Miracle-dz/UniFAR-FTUs huggingface dataset:
Measurements of Physical Parameters of White Dwarfs: A Test of the Mass–Radius Relation

We present a detailed spectroscopic and photometric analysis of 219 DA and DB white dwarfs for which trigonometric parallax measurements are available. Our aim is to compare the physical parameters derived from the spectroscopic and photometric techniques, and then to test the theoretical mass–radius relation for white dwarfs using these results. The agreement between spectroscopic and photometric parameters is found to be excellent, especially for effective temperatures, showing that our model atmospheres and fitting procedures provide an accurate, internally consistent analysis. The values of surface gravity and solid angle obtained, respectively, from spectroscopy and photometry, are combined with parallax measurements in various ways to study the validity of the mass–radius relation from an empirical point of view. After a thorough examination of our results, we find that 73% and 92% of the white dwarfs are consistent within 1σ and 2σ confidence levels, respectively, with the predictions of the mass–radius relation, thus providing strong support to the theory of stellar degeneracy. Our analysis also allows us to identify 15 stars that are better interpreted in terms of unresolved double degenerate binaries. Atmospheric parameters for both components in these binary systems are obtained using a novel approach. We further identify a few white dwarfs that are possibly composed of an iron core rather than a carbon/oxygen core, since they are consistent with Fe-core evolutionary models.
Variable emission mechanism of a Type IV radio burst

Context. The Sun is an active star and the source of the largest explosions in the solar system, such as flares and coronal mass ejections (CMEs). Flares and CMEs are powerful particle accelerators that can generate radio emission through various emission mechanisms. Aims. CMEs are often accompanied by Type IV radio bursts that are observed as continuum emission in dynamic spectra at decimetric and metric wavelengths, but their emission mechanism can vary from event to event. Here, we aim to determine the emission mechanism of a complex Type IV burst that accompanied the flare and CME on 22 September 2011. Methods. We used radio imaging from the Nançay Radioheliograph, spectroscopic data from the e-Callisto network, ARTEMIS, Ondrejov, and Phoenix3 spectrometers combined with extreme-ultraviolet observations from NASA’s Solar Dynamic Observatory to analyse the Type IV radio burst and determine its emission mechanism. Results. We show that the emission mechanism of the Type IV radio burst changes over time. We identified two components in the Type IV radio burst: an earlier stationary Type IV showing gyro-synchrotron behaviour, and a later moving Type IV burst covering the same frequency band. This second component has a coherent emission mechanism. Fundamental plasma emission and the electron-cyclotron maser emission are further investigated as possible emission mechanisms for the generation of the moving Type IV burst. Conclusions. Type IV bursts are therefore complex radio bursts, where multiple emission mechanisms can contribute to the generation of the wide-band continuum observed in dynamic spectra. Imaging spectroscopy over a wide frequency band is necessary to determine the emission mechanisms of Type IV bursts that are observed in dynamic spectra.
Curvature-radiation--pair-production model for. gamma. -ray pulsars

Assuming that pulsar . gamma. -rays are produced via curvature radiation of primary electrons near the neutron star and that they are attenuated only through the pair production process in strong electric and magnetic fields, we use a detailed model of the magnetosphere to calculate the resulting optical depths and pulse shapes. We consider both the effect of E.B=0 and E.Bnot =0 on the attenuation of the photons, and the effect of photon energy, rotation rate, and obliquity on the pulse shapes. It is found that pulsar rotation tends to increase pair production, causing large optical depths for the shortest period pulsars. The calculations also predict high-energy cutoffs and spectra for the observable . gamma. -ray emission.
AGB candidates in the field of gamma Cas

We report the spectroscopic and photometric monitoring of a sample of 530 candidate AGB stars in a 5 degrees field, selected from the IPHAS catalog: historic light curves were derived from Asiago IR plates taken in the years 1965 -1984. We found 10 Miras, 5 stars with long term trends, 3 semiregular and 3 irregular. Spectral types from CCD slit spectra gave 8 M-type, 7 C-type and 6 S-type stars. In the color-color plots made from IPHAS and 2MASS catalogs, the S-type and M-type stars occupy the same regions, while C-type stars are well separated. All C-type stars with IR excess showed long term trends in their light curve. Distances of the Mira stars, estimated from their periods and K magnitudes, gave a median value of 4.9 kpc with a large spread. A comparison with astrometric parallaxes from Gaia DR2 is briefly discussed.
Ensemble learning for glioma patients overall survival prediction using pre-operative MRIs

