness of fit. We also present an orthogonalization technique for linearly correlated parameters that accelerates the convergence of Markov chains that employ the Metropolis random walk sampler. The electronic supplement contains light-curve files.
Spinor classification of the Weyl tensor in five dimensions

We investigate the spinor classification of the Weyl tensor in five dimensions due to De Smet. We show that a previously overlooked reality condition reduces the number of possible types in the classification. We classify all vacuum solutions belonging to the most special algebraic type. The connection between this spinor and the tensor classification due to Coley, Milson, Pravda and Pravdová is investigated and the relation between most of the types in each of the classifications is given. We show that the black ring is algebraically general in the spinor classification.
Schwarzschild and Kerr Solutions of Einstein's Field Equation -- an introduction

Starting from Newton's gravitational theory, we give a general introduction into the spherically symmetric solution of Einstein's vacuum field equation, the Schwarzschild(–Droste) solution, and into one specific stationary axially symmetric solution, the Kerr solution. The Schwarzschild solution is unique and its metric can be interpreted as the exterior gravitational field of a spherically symmetric mass. The Kerr solution is only unique if the multipole moments of its mass and its angular momentum take on prescribed values. Its metric can be interpreted as the exterior gravitational field of a suitably rotating mass distribution. Both solutions describe objects exhibiting an event horizon, a frontier of no return. The corresponding notion of a black hole is explained to some extent. Eventually, we present some generalizations of the Kerr solution.
Response of a galactic disc to vertical perturbations: strong dependence on density distribution

We study the self-consistent, linear response of a galactic disc to non-axisymmetric perturbations in the vertical direction as due to a tidal encounter, and show that the density distribution near the disc mid-plane has a strong impact on the radius beyond which distortions like warps develop. The self-gravity of the disc resists distortion in the inner parts. Applying this approach to a galactic disc with an exponential vertical profile, Saha & Jog showed that warps develop beyond 4-6 disc scalelengths, which could hence be only seen in HI. The real galactic discs, however, have less steep vertical density distributions that lie between a sech and an exponential profile. Here we calculate the disc response for such a general sec h2/n density distribution, and show that the warps develop from a smaller radius of 2-4 disc scalelengths. This naturally explains why most galaxies show stellar warps that start within the optical radius. Thus, a qualitatively different picture of ubiquitous optical warps emerges for the observed less steep density profiles. The surprisingly strong dependence on the density profile is due to the fact that the disc self-gravity depends crucially on its mass distribution close to the mid-plane. General results for the radius of onset of warps, obtained as a function of the disc scalelength and the vertical scaleheight, are presented as contour plots which can be applied to any galaxy.
THE BRIGHT END OF THE ULTRAVIOLET LUMINOSITY FUNCTION AT z ∼ 8: NEW CONSTRAINTS FROM CANDELS DATA IN GOODS-SOUTH

We present new z ∼ 8 galaxy candidates from a search over ∼95 arcmin2 of WFC3/IR data, tripling the previous search area for bright z ∼ 8 galaxies. Our analysis uses newly acquired WFC3/IR imaging data from the CANDELS Multi-Cycle Treasury program over the GOODS-South field. These new data are combined with existing deep optical Advanced Camera for Surveys (ACS) imaging to search for relatively bright (MUV < −19.5 mag) z ∼ 8 galaxy candidates using the Lyman break technique. These new candidates are used to determine the bright end of the UV luminosity function (LF) of star-forming galaxies at z ∼ 7.2–8.7, i.e., a cosmic age of 600 ± 80 Myr. To minimize contamination from lower redshift galaxies, we make full use of all optical ACS data and impose strict non-detection criteria based on an optical χ2opt flux measurement. In the whole search area, we identify 16 candidate z ∼ 8 galaxies, spanning a magnitude range H160, AB = 25.7–27.9 mag. The new data show that the UV LF is a factor ∼1.7 lower at MUV < −19.5 mag than determined from the HUDF09 and Early Release Science (ERS) data alone. Combining this new sample with the previous candidates from the HUDF09 and ERS data allows us to perform the most accurate measurement of the z ∼ 8 UV LF yet. Schechter function fits to the combined data result in a best-fit characteristic magnitude of M*(z = 8) = −20.04 ± 0.46 mag. The faint-end slope is very steep, though quite uncertain, with α = −2.06 ± 0.32. A combination of wide-area data with additional ultra-deep imaging will be required to significantly reduce the uncertainties on these parameters in the future.
Sound waves and resonances in electron-hole plasma

