Miracle-dz/UniFAR-FTUs huggingface dataset:
TEST OF PARAMETRIZED POST-NEWTONIAN GRAVITY WITH GALAXY-SCALE STRONG LENSING SYSTEMS

Based on a mass-selected sample of galaxy-scale strong gravitational lenses from the SLACS, BELLS, LSD, and SL2S surveys and using a well-motivated fiducial set of lens-galaxy parameters, we tested the weak-field metric on kiloparsec scales and found a constraint on the post-Newtonian parameter under the assumption of a flat ΛCDM universe with parameters taken from Planck observations. General relativity (GR) predicts exactly γ = 1. Uncertainties concerning the total mass density profile, anisotropy of the velocity dispersion, and the shape of the light profile combine to systematic uncertainties of ∼25%. By applying a cosmological model-independent method to the simulated future LSST data, we found a significant degeneracy between the PPN γ parameter and the spatial curvature of the universe. Setting a prior on the cosmic curvature parameter −0.007 < Ωk < 0.006, we obtained the constraint on the PPN parameter that . We conclude that strong lensing systems with measured stellar velocity dispersions may serve as another important probe to investigate validity of the GR, if the mass-dynamical structure of the lensing galaxies is accurately constrained in future lens surveys.
Melanopogenesis: dark matter of (almost) any mass and baryonic matter from the evaporation of primordial black holes weighing a ton (or less)

The evaporation of primordial black holes with a mass in the 1 gram≲ MPBH≲1000 kg range can lead to the production of dark matter particles of almost any mass in the range 0.1 MeV≲ mDM≲ 1018 GeV with the right relic density at very early times, τ≲ 10−10 s. We calculate, as a function of the primordial black holes mass and initial abundance, the combination of dark matter particle masses and number of effective dark degrees of freedom leading to the right abundance of dark matter today, whether or not evaporation stops around the Planck scale. In addition, since black hole evaporation can also lead to the production of a baryon asymmetry, we calculate where dark matter production and baryogenesis can concurrently happen, under a variety of assumptions: baryogenesis via grand unification boson decay, via leptogenesis, or via asymmetric co-genesis of dark matter and ordinary matter. Finally, we comment on possible ways to test this scenario.
Study of p-mode excitation and damping rate variations from IRIS$^{++}$ observations

11 years of low degree helioseismic data collected by the IRIS ++ network ( International Research of the Interior of the Sun ) have been analyzed. The epoch covered (mid-1989 to end-1999) spans the maximum and the falling phase of solar cycle 22 and the rising phase of the current solar cycle 23. Annual timeseries with an overlap of 6 months are used to study the variations with solar activity of the p -mode frequencies $\nu_{n,\ell}$, heights $H_{n,\ell}$, and linewidths $\Gamma_{n,\ell}$, taking into account the effects of the window function. These are used to infer variations in the velocity power $ $ and the energy supply rate $\dot{E}_{n,\ell}$ which relate to changes in the excitation and the damping of the modes. We find global changes over the range 2600 $\leq \nu \leq 3600~\mu$Hz of about -26%, 11%, -11% for the heights, the linewidths, and the velocity power respectively, and a constant energy supply to the modes.
Oligomorphic transformation monoids and homomorphism-homogeneous structures

A structure is called homomorphism-homogeneous if every homomorphism between ﬁnitely generated substructures of the structure extends to an endomorphism of the structure (P. J. Cameron and J. Neˇsetˇril, 2006). In this paper we introduce oligomorphic transformation monoids in full analogy to oligomorphic permutation groups and use this notion to propose a solution to a problem, posed by Cameron and Neˇsetˇril in 2006, to characterize endomorphism monoids of homomorphism-homogeneous relational structures over ﬁnite signatures. However, the main goal of this paper is to provide more evidence that the concept of homomorphism-homogeneity is analogous to that of ultrahomogeneity. It turns out that many results that hold for ultrahomogeneous or ω -categorical structures have their analogues in the class of countable homomorphism-homogeneous structures, or countable weakly oligomorphic structures (these are structures whose endomorphism monoids are oligomorphic). For example, we characterize countable weakly oligomorphic structures in terms of the Ryll-Nardzewski property with respect to positive formulas; we prove that for countable weakly oligomorphic structures homomorphism-homogeneity is equivalent to quantiﬁer elimination for positive formulas; ﬁnally, we prove that an ω -categorical structure is both ultrahomogeneous and homomorphism-homogeneous if and only if it has quantiﬁer elimination where positive formulas reduce to positive quantiﬁer-free formulas.
A Local Approach to Chinburg's Root Number Conjecture

