Miracle-dz/UniFAR-FTUs huggingface dataset:
OPTICAL IDENTIFICATION OF CEPHEIDS IN 19 HOST GALAXIES OF TYPE Ia SUPERNOVAE AND NGC 4258 WITH THE HUBBLE SPACE TELESCOPE

We present results of an optical search conducted as part of the SH0ES project (Supernovae and H0 for the Equation of State of dark energy) for Cepheid variable stars using the Hubble Space Telescope (HST) in 19 hosts of Type Ia supernovae (SNe Ia) and the maser-host galaxy NGC 4258. The targets include nine newly imaged SN Ia hosts using a novel strategy based on a long-pass filter that minimizes the number of HST orbits required to detect and accurately determine Cepheid properties. We carried out a homogeneous reduction and analysis of all observations, including new universal variability searches in all SN Ia hosts, which yielded a total of 2200 variables with well-defined selection criteria, the largest such sample identified outside the Local Group. These objects are used in a companion paper to determine the local value of H0 with a total uncertainty of 2.4%.
CONSTRAINTS ON THE MASS AND RADIUS OF THE NEUTRON STAR XTE J1807-294

The accreting millisecond pulsar XTE J1807-294 is studied through a pulse-shape modeling analysis. The model includes blackbody and Comptonized emission from the one visible hot spot and makes use of the Oblate Schwarzschild approximation for ray-tracing. We include a scattered light contribution, which accounts for flux scattered off an equatorial accretion disk to the observer including time delays in the scattered light. We give limits to mass and radius for XTE J1807-294 and compare these to limits determined for SAX J1808-3658 and XTE J1814-334 previously determined using similar methods. The resulting allowed region for mass–radius curves is small but consistent with a mass–radius relation with nearly constant radius (∼12 km) for masses between 1 and 2.5 solar masses.
The Effect of Soft Tissue and Bone Morphology on the Stresses in the Foot and Ankle

THE EFFECT OF SOFT TISSUE AND BONE MORPHOLOGY ON THE STRESSES IN THE FOOT AND ANKLE Jinhyuk Kim Old Dominion University, 2022 Director: Dr. Stacie I. Ringleb The foot and ankle interface with the ground, thus they absorb reaction forces and initiate load distribution through the body. The plantar fascia (PF) is a flexible structure that absorbs reaction forces and distributes loading across the foot. It is frequently a source of foot pain especially when people have plantar fasciitis and/or diabetes mellitus. Finite element (FE) models of the foot and ankle were created to examine the function however, the plantar fascia is frequently modeled as a 1D tension only spring, which does not represent variations caused by injury and/or disease. As models move toward being patient specific, understanding what components of a model can be generic versus what should be patient specific is critical when minimizing the time to create and simulate results. The purpose of this dissertation was to develop 3D finite element foot and ankle models including different thickness of 3D solid plantar fascia (i.e., 3mm, 4mm, and 5mm) and different ankle positions (i.e., neutral position, 10° dorsiflexion, and 10° plantarflexion). Additionally, the effect of different thicknesses of cartilage (i.e., 0.5mm, 1.0mm, and 1.7mm) and bone morphology (health and injured) was investigated in a model of the talocrural joint. As the thickness of plantar fascia increased, the strains of plantar fascia were increased, and the peak plantar pressure moved from hindfoot to forefoot. Also, the peak plantar pressures were highest when the foot was in 10° of plantarflexion and lowest in the neutral position. Finally, contact area decreased with decreasing cartilage thickness, with a greater decrease in contact area in healthy ankles. In 3 models, contact stress increased as cartilage thickness decreased. The fourth model had little decrease in contact area, thus the contact pressures may have been affected more by bone morphology. In conclusion, in models of the foot and ankle, the plantar fascia can be generic if it is less than 4 mm thick, a variety of foot positions should be considered, and specific bone morphologies should be included in the ankle if there is a known pathology.
Entanglement entropy of two disjoint intervals in c = 1 theories

We study the scaling of the Rényi entanglement entropy of two disjoint blocks of critical lattice models described by conformal field theories with central charge c = 1. We provide the analytic conformal field theory result for the second order Rényi entropy for a free boson compactified on an orbifold describing the scaling limit of the Ashkin–Teller (AT) model on the self-dual line. We have checked this prediction in cluster Monte Carlo simulations of the classical two-dimensional AT model. We have also performed extensive numerical simulations of the anisotropic Heisenberg quantum spin chain with tree tensor network techniques that allowed us to obtain the reduced density matrices of disjoint blocks of the spin chain and to check the correctness of the predictions for Rényi and entanglement entropies from conformal field theory. In order to match these predictions, we have extrapolated the numerical results by properly taking into account the corrections induced by the finite length of the blocks on the leading scaling behavior.
Non‐Riemannian model of the space‐time responsible for quantum effects