Inspired by the recent experimental signatures of relativistic hydrodynamics in graphene, we investigate theoretically the behavior of hydrodynamic sound modes in such quasi-relativistic fluids near charge neutrality, within linear response. Locally driving an electron fluid at a resonant frequency to such a sound mode can lead to large increases in the electrical response at the edges of the sample, a signature which cannot be explained using diffusive models of transport. We discuss the robustness of this signal to various effects, including electron-acoustic phonon coupling, disorder, and long-range Coulomb interactions. These long range interactions convert the sound mode into a collective plasmonic mode at low frequencies unless the fluid is charge neutral. At the smallest frequencies, the response in a disordered fluid is quantitatively what is predicted by a "momentum relaxation time" approximation. However, this approximation fails at higher frequencies (which can be parametrically small), where the classical localization of sound waves cannot be neglected. Experimental observation of such resonances is a clear signature of relativistic hydrodynamics, and provides an upper bound on the viscosity of the electron-hole plasma.
MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE

Different theoretical methodologies lead to order-of-magnitude variations in predicted galaxy–galaxy merger rates. We examine how this arises and quantify the dominant uncertainties. Modeling of dark matter and galaxy inspiral/merger times contribute factor of ∼2 uncertainties. Different estimates of the halo–halo merger rate, the subhalo “destruction” rate, and the halo merger rate with some dynamical friction time delay for galaxy–galaxy mergers, agree to within this factor of ∼2, provided proper care is taken to define mergers consistently. There are some caveats: if halo/subhalo masses are not appropriately defined the major-merger rate can be dramatically suppressed, and in models with “orphan” galaxies and under-resolved subhalos the merger timescale can be severely over-estimated. The dominant differences in galaxy–galaxy merger rates between models owe to the treatment of the baryonic physics. Cosmological hydrodynamic simulations without strong feedback and some older semi-analytic models (SAMs), with known discrepancies in mass functions, can be biased by large factors (∼5) in predicted merger rates. However, provided that models yield a reasonable match to the total galaxy mass function, the differences in properties of central galaxies are sufficiently small to alone contribute small (factor of ∼1.5) additional systematics to merger rate predictions. But variations in the baryonic physics of satellite galaxies in models can also have a dramatic effect on merger rates. The well-known problem of satellite “over-quenching” in most current SAMs—whereby SAM satellite populations are too efficiently stripped of their gas—could lead to order-of-magnitude under-estimates of merger rates for low-mass, gas-rich galaxies. Models in which the masses of satellites are fixed by observations (or SAMs adjusted to resolve this “over-quenching”) tend to predict higher merger rates, but with factor of ∼2 uncertainties stemming from the uncertainty in those observations. The choice of mass used to define “major” and “minor” mergers also matters: stellar–stellar major mergers can be more or less abundant than halo–halo major mergers by an order of magnitude. At low masses, most true major mergers (mass ratio defined in terms of their baryonic or dynamical mass) will appear to be minor mergers in their stellar mass ratio—observations and models using just stellar criteria could underestimate major-merger rates by factors of ∼3–5. We discuss the uncertainties in relating any merger rate to spheroid formation (in observations or theory): in order to achieve better than factor of ∼3 accuracy, it is necessary to account for the distribution of merger orbital parameters, gas fractions, and the full efficiency of merger-induced effects as a function of mass ratio.
GM-RF: An AV1 Intra-Frame Fast Decision Based on Random Forest

This paper presents the Grouping of Modes based on Random Forest (GM-RF), a fast decision algorithm for the AOMedia Video 1 (AV1) intra-frame prediction applying machine learning (ML). AV1 implements a wide variety of intra-frame prediction tools, significantly increasing the required computational effort. The GM-RF uses trained Random Forest (RF) models to reduce the number of intra-frame prediction modes evaluated for each encoded block. Experimental results show that the GM-RF achieves an average time savings of 50.19%, with a BD-BR of 7.41%. Compared with related works, GM-RF reached time savings from 5.6 to 10 times higher at a cost of a higher BDBR. To the best of the authors’ knowledge, this is the first solution in the literature using ML to reduce the AV1 intra-frame prediction computational effort.
Substellar Companions to Evolved Intermediate-Mass Stars: HD 145457 and HD 180314

We report on the detection of two substellar companions orbiting around evolved intermediate-mass stars by precise Doppler measurements at Subaru Telescope and Okayama Astrophysical Observatory. HD 145457 is a K0 giant with a mass of 1.9 Mˇ, and has a planet of minimum mass, m2 sin i = 2.9 MJ, orbiting with a period of P = 176 d and eccentricity of e = 0:11. HD 180314 is also a K0 giant with 2. 6Mˇ, and hosts a substellar companion of m2 sin i = 22 MJ, which falls in the brown-dwarf mass regime, in an orbit with P = 396 d and e = 0.26. HD 145457 b is one of the innermost planets and HD 180314 b is the seventh candidate of a brown-dwarf-mass companion found around evolved intermediate-mass stars.
THE XMM-NEWTON SPECTRUM OF A CANDIDATE RECOILING SUPERMASSIVE BLACK HOLE: AN ELUSIVE INVERTED P-CYGNI PROFILE