Suppose given a finite Galois extension K/k of number fields with group G and a finite sufficiently large G‐stable set S of primes of K, write E for the group of S‐units in K, and Δ S for the augmentation submodule of the Z‐free permutation module ZS on S. Let also A, B be finitely generated cohomologically trivial ZG‐modules, and τ Tate's canonical class defining a 2‐extension E↣A→B↠ΔS . Chinburg has assigned the algebraic invariant Ω = [A]−[B] ∈ K0ZG to τ and conjectured that Ω equals the root number class W(K/k), an analytic invariant defined by Cassou‐Nogués and Fröhlich, and based on Artin's root numbers. We combine Ω with G‐injections φ:ΔS↣E to obtain lifts Ωφ∈K0T(ZG) of Ω in the Grothendieck group of finite ZG‐modules of finite projective dimension. Unlike K0ZG, the group K0T(ZG) has a natural decomposition as a direct sum ⊕ K0T(ZlG), over all finite rational primes l. This provides a local setting for the study of the Ωφ.
YIELD-STABILITY DIFFERENCES AMONG FRENCH BEAN (PHASEOLUS VULGARIS L.) GENOTYPES UNDER NORTH- WESTERN HIMALAYAN CONDITIONS

French bean (Phaseolus vulgaris L.) is one of the most important leguminous vegetables, which is grown for fresh pod consumption and for processing as a frozen vegetable in many countries (Biswas et al., 2010). It is an annual, diploid (2n=2x=22) species derived from wild ancestors distributed from northern Mexico to north western Argentina (Galvan et al., 2003) and regarded as “grain of hope” as it is an important component of subsistence agriculture and offer an alternative for diversification of agricultural system (Sofi et al., 2011). But, despite continuous breeding efforts, its average yield is low due to unsuitable cultivars, biotic and abiotic stresses, genetic drift in the cultivars and development of new pathogen races.
Pulsar Wind Bubble Blowout from a Supernova

For pulsars born in supernovae, the expansion of the shocked pulsar wind nebula is initially in the freely expanding ejecta of the supernova. While the nebula is in the inner flat part of the ejecta density profile, the swept-up, accelerating shell is subject to the Rayleigh–Taylor instability. We carried out two- and three-dimensional simulations showing that the instability gives rise to filamentary structure during this initial phase but does not greatly change the dynamics of the expanding shell. The flow is effectively self-similar. If the shell is powered into the outer steep part of the density profile, the shell is subject to a robust Rayleigh–Taylor instability in which the shell is fragmented and the shocked pulsar wind breaks out through the shell. The flow is not self-similar in this phase. For a wind nebula to reach this phase requires that the deposited pulsar energy be greater than the supernova energy, or that the initial pulsar period be in the ms range for a typical 1051 erg supernova. These conditions are satisfied by some magnetar models for Type I superluminous supernovae. We also consider the Crab Nebula, which may be associated with a low energy supernova for which this scenario applies.
A simulation study of microstructure evolution during solidification process of liquid metal Ni

A molecular dynamics simulation study has been performed for the microstructure evolution in a liquid metal Ni system during crystallization process at two cooling rates by adopting the embedded atom method (EAM) model potential. The bond-type index method of Honeycutt–Andersen (HA) and a new cluster-type index method (CTIM-2) have been used to detect and analyse the microstructures in this system. It is demonstrated that the cooling rate plays a critical role in the microstructure evolution: below the crystallization temperature Tc, the effects of cooling rate are very remarkable and can be fully displayed. At different cooling rates of 2.0 × 1013 K · s−1 and 1.0 × 1012 K · s−1, two different kinds of crystal structures are obtained in the system. The first one is the coexistence of the hcp (expressed by (12 0 0 0 6 6) in CTIM-2) and the fcc (12 0 0 0 12 0) basic clusters consisting of 1421 and 1422 bond-types, and the hcp basic cluster becomes the dominant one with decreasing temperature, the second one is mainly the fcc (12 0 0 0 12 0) basic clusters consisting of 1421 bond-type, and their crystallization temperatures Tc would be 1073 and 1173 K, respectively.
Long-period variables in the Magellanic Clouds: Supergiants, AGB stars, supernova precursors, planetary nebula precursors, and enrichment of the interstellar medium