A class of homogeneous isotropic space‐time models including pseudo‐Euclidean space as a special case is considered. Such a model is chosen, where the particle motion is described in the most adequate way. It means that the world tubes of all free particles (both classical and quantal) are characteristic geometrical structures of the space‐time. The world function σ of this model has the form σ=σE+σ0, σE>σ0 where σE is the world function of the pseudo‐Euclidean space, σ0 is a constant responsible for quantum effects. It is proportional to Planck’s constant ℏ.
Cosmological parameters from the comparison of peculiar velocities with predictions from the 2M++ density field

Abstract Using redshifts from the 2M++ redshift compilation, we reconstruct the density of galaxies within 200 h −1 Mpc, and compare the predicted peculiar velocities Tully-Fisher and SNe peculiar velocities. The comparison yields a best-fit value of β ≡ Ωm 0.55/b* = 0.431 ± 0.021, suggesting Ωm 0.55σ8,lin = 0.401 ± 0.024, in good agreement with other probes. The predicted peculiar velocity of the Local Group from sources within the 2M++ volume is 540 ± 40 km s−1, towards l = 268° ± 4°, b = 38° ± 6°, which is misaligned by only 10° with the Cosmic Microwave Background dipole. To account for sources outside the 2M++ volume, we fit simultaneously for β* and an external bulk flow in our analysis. The external bulk flow has a velocity of 159 ± 23 km s−1 towards l = 304° ± 11°, b6° ± 13°.
THE CONTRIBUTION OF SUPERNOVAE TO COSMIC REIONIZATION

While stars are widely discussed as the source of the high-energy photons that reionized the universe, an additional source of ionizing photons that must also contribute to reionization in this scenario are the supernovae (SNe) which mark the end of the life of massive stars. Here we estimate the relative contributions of SNe and stars to reionization. While the rate at which ionizing photons are produced in SNe shocks is well below that at which they are produced by stars, the harder spectra of radiation emitted from SNe lead to an enhanced escape fraction of SN-generated photons relative to that of stellar photons. In particular, along a given line of sight out of a galaxy, we find that for neutral hydrogen column densities NH ≳ 1018 cm−2 the contribution to reionization from SNe is greater than that from stars. Drawing on the results of simulations presented in the literature, we find that the overall (line-of-sight-averaged) SNe shock-generated ionizing photon escape fraction is larger than the stellar photon escape fraction by a factor of ≃4 to ≃7, depending on the metallicity of the stellar population. Overall, our results suggest that the effect of SNe is an enhancement of up to ∼10% in the fraction of hydrogen reionized by stellar sources. We briefly discuss the implications of our results for the population of galaxies responsible for reionization.
Plasmonic metagratings for simultaneous determination of Stokes parameters

Measuring light's state of polarization is an inherently difficult problem, since the phase information between orthogonal polarization states is typically lost in the detection process. In this work, we bring to the fore the equivalence between normalized Stokes parameters and diffraction contrasts in appropriately designed phase-gradient birefringent metasurfaces and introduce a concept of all-polarization birefringent metagratings. The metagrating, which consists of three interweaved metasurfaces, allows one to easily analyze an arbitrary state of light polarization by conducting simultaneous (i.e., parallel) measurements of the correspondent diffraction intensities that reveal immediately the Stokes parameters of the polarization state under examination. Based on plasmonic metasurfaces operating in reflection at the wavelength of 800 nm, we design and realize phase-gradient birefringent metasurfaces and the correspondent metagrating, while experimental characterization of the fabricated components convincingly demonstrates the expected functionalities. We foresee the use of the metagrating in compact polarimetric setups at any frequency regime of interest.
Non-normal numbers with respect to infinite Markov partitions

In the present paper we investigate two special types of non-normal numbers. On the one hand we call a number extremely non-normal if the set of accumulation points of its frequency of blocks vector is the full set of shift invariant probability vectors. On the other hand we call a number having maximal oscillation frequency if for any fixed block the set of accumulation points of its frequency vector is the full set of possible probability vectors. The goal is to investigate the Baire category of these numbers for infinite Markov partitions.
Distribution amplitudes of radially-excited pi- and K-mesons