We present a detailed spectral analysis of new XMM-Newton data of the source CXOC J100043.1+020637, also known as CID-42, detected in the COSMOS survey at z = 0.359. Previous works suggested that CID-42 is a candidate recoiling supermassive black hole (SMBH) showing also an inverted P-Cygni profile in the X-ray spectra at ∼6 keV (rest) with an iron emission line plus a redshifted absorption line (detected at 3σ in previous XMM-Newton and Chandra observations). Detailed analysis of the absorption line suggested the presence of ionized material flowing into the black hole at high velocity. In the new long XMM-Newton observation, while the overall spectral shape remains constant, the continuum 2–10 keV flux decrease of ∼20% with respect to previous observation and the absorption line is undetected. The upper limit on the intensity of the absorption line is EW < 162 eV. Extensive Monte Carlo simulations show that the nondetection of the line is solely due to variation in the properties of the inflowing material, in agreement with the transient nature of these features, and that the intensity of the line is lower than the previously measured with a probability of 98.8%. In the scenario of CID-42 as a recoiling SMBH, the absorption line can be interpreted as being due to an inflow of gas with variable density that is located in the proximity of the SMBH and recoiling with it. New monitoring observations will be requested to further characterize this line.
Nebular-line emission during the Epoch of Reionization

Nebular emission lines associated with galactic H ii regions carry information about both physical properties of the ionized gas and the source of ionizing photons as well as providing the opportunity of measuring accurate redshifts and thus distances once a cosmological model is assumed. While nebular-line emission has been extensively studied at lower redshift there are currently only few constraints within the epoch of reionization (EoR; z > 6), chiefly due to the lack of sensitive near-IR spectrographs. However, this will soon change with the arrival of the Webb Telescope providing sensitive near-IR spectroscopy covering the rest-frame UV and optical emission of galaxies in the EoR. In anticipation of Webb, we combine the large cosmological hydrodynamical simulation BlueTides with photoionization modelling to predict the nebular emission-line properties of galaxies at z = 8 → 13. We find good agreement with the, albeit limited, existing direct and indirect observational constraints on equivalent widths though poorer agreement with luminosity function constraints.
Butterflies with rotation and charge

We explore the butterfly effect for black holes with rotation or charge. We perturb rotating BTZ and charged black holes in 2 + 1 dimensions by adding a small perturbation on one asymptotic region, described by a shock wave in the spacetime, and explore the effect of this shock wave on the length of geodesics through the wormhole and hence on correlation functions. We find the effect of the perturbation grows exponentially at a rate controlled by the temperature; dependence on the angular momentum or charge does not appear explicitly. We comment on issues affecting the extension to higher-dimensional charged black holes.
Supersymmetric AdS Black Rings

It has been proven in arXiv:1303.0853 that all regular supersymmetric near-horizon geometries in minimal five-dimensional gauged supergravity admit automatic supersymmetry enhancement. Using this result, the integrability conditions associated with the existence of the additional supersymmetry are analysed, and the near-horizon geometries are determined explicitly. We show that they all correspond to previously constructed examples. Hence, there are no supersymmetric black ring solutions in minimal five-dimensional gauged supergravity.
Bose-Einstein condensation and Berezinskii-Kosterlitz-Thouless transition in the two-dimensional nonlinear Schrödinger model

We analyze the Bose-Einstein condensation process and the Berezinskii-Kosterlitz-Thouless phase transition within the nonlinear Schrodinger model and their interplay with wave turbulence theory. By using numerical experiments we study how the condensate fraction and the first-order correlation function behave with respect to the mass, the energy, and the size of the system. By relating the free-particle energy to the temperature, we are able to estimate the Berezinskii-Kosterlitz-Thouless transition temperature. Below this transition we observe that for a fixed temperature the superfluid fraction appears to be size independent, leading to a power-law dependence of the condensate fraction with respect to the system size.
Failure of hydrogenation in protecting polycyclic aromatic hydrocarbons from fragmentation

A recent study of soft x-ray absorption in native and hydrogenated coronene cations, C_24H_12+m^+ m=0–7, led to the conclusion that additional hydrogen atoms protect (interstellar) polycyclic aromatic hydrocarbon (PAH) molecules from fragmentation [Reitsma et al., Phys. Rev. Lett. 113, 053002 (2014)]. The present experiment with collisions between fast (30–200 eV) He atoms and pyrene (C_16H_10+m^+, m=0, 6, and 16) and simulations without reference to the excitation method suggests the opposite. We find that the absolute carbon-backbone fragmentation cross section does not decrease but increases with the degree of hydrogenation for pyrene molecules.