Miracle-dz/UniFAR-FTUs huggingface dataset:
Adequacy of Healthcare by Insurance Type in Traumatic Brain Injury Patients

Traumatic brain injury (TBI) is a significant contributor to disability, especially among patients younger than 18 years old in the United States. While insurance is often needed to receive services, studies investigating whether TBI treatment adequacy is dependent on the insurance type are scant. Our objective was to determine whether private insurance in paediatric TBI patients is associated with a higher perceived adequacy of healthcare compared with non-private insurance. This was a cross-sectional study utilising secondary data collected from the National Survey of Children Health 2011/12. The main exposure of interest was the insurance status of children at the time of a TBI (private vs non-private). The study outcome was the perceived adequacy of healthcare, defined as having coverage needs that were usually or always met by insurance. Unadjusted and adjusted logistic regression analysis were used. After adjustments for the covariates, the odds of adequate healthcare among those with non-private insurance compared with those with private were not statistically significant (OR 1.49; 95% CI 0.87–2.55). This study implicates paediatric TBI patients do not believe they receive adequate healthcare independent of insurance status. Clinicians, policy makers, and researchers need to better evaluate and address this issue.
A note on field redefinitions and higher-spin equations

In this note we provide some details on the quasi-local field redefinitions which map interactions extracted from Vasiliev’s equations to those obtained via holographic reconstruction. Without loss of generality, we focus on the source to the Fronsdal equations induced by current interactions quadratic in the higher-spin linearised curvatures.
Replica solution of the random energy model

The alternative replica technique which involves summation over all integer momenta of the partition function and which does not require analytic continuation to non-integer values of the replica parameter n is discussed. In terms of this technique (which does not involve any replica symmetry breaking “magic operations”), a well-known solution for the average free energy of the random energy model is recovered in a very simple way.
THE IMPACT OF INTERACTIONS, BARS, BULGES, AND ACTIVE GALACTIC NUCLEI ON STAR FORMATION EFFICIENCY IN LOCAL MASSIVE GALAXIES

Using atomic and molecular gas observations from the GASS and COLD GASS surveys and complementary optical/UV data from the Sloan Digital Sky Survey and the Galaxy Evolution Explorer, we investigate the nature of the variations in the molecular gas depletion time observed across the local massive galaxy population. The large and unbiased COLD GASS sample allows us for the first time to statistically assess the relative importance of galaxy interactions, bar instabilities, morphologies, and the presence of active galactic nuclei (AGNs) in regulating star formation efficiency. We find that both the H2 mass fraction and depletion time vary as a function of the distance of a galaxy from the main sequence traced by star-forming galaxies in the SFR–M* plane. The longest gas depletion times are found in below-main-sequence bulge-dominated galaxies (μ* >5 × 108 M☉ kpc−2, C > 2.6) that are either gas-poor (/M* <1.5%) or else on average less efficient by a factor of ∼2 than disk-dominated galaxies at converting into stars any cold gas they may have. We find no link between the presence of AGNs and these long depletion times. In the regime where galaxies are disk-dominated and gas-rich, the galaxies undergoing mergers or showing signs of morphological disruptions have the shortest molecular gas depletion times, while those hosting strong stellar bars have only marginally higher global star formation efficiencies as compared to matched control samples. Our interpretation is that the molecular gas depletion time variations are caused by changes in the ratio between the gas mass traced by the CO(1–0) observations and the gas mass in high-density star-forming cores (as traced by observations of, e.g., HCN(1–0)). While interactions, mergers, and bar instabilities can locally increase pressure and raise the ratio of efficiently star-forming gas to CO-detected gas (therefore lowering the CO-based depletion time), massive bulges may prevent the formation of dense clumps by stabilizing gas disks against fragmentation, therefore producing the long depletion times. Building a sample representative of the local galaxy population with M* >1010 M☉, we derive a global Kennicutt–Schmidt star formation relation of slope 1.18 ± 0.24 and observe structure within the scatter around this relation, with galaxies having low (high) stellar mass surface densities lying systematically above (below) the mean relation, suggesting that is not the only parameter driving the global star formation ability of a galaxy.
The proof of non-homogeneous T1 theorem via averaging of dyadic shifts