A symmetry-preserving truncation of the two-body bound state problem in relativistic quantum field theory is used to compute the leading-twist parton distribution amplitudes (PDAs) for the first radial excitations of the $\ensuremath{\pi}$ and $K$ mesons. In common with ground states in these channels, the PDAs are found to be dilated with respect to the relevant conformal-limit form and skewed toward the heavier valence quark in asymmetric systems. In addition, the PDAs of radially excited pseudoscalar mesons are not positive definite, owing to the fact that dynamical chiral symmetry breaking (DCSB) forces the leptonic decay constant of such states to vanish in the chiral limit. These results highlight that DCSB is expressed visibly in every pseudoscalar meson constituted from light quarks. Hence, so long as its impact is empirically evident in the pseudoscalar members of a given spectrum level, it is unlikely that chiral symmetry is restored in any of the hadrons that populate this level.
Towards a realistic astrophysical interpretation of the gamma-ray Galactic center excess

A spherical-symmetric gamma-ray emission from {the inner region of the Galaxy (at least up to roughly 10° in latitude and longitude)} has been recently identified in Fermi-LAT data, and initially associated to dark matter particle annihilations. Guided by the evidence for a high gas density in the inner kpc of the Galaxy correlated with a very large Supernova rate, and hence with ongoing cosmic-ray acceleration, we investigate instead the possibility of addressing this excess in terms of ordinary cosmic-ray sources and standard steady-state diffusion. We {alter the source term, and consistently the correlated gamma-ray emissions, in the context of a template-fitting analysis. We focus on a region of interest (ROI) defined as: |l| < 20°; 2° < |b| < 20°, with l and b the Galactic longitude and latitude coordinates. } We analyze in detail the overall goodness of the fit of our framework, and perform a detailed direct comparison against data examining profiles in different directions. Remarkably, the test statistic of the fit related to our scenario turns out to be as good as the Dark Matter one in the ROI here considered.
Central European Journal of Mathematics Instanton bundles on Fano threefolds

We introduce the notion of an instanton bundle on a Fano threefold of index 2. For such bundles we give an analogue of a monadic description and discuss the curve of jumping lines. The cases of threefolds of degree 5 and 4 are considered in a greater detail. MSC: 14J60, 14F05
The colour-magnitude relation of elliptical and lenticular galaxies in the ESO distant cluster survey

In this paper we study the colour-magnitude relation (CMR) for a sample of 172 morphologically classified elliptical and S0 cluster galaxies from the ESO Distant Cluster Survey (EDisCS) at 0.4 less than or similar to z less than or similar to 0.8. The intrinsic colour scatter about the CMR is very small ( = 0.076) in rest-frame U - V. However, there is a small minority of faint early-type galaxies (7 per cent) that are significantly bluer than the CMR. We observe no significant dependence of Sigma(int) with redshift or cluster velocity dispersion. Because our sample is strictly morphologically selected, this implies that by the time cluster elliptical and S0 galaxies achieve their morphology, the vast majority have already joined the red sequence. The only exception seems to be the very small fraction of faint blue early types. Assuming that the intrinsic colour scatter is due to differences in stellar population ages, we estimate the galaxy formation redshift z(F) of each cluster and find that z(F) does not depend on the cluster velocity dispersion. However, z(F) increases weakly with cluster redshift within the EDisCS sample. This trend becomes very clear when higher redshift clusters from the literature are included. This suggests that, at any given redshift, in order to have a population of fully formed ellipticals and S0s they needed to have formed most of their stars similar or equal to 2-4 Gyr prior to observation. That does not mean that all early-type galaxies in all clusters formed at these high redshifts. It means that the ones we see already having early-type morphologies also have reasonably old stellar populations. This is partly a manifestation of the 'progenitor bias', but also a consequence of the fact that the vast majority of the early-type galaxies in clusters (in particular the massive galaxies) were already red (i.e. already had old stellar populations) by the time they achieved their morphology. Elliptical and S0 galaxies exhibit very similar colour scatter, implying similar stellar population ages. The scarcity of blue S0s indicates that, if they are the descendants of spirals whose star formation has ceased, the parent galaxies were already red when they became S0s. This suggests the red spirals found preferentially in dense environments could be the progenitors of these S0s. We also find that fainter early-type galaxies finished forming their stars later (i.e. have smaller z(F)), consistent with the cluster red sequence being built over time and the brightest galaxies reaching the red sequence earlier than fainter ones. Combining the CMR scatter analysis with the observed evolution in the CMR zero-point we find that the early-type cluster galaxy population must have had their star formation truncated/stopped over an extended period delta t greater than or similar to 1 Gyr.
COMPLEX SCATTERED RADIATION FIELDS AND MULTIPLE MAGNETIC FIELDS IN THE PROTOSTELLAR CLUSTER IN NGC 2264