Objective: Gliomas are the most common primary brain tumors. Approximately 70% of the glioma patients diagnosed with glioblastoma have an averaged overall survival (OS) of only ∼16 months. Early survival prediction is essential for treatment decision-making in glioma patients. Here we proposed an ensemble learning approach to predict the post-operative OS of glioma patients using only pre-operative MRIs. Approach: Our dataset was from the Medical Image Computing and Computer Assisted Intervention Brain Tumor Segmentation challenge 2020, which consists of multimodal pre-operative MRI scans of 235 glioma patients with survival days recorded. The backbone of our approach was a Siamese network consisting of twinned ResNet-based feature extractors followed by a 3-layer classifier. During training, the feature extractors explored traits of intra and inter-class by minimizing contrastive loss of randomly paired 2D pre-operative MRIs, and the classifier utilized the extracted features to generate labels with cost defined by cross-entropy loss. During testing, the extracted features were also utilized to define distance between the test sample and the reference composed of training data, to generate an additional predictor via K-NN classification. The final label was the ensemble classification from both the Siamese model and the K-NN model. Main results: Our approach classifies the glioma patients into 3 OS classes: long-survivors (>15 months), mid-survivors (between 10 and 15 months) and short-survivors (<10 months). The performance is assessed by the accuracy (ACC) and the area under the curve (AUC) of 3-class classification. The final result achieved an ACC of 65.22% and AUC of 0.81. Significance: Our Siamese network based ensemble learning approach demonstrated promising ability in mining discriminative features with minimal manual processing and generalization requirement. This prediction strategy can be potentially applied to assist timely clinical decision-making.
Detections of [O iii] 88 μm in two quasars in the reionization epoch

We report on detections with the Atacama Large Millimeter/sub-millimeter Array of the far-infrared [O iii] 88 μm line and the underlying dust continuum in two quasars in the reionization epoch, J205406.48−000514.8 (hereafter J2054−0005) at z = 6.0391 ± 0.0002 and J231038.88+185519.7 (hereafter J2310+1855) at z = 6.0035 ± 0.0007. The [O iii] luminosities of J2054−0005 and J2310+1855 are L[O iii] = (6.8 ± 0.6) × 109 and $(2.4 \pm 0.6) \times 10^{9}\,$L⊙, corresponding to ∼0.05% and 0.01% of the total infrared luminosity, LTIR, respectively. Combining these [O iii] luminosities with [C ii] 158 μm luminosities in the literature, we find that J2054−0005 and J2310+1855 have [O iii]-to-[C ii] luminosity ratios of 2.1 ± 0.4 and 0.3 ± 0.1, respectively, the latter of which is the lowest among objects so far reported at z > 6. Combining [O iii] observations at z ≈ 6–9 from our study and the literature, we identify the [O iii] line deficit: objects with a larger LTIR (total infrared luminosity) have lower L[O iii]-to-LTIR ratios. Furthermore, we also find that the anti-correlation is shifted toward a higher LTIR value when compared with the local [O iii] line deficit.
Distance priors from Planck final release

We present the distance priors from the finally released Planck TT, TE, EE+lowE data in 2018. The uncertainties are around 40% smaller than those from Planck 2015 TT+lowP. In order to check the validity of these new distance priors, we adopt the distance priors to constrain the cosmological parameters in different dark energy models, including the ΛCDM model, the wCDM model and the CPL model, and conclude that the distance priors provide consistent constraints on the relevant cosmological parameters compared to those from the full Planck 2018 data release.
Distances and Kinematics of Gould Belt Star-forming Regions with Gaia DR2 Results