We give again a proof of non-homogeneous T1 theorem. Our proof consists of three main parts: a construction of a random dyadic lattice; an estimate of matrix coefficients of a Calder\'on--Zygmund operator with respect to random Haar basis if a smaller Haar support is good; a clever averaging trick from Hyt\"onen's papers which uses the averaging over dyadic lattices to decompose operator into dyadic shifts eliminating the error term that was present in the previous proofs by Nazarov--Treil--Volberg.
DISCOVERY OF A LOW-LUMINOSITY, TIGHT SUBSTELLAR BINARY AT THE T/Y TRANSITION

We have discovered that the brown dwarf WISE J014656.66+423410.0 is a close binary (0.″ 0875 ± 0.″ 0021, 0.93 − 0.16 + 0.12 ? > AU) from Keck laser guide star adaptive optics imaging. Our photometry for this system reveals that both components are less luminous than those in any known substellar binary. Combining a new integrated-light spectrum (T9p) and resolved YJH-band photometry from Keck allows us to perform spectral decomposition and assign component types of T9 and Y0. Many of the unusual features in the spectrum might be explained by high surface gravity: Y-band peak broadened to the blue; J-band peak broadened to the red; H-band peak shifted slightly to the red; and red Y − J colors. Interestingly, the very low component luminosities imply that the T9 primary is unexpectedly cold (Teff = 345 ± 45 K assuming an age of 10 Gyr), making it ≈100 K cooler than any other late-T dwarf and comparable to Y dwarfs. One intriguing explanation for this apparent discrepancy is that the J- and H-band spectral features that trigger the transition from T to Y spectral types are highly gravity dependent. This can be tested directly in the very near future by orbit monitoring. We constrain the orbital period to be ≲10 yr by combining evolutionary-model-based mass estimates for the components (≈12–21 MJup, 1σ at 10 Gyr) with a statistical constraint on the semimajor axis (≲1.3 AU). Such a period is shorter than any other known T/Y transition binary, meaning that WISE J0146+4234AB will likely yield a dynamical mass within the next few years.
Probing galaxy dark matter haloes in COSMOS with weak lensing flexion

Current theories of structure formation predict specific de nsity profiles of galaxy dark matter haloes, and with weak gravitational lensing we can probe these profiles on several scales. On small scales, higher-order shape distortions known as flexi on add significant detail to the weak lensing measurements. We present here the first detection of a galaxy-galaxy flexion signal in space-based data, obtained using a new Shapelets pipeline introduced here. We combine this higher-order lensing signal with shear to constrain the ave rage density profile of the galaxy lenses in the Hubble Space Telescope COSMOS survey. We also show that light from nearby bright objects can significantly affect flexion measurement s. After correcting for the influence of lens light, we show that the inclusion of flexion provides t ighter constraints on density profiles than does shear alone. Finally we find an average dens ity profile consistent with an isothermal sphere.
Estimates of cluster masses in screened modified gravity

We use cosmological hydrodynamical simulations to study the effect of screened modified gravity models on the mass estimates of galaxy clusters. In particular, we focus on two novel aspects: (i) we study modified gravity models in which baryons and dark matter are coupled with different strengths to the scalar field, and; (ii) we put the simulation results into the greater context of a general screened-modified gravity parametrization. We have compared the mass of clusters inferred via lensing versus the mass inferred via kinematical measurements as a probe of violations of the equivalence principle at Mpc scales. We find that estimates of cluster masses via X-ray observations is mainly sensitive to the coupling between the scalar degree of freedom and baryons – while the kinematical mass is mainly sensitive to the coupling to dark matter. Therefore, the relation between the two mass estimates is a probe of a possible non-universal coupling between the scalar field, the standard model fields, and dark matter. Finally, we used observational data of kinetic, thermal and lensing masses to place constraints on deviations from general relativity on cluster scales for a general parametrization of screened modified gravity theories which contains f ( R ) and Symmetron models. We find that while the kinematic mass can be used to place competitive constraints, using thermal measurements is challenging as a potential non-thermal contribution is degenerate with the imprint of modified gravity.
SELF-CONSISTENT EVOLUTION OF GAS AND COSMIC RAYS IN CYGNUS A AND SIMILAR FR II CLASSICAL DOUBLE RADIO SOURCES