Infrared JHK magnitudes and low-dispersion red spectra have been obtained for 90 long-period variables (LPVs) in the Small and Large Magellanic Clouds. The LPVs fall into two distinct groups, core helium (or carbon) burning supergiants and stars on the asymptotic giant branch (AGB). The supergiants have small pulsation amplitudes in K ( or approx. =5 M/sub sun/ produce supernovae while less massive stars produce planetary nebulae with nebula masses from approx.0. 1--2.1 M/sub sun/. The coreburning red supergiants appear highly overluminous for their pulsation mass, indicating that they have lost up to half their mass since the main-sequence phase. « less
Critical Charge in Gapped Graphene: the role of the screening of the interaction potential by $\sigma$-orbitals

Due to its unique structure, graphene provides a condensed-matter model of particle physics phenomena. One is the critical charge which is highly interested. The investigation of critical charge in gapped graphene is performed within single particle approach by means of Dirac equation integration. The screened Coulomb interaction between charged defect and graphene electron excitations is investigated. Two kinds of mass gap generation and various values of substrate dielectric permittivities are considered. It is shown that the critical charge phenomenon can be observed even with quite small charges for physically motivated parameters.
A Numerical Investigation of the Eyewall Evolution in a Landfalling Typhoon

Abstract An interesting eyewall evolution occurred in Typhoon Zeb (1998) when it devastated Luzon. The eyewall of Zeb contracted before landfall and broke down and weakened after landfall; then a much larger new eyewall formed and strengthened as it left Luzon and reentered the ocean. The fifth-generation Pennsylvania State University–NCAR Mesoscale Model (MM5) with four nested domains was used to perform numerical experiments to understand the effects of terrain and land surface variation on the observed eyewall evolution. Results show that the presence of Luzon plays a critical role in the observed eyewall evolution. Quite different from the conventional concentric eyewall replacement, the eyewall replacement that occurred in Typhoon Zeb was triggered by the mesoscale landmass and terrain variation with a horizontal scale similar to the core of the typhoon. In Typhoon Zeb, the original eyewall contracted and broke down because of enhanced surface friction after landfall. The outer eyewall was triggered .
The Hot, Accreted Halo of NGC 891

Galaxies are surrounded by halos of hot gas whose mass and origin remain unknown. One of the most challenging properties to measure is the metallicity, which constrains both of these. We present a measurement of the metallicity around NGC 891, a nearby, edge-on, Milky Way analog. We find that the hot gas is dominated by low-metallicity gas near the virial temperature at and and that this gas coexists with hotter ( ) gas that is concentrated near the star-forming regions in the disk. Model choices lead to differences of , and higher signal-to-noise ratio observations would be limited by systematic error and plasma emission model or abundance ratio choices. The low-metallicity gas is consistent with the inner part of an extended halo accreted from the intergalactic medium, which has been modulated by star formation. However, there is much more cold gas than hot gas around NGC 891, which is difficult to explain in either the accretion or supernova-driven outflow scenarios. We also find a diffuse nonthermal excess centered on the galactic center and extending to 5 kpc above the disk with a 0.3–10 keV . This emission is inconsistent with inverse Compton scattering or single-population synchrotron emission, and its origin remains unclear.
The Identification of Hydrogen-deficient Cataclysmic Variable Donor Stars

We have used ATLAS12 to generate hydrogen-deficient stellar atmospheres to allow us to construct synthetic spectra to explore the possibility that the donor stars in some cataclysmic variables (CVs) are hydrogen deficient. We find that four systems, AE Aqr, DX And, EY Cyg, and QZ Ser, have significant hydrogen deficits. We confirm that carbon and magnesium deficits, and sodium enhancements, are common among CV donor stars. The three Z Cam systems we observed are found to have solar metallicities and no abundance anomalies. Two of these objects, Z Cam and AH Her, have M-type donor stars—much cooler than expected, given their long orbital periods. By using the combination of equivalent width measurements and light curve modeling, we have developed the ability to account for contamination of the donor star spectra by other luminosity sources in the binary. This enables more realistic assessments of secondary star metallicities. We find that the use of equivalent width measurements should allow for robust metallicities and abundance anomalies to be determined for CVs with M-type donor stars.
Tomographic Separation of Composite Spectra. X. The Massive Close Binary HD 101131