We present an analysis of the astrometric results from the Gaia second data release (DR2) for young stellar objects (YSOs) in star-forming regions related to the Gould Belt (GB). These regions are Barnard 59, Lupus 1 to 4, Chamaeleon I and II, ϵ Chamaeleontis, the Cepheus flare, IC 5146, and Corona Australis. The mean distance to the YSOs in each region is consistent with earlier estimations, though a significant improvement in the final errors was obtained. The mean distances to the star-forming regions were used to fit an ellipsoid of size (358 ± 7) ×(316 ± 13) × (70 ± 4) pc3, centered at (X0, Y0, Z0) = (−82 ± 15, 39 ± 7, −25 ± 4) pc, consistent with recently determined parameters of the GB. The mean proper motions were combined with radial velocities from the literature to obtain the three-dimensional motions of the star-forming regions, which are consistent with a general expansion of the GB. We estimate that this expansion is occurring at a velocity of 2.5 ± 0.1 km s−1. This is the first time that motions of YSOs have been used to investigate the kinematics of the GB. As an interesting side result, we also identified stars with large peculiar velocities.
The Long-Term Healthcare Utilization and Economic Burden of RSV Infection in Children ≤5 Years in Japan: Propensity Score Matched Cohort Study

Background The objective of this study was to estimate the long-term healthcare utilization and cost burden of RSV by chronological age of diagnosis (Year 1, Year 2 and Years 3–5 cohorts) as well as by gestational age at birth in Japan. Methods The JMDC database was used to retrospectively identify RSV and control patients between February 1, 2011 and January 31, 2016 and follow them through December 31, 2017. Infants with RSV infection (n = 9028 in Year 1; n = 4929 in Year 2; n = 2004 in Years 3–5) were matched to controls (n = 17,886; n = 9351; n = 3655, respectively) based on gestational age and year and quarter of birth; controls were assigned the index date (ie, diagnosis) of their respective match. Covariate-balancing propensity score weights were employed adjusting for remaining imbalances between cohorts. The main outcomes were average cumulative rates for all-cause, asthma/wheezing, and respiratory-related hospitalizations, physician and urgent care/emergency visits and associated costs (reported as 2018 ¥JPY) over 36-months of follow-up since index. Results Healthcare utilization was significantly higher among RSV cases for most comparisons. All-cause average differential cost burden was higher for RSV, compared to controls, among the following cohorts: Year 1 full-term (¥277,727); Year 2 preterm (¥530,302), late preterm (¥270,797), full-term (¥238,832); Years 3–5 preterm (¥110,057), late preterm (¥486,670), full-term (¥289,986). While all-cause costs were similar for preterm and late preterm children in the Year 1 cohort, respiratory- and asthma/wheezing-related attributable costs were substantially higher for RSV. Conclusion RSV infection had a significant long-term health and economic burden among children infected during their first year of life and later in life. Study findings have import for prevention strategies, currently directed at maternal immunization and monoclonal antibodies for preventing primary RSV infections in the first six months of life and beyond but also for older age not targeted currently.
Fast fault-tolerant filtering of quantum codewords

The stabilization of a quantum computer by repeated error correction can be reduced almost entirely to repeated preparation of blocks of qubits in quantum codeword states. These are multiparticle entangled states with a high degree of symmetry. The required accuracy can be achieved by measuring parity checks, using imperfect apparatus, and rejecting states which fail them. This filtering process is considered for t-error-correcting codes with t > 1. It is shown how to exploit the structure of the codeword and the check matrix, so that the filter is reduced to a minimal form where each parity check need only be measured once, not > t times by the (noisy) verification apparatus. This both raises the noise threshold and also reduces the physical size of the computer. A method based on latin rectangles is proposed, which enables the most parallel version of a logic gate network to be found, for a class of networks including those used in verification. These insights allowed the noise threshold to be increased by an order of magnitude.
WEAK SELECTION AND STABILITY OF LOCALIZED DISTRIBUTIONS IN OSTWALD RIPENING

We support and generalize a weak selection rule predicted recently for the self-similar asymptotics of the distribution function (DF) in the zero-volume-fraction limit of Ostwald ripening (OR). An asymptotic perturbation theory is developed that, when combined with an exact invariance property of the system, yields the selection rule in terms of the initial condition, predicts a power-law convergence towards the selected self-similar DF, and agrees well with our numerical simulations for the interface- and diffusion-controlled OR.
Flux Backgrounds and Exceptional Generalised Geometry