In Cygnus A and other classical FR II double radio sources, powerful opposing jets from the cores of halo-centered galaxies drive out into the surrounding cluster gas, forming hotspots of shocked and compressed cluster gas at the jet extremities. The moving hotspots are sandwiched between two shocks. An inner-facing shock receives momentum and cosmic rays from the jet and creates additional cosmic rays that form a radio lobe elongated along the jet axis. An outer-facing bow shock moves directly into the undisturbed group or cluster gas, creating a cocoon of shocked gas enclosing the radio lobe. We describe computations that follow the self-consistent dynamical evolution of the shocked cluster gas and the relativistic synchrotron-emitting gas inside the lobes. Relativistic and non-relativistic components exchange momentum by interacting with small magnetic fields having dynamically negligible energy densities. The evolution of Cygnus A is governed almost entirely by cosmic ray energy flowing from the hotspots. Mass flowing into hotspots from the jets is assumed to be small, greatly reducing the mass of gas flowing back along the jet, common in previous calculations, that would disrupt the spatial segregation of synchrotron-loss ages observed inside FR II radio lobes. We compute the evolution of the cocoon when the velocity and cosmic ray luminosity of the hotspots are constant and when they vary with time. If cosmic rays mix with cluster gas in hotspots before flowing into the radio lobe, the thermal gas is heated to mildly relativistic temperatures, producing an unobserved pressure inside the lobe.
Retrieval of Physical Parameters With Deep Structured Kernel Regression

Retrieval of physical parameters is of paramount relevance for Earth monitoring. Statistical (machine) learning approaches have been successfully introduced in the community, because they can learn nonlinear functional relations from observational data with no strong a priori assumptions and parametric forms. However, these methods still have two relevant problems: they only consider only one nonlinear feature map of the data, which can be limiting in complex problems where inputs (e.g., radiances) and outputs (e.g., state vectors) have strong nonlinear relations, and in most of the cases, models do not incorporate the structure of the output (dependent) variables. This article proposes a kernel method that solves the two aforementioned problems for physical parameter retrieval: first, it performs multioutput regression with the desired number of connected mappings, and second, it incorporates the output variables structure via a dedicated kernel. The proposed method has a closed-form solution, and thus, neither kernel dimensionality reduction nor preimaging is necessary unlike in previous structured kernel methods. Through the definition of appropriate kernel feature mappings, we also derive a pragmatic deep structured kernel ridge regression (KRR). The method is characterized statistically using a Gaussian process (GP) treatment and providing guarantees based on the concepts of leverage scores (LSs) and effective dimension: both explain that including an output structure acts as a powerful regularizer. We illustrate the method’s performance in toy examples and remote sensing parameter estimation problems involving vegetation parameters [chlorophyll, leaf area index (LAI), and fractional vegetation cover (FVC)] from compact high-resolution imaging spectrometer (CHRIS) images and the atmospheric temperature, moisture, and ozone profiles from infrared atmospheric sounding interferometer (IASI) data.
Possibility Theorems for Aggregating Infinite Utility Streams Equitably

The standard route for aggregating infinite utility streams using a real-valued representation runs into well-known difficulties as soon as we insist on the axiom of inter-generational equity. The aim of this paper is to explore what is feasible without abandoning this axiom. The paper focusses its attention on the Pareto axiom and domain restrictions. It turns out that once we weaken these requirements, realvalued aggregation becomes possible in a variety of ways (though, of course, impossibility results lurk everywhere). By establishing a series of results, this paper tries to chalk out the frontier between what is possible and what is not.
THE WOLF-RAYET CONTENT OF M33