We present the first orbital elements for the massive close binary HD 101131, one of the brightest objects in the young open cluster IC 2944. This system is a double-lined spectroscopic binary in an elliptical orbit with a period of 9.64659 ± 0.00012 days. It is a young system of unevolved stars (approximately 2 million yr old) that are well within their critical Roche surfaces. We use a Doppler tomography algorithm to reconstruct the individual component optical spectra, and we apply well-known criteria to arrive at classifications of O6.5 V((f)) and O8.5 V for the primary and secondary, respectively. We compare the reconstructed spectra of the components to single-star spectrum standards to determine a flux ratio of f2/f1 = 0.55 ± 0.08 in the V band. Both components are rotating faster than synchronously. We estimate the temperatures and luminosities of the components from the observed spectral classifications, composite V magnitude, and cluster distance modulus. The lower limits on the masses derived from the orbital elements and the lack of eclipses are 25 and 14 M☉ for the primary and secondary, respectively. These limits are consistent with the somewhat larger masses estimated from the positions of the stars in the Hertzsprung-Russell diagram and evolutionary tracks for single stars.
Quasiparticle interference in ZrSiS: Strongly band-selective scattering depending on impurity lattice site

Scanning tunneling microscopy visualizations of quasiparticle interference (QPI) enable powerful insights into the k-space properties of superconducting, topological, Rashba and other exotic electronic phases, but their reliance on impurities acting as scattering centers is rarely scrutinized. Here we investigate QPI at the vacuum-cleaved (001) surface of the Dirac semimetal ZrSiS. We find that interference patterns around impurities located on the Zr and S lattice sites appear very different, and can be ascribed to selective scattering of different sub-sets of the predominantly Zr 4d-derived band structure, namely the m = 0 and m = +/-1 components. We show that the selectivity of scattering channels requires an explanation beyond the different bands' orbital characteristics and their respective charge density distributions over Zr and S lattices sites. Importantly, this result shows that the usual assumption of generic scattering centers allowing observations of quasiparticle interference to shed light indiscriminately and isotropically upon the \textit{q}-space of scattering events does not hold, and that the scope and interpretation of QPI observations can therefore be be strongly contingent on the material defect chemistry. This finding promises to spur new investigations into the quasiparticle scattering process itself, to inform future interpretations of quasiparticle interference observations, and ultimately to aid the understanding and engineering of quantum electronic transport properties.
Some Simple Methods for Estimating Intraindividual Variability in Nonlinear Mixed Effects Models

Methods are proposed to improve both population and individual inference within the nonlinear random coefficient regression framework by incorporating possible heterogeneity in the intraindividual variance structure. These methods extend existing variance function estimation techniques by pooling information across individuals. The methods are appropriate when it is reasonable to assume that there exists a common intraindividual variance structure.
Atmospheric Parameters and Iron Abundances of Low-Mass Pre-Main-Sequence Stars in Nearby Star Formation Regions

High-resolution echelle spectra have been obtained for low-mass pre-main-sequence stars in the Taurus-Auriga, Orion, Chamaeleon, Ophiuchus, and other star formation regions. Using temperature-sensitive individual metallic line ratios, new effective temperatures are determined for a sample of 30 G and K pre-main-sequence stars in nearby star-forming clouds to an accuracy of ± 200 K or better in most cases. Comparison of these values with previous spectral classifications using low-resolution spectra reveals occasional large discrepancies in spectral type. Microturbulences derived for 23 “weak line” T Tauri stars range as high as 3.1 ± 0.4 km s–1. The mean microturbulent velocity of the sample is 1.6 ± 0.6 km s–1. Using these new effective temperatures and microturbulences, iron abundances have been determined for 30 pre-main-sequence stars in several northern and southern sky star-formation regions. By determining the mean [Fe/H] for at least five stars in each cloud, bulk metallicities have been derived for the Taurus-Auriga, Orion, Chamaeleon, and Ophiuchus molecular clouds. [Fe/H] is approximately solar in all the regions surveyed.
Measurement of electron-neutrino electron elastic scattering