The main topic of this thesis are flux compactifications. Firstly, we study dimensional reductions of type II and eleven-dimensional supergravities using exceptional generalised geometry. We start by presenting the needed mathematical tools, focusing on G-structures and their extension to generalised geometry. Then, we move our focus on compactifications. In particular, we mainly focus on type IIA, building the version of exceptional generalised geometry adapted to such supergravity and finding the right deformations of generalised Lie derivative to accomodate the Romans mass. We describe the generalised Scherk-Schwarz method to find consistent truncation ansatze preserving the maximal amount of supersymmetry. As further point, we study generalised calibrations on AdS backgrounds in type IIB and M-theory.
Probabilistic approach to Page's formula for the entropy of a quantum subsystem

Page conjectured [Phys. Rev. Lett. 71, 1291–1294 (1993)] that if a quantum system of Hilbert space dimension mn is in a random pure state, the average entropy of a subsystem of dimension should be given by the simple and elegant formula . This formula appeared to be true and was first proved by Foong and Kanno [Phys. Rev. Lett. 72, 1148–1151 (1994)] by using Fourier transform, and next by Sánchez-Ruiz [Phys. Rev. E 52, 5653–5655 (1995)] and by Sen [Phys. Rev. Lett. 77, 1–3 (1996)] by using random matrix theory connected with generalized Laguerre polynomials. Adopting this last viewpoint, we detail the probabilistic approach to this problem. Especially, viewing any Gaussian vector as a product of a uniformly distributed unitary vector by an Erlang distribution, we give a new insight for the different entropies introduced by Page.
Access time of an adaptive random walk on the world-wide Web

We introduce and simulate the random walk that adapts move strategies according to local node preferences on a directed graph. We consider graphs with double-hierarchical connectivity and variable wiring diagram in the universality class of the world-wide Web. The ensemble of walkers reveals the structure of local subgraphs with dominant promoters and attractors of links. The average access time decays with the distance in hierarchy $\Delta q$ as a power $ \sim (\Delta q)^{-\theta}$. The access to highly connected nodes is orders of magnitude shorter compared to the standard random walk, suggesting the adaptive walk as an efficient message-passing algorithm on this class of graphs.
On the Origin of Gas-poor Galaxies in Galaxy Clusters Using Cosmological Hydrodynamic Simulations

The environmental effect is commonly used to explain the excess of gas-poor galaxies in galaxy clusters. Meanwhile, the presence of gas-poor galaxies at cluster outskirts, where galaxies have not spent enough time to feel the cluster environmental effect, hints at the presence of preprocessing. Using cosmological hydrodynamic simulations on 16 clusters, we investigate the mechanisms of gas depletion of galaxies found inside clusters. The gas-depletion mechanisms can be categorized into three channels based on where and when they took place. First, 34% of our galaxies are gas poor before entering clusters (“preprocessing”). They are mainly satellites that have undergone the environmental effect inside group halos. Second, 43% of the sample quickly became gas deficient in clusters before the first pericentric pass (“fast cluster processing”). Some of them were group satellites that are low in gas at the time of cluster entry compared to the galaxies directly coming from the field. Even the galaxies with large gas fractions take this channel if they fall into massive clusters (≳1014.5 M⊙) or approach cluster centers through radial orbits. Third, 24% of our sample retain gas even after their first pericentric pass (“slow cluster processing”) as they fall into the less massive clusters or have circular orbits. The relative importance of each channel varies with a cluster’s mass, while the exact degree of significance is subject to large uncertainties. Group preprocessing accounts for one-third of the total gas depletion, but it also determines the gas fraction of galaxies at their cluster entry, which in turn determines whether a galaxy should take the fast or slow cluster processing.
Quantification of the transmission properties of metasurfaces illuminated by finite-size beams

The aim of this letter is to {present analytical method to} quantitatively address the influence of a focusing illumination on the transmission /reflection properties of a {metasurface illuminated by a finite-size beam}. In fact, most theoretical and numerical studies are performed by considering an infinite periodic structure illuminated by a plane wave. In practice, one deals with a finite-size illumination and structure. Combination of the angular spectrum expansion with a monomodal modal method is performed to determine the beam size needed to acquire efficient properties of a Metasurface that behaves as Anisotropic Plate MAP Interesting results show that the beam-size can be as small as 5X5 periods to recover the results of a plane wave. Other results also show that the beam-size could be used as an extrinsic parameter to enhance the MAP performance and to finely adjust its expected properties (birefringence and/or transmission coefficient).
Resonant Inverse Compton Scattering Spectra from Highly Magnetized Neutron Stars