Wolf-Rayet (WR) stars are evolved massive stars, and the relative number of WC-type and WN-type WRs should vary with metallicity, providing a sensitive test of stellar evolutionary theory. The observed WC/WN ratio is much higher than that predicted by theory in some galaxies but this could be due to observational incompleteness for WN types, which have weaker lines. Previous studies of M33's WR content show a galactocentric gradient in the relative numbers of WCs and WNs, but only small regions have been surveyed with sufficient sensitivity to detect all of the WNs. Here, we present a sensitive survey for WRs covering all of M33, finding 55 new WRs, mostly of WN type. Our spectroscopy also improves the spectral types of many previously known WRs, establishing in one case that the star is actually a background quasar. The total number of spectroscopically confirmed WRs in M33 is 206, a number we argue is complete to ∼5%, with most WRs residing in OB associations, although ∼2% are truly isolated. The WC/WN ratio in the central regions (<2 kpc) of M33 is much higher than that predicted by the current Geneva evolutionary models, while the WC/WN ratios in the outer regions are in good accord, as are the values in the Small Magellanic Cloud and Large Magellanic Cloud. The WC/WN ratio and the WC subtype distribution both argue that the oxygen abundance gradient in M33 is significantly larger than that found by some recent studies, but are consistent with the two-component model proposed by Magrini et al.
SPECTRUM OF RELATIVISTIC AND SUBRELATIVISTIC COSMIC RAYS IN THE 100 pc CENTRAL REGION

From the rate of hydrogen ionization and the gamma-ray flux, we derived the spectrum of relativistic and subrelativistic cosmic rays (CRs) nearby and inside the molecular cloud Sgr B2 near the Galactic Center. We studied two cases of CR propagation in molecular clouds: free propagation and scattering of particles by magnetic fluctuations excited by the neutral gas turbulence. We showed that in the latter case CR propagation inside the cloud can be described as diffusion with a coefficient of ∼ 3 × 10 27 ? > cm2 s−1. For the case of hydrogen ionization by subrelativistic protons, we showed that their spectrum outside the cloud is quite hard with a spectral index of δ > − 1 ? > . The energy density of subrelativistic protons ( > 50 ? > eV cm−3) is one order of magnitude higher than that of relativistic CRs. These protons generate the 6.4 keV emission from Sgr B2, which was about 30% of the flux observed by Suzaku in 2013. Future observations for the period after 2013 may discover the background flux generated by subrelativistic CRs in Sgr B2. Alternatively, hydrogen ionization of the molecular gas in Sgr B2 may be caused by high energy electrons. We showed that the spectrum of electron bremsstrahlung is harder than the observed continuum from Sgr B2, and in principle, this X-ray component provided by electrons could be seen from the INTEGRAL data as a stationary high energy excess above the observed spectrum E x − 2 ? > .
A Fundamental Line of Black Hole Activity

Black hole systems with outflows are characterized by intrinsic physical quantities such as the outflow beam power, Lj, the bolometric accretion disk luminosity, Lbol, and black hole mass or Eddington luminosity, LEdd. When these systems produce compact radio emission and X-ray emission, they can be placed on the fundamental plane (FP), an empirical relationship between compact radio luminosity, X-ray luminosity, and black hole mass. We consider a fundamental line (FL) of black hole activity written in terms of dimensionless intrinsic physical quantities: log(Lj/LEdd) = A log(Lbol/LEdd) + B or equivalently log(Lj/Lbol) = (A − 1) log(Lbol/LEdd) + B, and show that the FP may be written in the form of the FL. The FL has a smaller dispersion than the FP, suggesting the FP derives from the FL. Disk-dominated and jet-dominated systems have consistent best-fit FL parameters that suggest they are governed by the same physics. There are sharp cutoffs at Lbol/LEdd ≃ 1 and Lj/LEdd ≃ 0.2, and no indication of a strong break as . Consistent values of A are obtained for numerous samples, including FRII sources, LINERS, AGNs with compact radio emission, and Galactic black holes, which indicate a weighted mean value of A ≃ 0.45 ± 0.01. The results suggest that a common physical mechanism related to the dimensionless bolometric luminosity of the disk controls the jet power relative to the disk power. The beam power Lj can be obtained by combining FP best-fit parameters and compact radio luminosity for sources that fall on the FP.
Fault Tolerable Cooperative Control for Charging Supercapacitors of Catenary-Free Trams