The cross section for the elastic scattering reaction ${\ensuremath{\nu}}_{e}{+e}^{\ensuremath{-}}\ensuremath{\rightarrow}{\ensuremath{\nu}}_{e}{+e}^{\ensuremath{-}}$ was measured by the Liquid Scintillator Neutrino Detector using a ${\ensuremath{\mu}}^{+}$ decay-at-rest ${\ensuremath{\nu}}_{e}$ beam at the Los Alamos Neutron Science Center. The standard model of electroweak physics predicts a large destructive interference between the charge current and neutral current channels for this reaction. The measured cross section, ${\ensuremath{\sigma}}_{{\ensuremath{\nu}}_{e}{e}^{\ensuremath{-}}}=[10.1\ifmmode\pm\else\textpm\fi{}1.1(\mathrm{stat})\ifmmode\pm\else\textpm\fi{}1.0(\mathrm{syst})]\ifmmode\times\else\texttimes\fi{}{E}_{{\ensuremath{\nu}}_{e}}(\mathrm{MeV})\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}45}{\mathrm{cm}}^{2},$ agrees well with standard model expectations. The measured value of the interference parameter, $I=\ensuremath{-}1.01\ifmmode\pm\else\textpm\fi{}0.13(\mathrm{stat})\ifmmode\pm\else\textpm\fi{}0.12(\mathrm{syst}),$ is in good agreement with the standard model expectation of ${I}^{\mathrm{SM}}=\ensuremath{-}1.09. $ Limits are placed on neutrino flavor-changing neutral currents. An upper limit on the muon-neutrino magnetic moment of $6.8\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}10}{\ensuremath{\mu}}_{\mathrm{Bohr}}$ is obtained using the ${\ensuremath{\nu}}_{\ensuremath{\mu}}$ and ${\overline{\ensuremath{\nu}}}_{\ensuremath{\mu}}$ fluxes from ${\ensuremath{\pi}}^{+}$ and ${\ensuremath{\mu}}^{+}$ decay.
Final-year student nurses’ knowledge and understanding of diabetes and its application to practice

The aim of this study was to investigate diabetes knowledge and application to practice in final-year nursing students. An “in-house” online diabetes knowledge questionnaire was sent to 92 final-year, adult branch, BSc Nursing students. The questionnaire considered two aspects of diabetes knowledge: general diabetes knowledge and application to clinical practice. Twenty-three (25%) online questionnaires were completed. The mean (SD) overall diabetes knowledge score was 7 ± 1.36 (77.8%) correct answers from a possible score of 9. Participants scored higher in questions related to application to practice than general diabetes knowledge (85% vs 72%). Knowledge gaps were identified in relation to pathophysiology and causes of hypoglycaemia. Future curricula should involve diabetes specialist teams and consider alternative and novel educational approaches as an adjunct to traditional teaching and learning strategies.
The direct image of a vector bundle

It is well known that if M is a vector bundle over a space Y, and r: X → Y is a map, then there is an ‘induced’ vector bundle r*M over X. It is also known that a vector bundle L over X determines a ‘direct image’ vector bundle r* L over Y provided that r is a finite covering map ((1), § 1).
Detection of circumstellar helium in Type Iax progenitor systems

We present direct spectroscopic modelling of 44 Type Iax supernovae (SNe Iax) using spectral synthesis code SYNAPPS. We confirm detections of helium emission in the early-time spectra of two SNe Iax: SNe 2004cs and 2007J. These He i features are better fit by a pure-emission Gaussian than by a P-Cygni profile, indicating that the helium emission originates from the circumstellar environment rather than the SN ejecta. Based on the modelling of the remaining 42 SNe Iax, we find no obvious helium features in other SN Iax spectra. However, ${\approx } 76{{\ \rm per\ cent}}$ of our sample lack sufficiently deep luminosity limits to detect helium emission with a luminosity of that seen in SNe 2004cs and 2007J. Using the objects with constraining luminosity limits, we calculate that 33 per cent of SNe Iax have detectable helium in their spectra. We examine 11 SNe Iax with late-time spectra and find no hydrogen or helium emission from swept-up material. For late-time spectra, we calculate typical upper limits of stripped hydrogen and helium to be 2 × 10−3 M⊙ and 10−2 M⊙, respectively. While detections of helium in SNe Iax support a white dwarf–He star binary progenitor system (i.e. a single-degenerate [SD] channel), non-detections may be explained by variations in the explosion and ejecta material. The lack of helium in the majority of our sample demonstrates the complexity of SN Iax progenitor systems and the need for further modelling. With strong independent evidence indicating that SNe Iax arise from an SD channel, we caution the common interpretation that the lack of helium or hydrogen emission at late-time in SN Ia spectra rules out SD progenitor scenarios for this class.