Hard, nonthermal, persistent pulsed X-ray emission extending between 10 and ∼150 keV has been observed in nearly 10 magnetars. For inner-magnetospheric models of such emission, resonant inverse Compton scattering of soft thermal photons by ultrarelativistic charges is the most efficient production mechanism. We present angle-dependent upscattering spectra and pulsed intensity maps for uncooled, relativistic electrons injected in inner regions of magnetar magnetospheres, calculated using collisional integrals over field loops. Our computations employ a new formulation of the QED Compton scattering cross section in strong magnetic fields that is physically correct for treating important spin-dependent effects in the cyclotron resonance, thereby producing correct photon spectra. The spectral cutoff energies are sensitive to the choices of observer viewing geometry, electron Lorentz factor, and scattering kinematics. We find that electrons with energies ≲15 MeV will emit most of their radiation below 250 keV, consistent with inferred turnovers for magnetar hard X-ray tails. More energetic electrons still emit mostly below 1 MeV, except for viewing perspectives sampling field-line tangents. Pulse profiles may be singly or doubly peaked dependent on viewing geometry, emission locale, and observed energy band. Magnetic pair production and photon splitting will attenuate spectra to hard X-ray energies, suppressing signals in the Fermi-LAT band. The resonant Compton spectra are strongly polarized, suggesting that hard X-ray polarimetry instruments such as X-Calibur, or a future Compton telescope, can prove central to constraining model geometry and physics.
Migration velocity analysis by wave-field extrapolation

Velocity information is essential to both common midpoint (CMP) stacking and migration. CMP stacking provides the basis for conventional velocity estimation techniques in that, for a number of trial velocities, the stack response of a CMP gather is computed and displayed in the form of a velocity table. An alternative approach to velocity estimation makes use of the basic ingredients of migration—downward extrapolation and imaging of seismic wave fields. The procedure involves migration of a CMP gather with a number of trial velocities and collection of the zero‐offset information, again in the form of a velocity table. Operating on a CMP gather, the migration‐based approach produces results similar to those of the conventional method. Analyses of synthetic CMP gathers using both methods show essentially equivalent treatments of seismic signal, and similar dependence of accuracy and resolving power on recording geometry. We have extended the migration‐based approach to include more than one CMP gather in .
Structural Features Affecting the Interactions and Transportability of LAT1-Targeted Phenylalanine Drug Conjugates

L-type amino acid transporter 1 (LAT1) transfers essential amino acids across cell membranes. Owing to its predominant expression in the blood–brain barrier and tumor cells, LAT1 has been exploited for drug delivery and targeting to the central nervous system (CNS) and various cancers. Although the interactions of amino acids and their mimicking compounds with LAT1 have been extensively investigated, the specific structural features for an optimal drug scaffold have not yet been determined. Here, we evaluated a series of LAT1-targeted drug-phenylalanine conjugates (ligands) by determining their uptake rates by in vitro studies and investigating their interaction with LAT1 via induced-fit docking. Combining the experimental and computational data, we concluded that although LAT1 can accommodate various types of structures, smaller compounds are preferred. As the ligand size increased, its flexibility became more crucial in determining the compound’s transportability and interactions. Compounds with linear or planar structures exhibited reduced uptake; those with rigid lipophilic structures lacked interactions and likely utilized other transport mechanisms for cellular entry. Introducing polar groups between aromatic structures enhanced interactions. Interestingly, compounds with a carbamate bond in the aromatic ring’s para-position displayed very good transport efficiencies for the larger compounds. Compared to the ester bond, the corresponding amide bond had superior hydrogen bond acceptor properties and increased interactions. A reverse amide bond was less favorable than a direct amide bond for interactions with LAT1. The present information can be applied broadly to design appropriate CNS or antineoplastic drug candidates with a prodrug strategy and to discover novel LAT1 inhibitors used either as direct or adjuvant cancer therapy.