Supercapacitor-powered devices are now being used as main supply units in catenary-free trams, for their rapid charging and environmental-friendly performance. Faced with the high-power-charging load from trams, the cooperative control protocol is widely adopted to charge onboard supercapacitors due to the properties of reducing current overshoot and imbalance. However, the charging system under the protocol inevitably suffers from potential fault data from physical malfunctions or cyberattacks. To deal with it, in this article, a reliable cooperative control strategy (RCCS) is designed to alleviate the effects of fault data regardless of where it comes from and protect the system's performance. Specifically, first, we introduce the cooperative charging system model and analyze the causes and effects of fault data. Then, we provide a total current control protocol (TCCP) and a data cooperative-screening control protocol (CSCP) to deal with fault data from the physical layer and cyberlayer, respectively. Combining TCCP and CSCP, RCCS is designed and the system stability is proved based on Lyapunov stability analysis under RCCS. Finally, both simulations and experiments are conducted to demonstrate the effectiveness of the proposed algorithms.
Association of the inflammatory balance of diet and lifestyle with colorectal cancer among Korean adults: a case-control study

OBJECTIVES Dietary and lifestyle exposures may affect the risk of colorectal cancer (CRC) by promoting chronic inflammation. Therefore, we assessed the separate and joint associations of dietary and lifestyle inflammation scores (DIS and LIS, respectively) with CRC. METHODS Data from 919 pathologically confirmed CRC cases and 1,846 age- and sex-matched controls recruited at the National Cancer Center Korea were analyzed. We calculated the DIS and LIS, which characterize the collective contributions of 19 dietary and 4 lifestyle factors, respectively, to systemic inflammation by applying weights based on high-sensitivity C-reactive protein. A higher score represented a higher balance of pro- to anti-inflammatory exposures. Unconditional logistic regression models were used to estimate odds ratios (ORs) and 95% confidence intervals (CIs) for CRC risk compared across the DIS and LIS tertile categories, with the lowest tertile as the reference group. RESULTS The highest DIS tertile had significantly increased odds of having CRC (OR, 2.65; 95% CI, 2.10 to 3.36), and the odds increased with increasing DIS. The highest LIS tertile group had 1.28-fold higher odds of having CRC (95% CI, 1.03 to 1.58). In the cross-classification analysis, the odds of having CRC increased as the DIS and LIS jointly increased until the DIS reached the highest tertile, where the risk was very high (3-fold or more) regardless of the LIS. CONCLUSIONS In conclusion, a higher balance of pro-inflammatory relative to anti-inflammatory dietary and lifestyle factors, especially dietary factors, was associated with higher CRC risk among Korean adults.
Quantum oscillations without magnetic field

Quantum oscillations are the fundamental measurement made when studying metals and semimetals. They provide information about the Fermi surface by measuring interference of particles drifting around it in a magnetic field. So far it was only possible to measure them by applying an external magnetic field. Here, the authors argue that the deformation of the Dirac/Weyl semimetal can produce a strong enough pseudo-magnetic field to measure quantum oscillations in the strength of the strain. They argue that the effect of the strain is identical to the effect of the real magnetic field at energies close to the Dirac/Weyl points. They propose a setup in which the strain can be tuned continuously, and in which the quantum oscillations can be first observed in the complete absence of a magnetic field.
Jordan algebraic approach to symmetric optimization

In this thesis we present a generalization of interior-point methods for linear optimization based on kernel functions to symmetric optimization. It covers the three standard cases of conic optimization: linear optimization, second-order cone optimization and semi-definite optimization. We give an introduction to Euclidean Jordan algebras and explain the connection between such algebras and symmetric cones. We establish some properties of eigenvalues in Jordan algebras and prove that the barrier functions based on kernel functions are separable spectral functions that only depend on the eigenvalues of their arguments. We propose an interior-point algorithm for symmetric optimization and derive its complexity bound.