Near-infrared imaging polarimetry in the J, H, and Ks bands has been carried out for the protostellar cluster region around NGC 2264 IRS 2 in the Monoceros OB1 molecular cloud. Various infrared reflection nebula clusters (IRNCs) associated with NGC 2264 IRS 2 and the IRAS 12 S1 core, as well as local infrared reflection nebulae (IRNe), were detected. The illuminating sources of the IRNe were identified with known or new near- and mid-infrared sources. In addition, 314 point-like sources were detected in all three bands and their aperture polarimetry was studied. Using a color–color diagram, reddened field stars and diskless pre-main-sequence stars were selected to trace the magnetic field (MF) structure of the molecular cloud. The mean polarization position angle of the point-like sources is 81° ± 29° in the cluster core, and 58° ± 24° in the perimeter of the cluster core, which is interpreted as the projected direction on the sky of the MF in the observed region of the cloud. The Chandrasekhar–Fermi method gives a rough estimate of the MF strength to be about 100 μG. A comparison with recent numerical simulations of the cluster formation implies that the cloud dynamics is controlled by the relatively strong MF. The local MF direction is well associated with that of CO outflow for IRAS 12 S1 and consistent with that inferred from submillimeter polarimetry. In contrast, the local MF direction runs roughly perpendicular to the Galactic MF direction.
Comment on"How many principles does it take to change a light bulb ... into a laser?"by Howard M. Wiseman, Physica Scripta 91 (3), 033001 (2016)

In a recent article entitled ”How many principles does it take to change a light bulb…into a laser? ” by Howard M. Wiseman, Physica Scripta 91 (3), 033001 (2016) the author addresses the question as expressed by the title in summarizing what he considers as the fundamental features which distinguish laser light from thermal light. He draws the conclusion that there are in fact 4 principles making this difference which he outlines in detail. Here, in this comment I am analyzing this extremely well formulated question in the framework of the Hanbury-Brown & Twiss experiment, thus also celebrating its 60 th anniversary. I am giving a straightforward, concise and unique answer to this question, namely emphasizing that the intensity correlations or the photon statistics make the difference between light emitted by a light bulb and that of a laser.
On the Incidence of Wise Infrared Excess Among Solar Analog, Twin, and Sibling Stars

This study presents a search for infrared (IR) excess in the 3.4, 4.6, 12, and 22 μm bands in a sample of 216 targets, composed of solar sibling, twin, and analog stars observed by the Wide-field Infrared Survey Explorer (WISE) mission. In general, an IR excess suggests the existence of warm dust around a star. We detected 12 μm and/or 22 μm excesses at the 3σ level of confidence in five solar analog stars, corresponding to a frequency of 4.1% of the entire sample of solar analogs analyzed, and in one out of 29 solar sibling candidates, confirming previous studies. The estimation of the dust properties shows that the sources with IR excesses possess circumstellar material with temperatures that, within the uncertainties, are similar to that of the material found in the asteroid belt in our solar system. No photospheric flux excess was identified at the W1 (3.4 μm) and W2 (4.6 μm) WISE bands, indicating that, in the majority of stars of the present sample, no detectable dust is generated. Interestingly, among the 60 solar twin stars analyzed in this work, no WISE photospheric flux excess was detected. However, a null-detection excess does not necessarily indicate the absence of dust around a star because different causes, including dynamic processes and instrument limitations, can mask its presence.
EFL University Students’ Metacognitive Awareness of Reading Strategy and Its Correlation with Their Reading Comprehension

Metacognitive awareness of reading strategy has a tremendous impact on the educational process, especially in acquiring a second language. It is concerned with not only what they suggest about how students organize their interactions with the context, but also with how they might employ the strategies that are still relevant to reading comprehension effectiveness. However, the EFL learners are still having a lack using metacognitive awareness of reading strategies significantly because of unknowing and inadequate understanding of what reading strategies to use, how and when to use them appropriately. Hence, the present study is attempted to locate the relationship between EFL learners’ metacognitive awareness of reading strategy and reading comprehension. A quantitative study, with 60 EFL students as participants, was conducted by using a questionnaire, and reading comprehension score to discover the level of EFL students’ Metacognitive Awareness of Reading Strategy. Those are the Metacognitive Awareness of Reading Strategy Inventory - revised (MARSI-R) and the Test English Proficiency (TEP) to discover the level of EFL students’ metacognitive awareness. The result of this study showed that 49 participants (mean 3.5 – >3.5), categorized as high group levels, and 11 participants (mean 2.5 – 3.4), categorized as moderate group levels. This research also revealed that the most strategies used by EFL learners found using PRS (Problem-solving strategies) M = 3.99; GRS (Global reading strategies) M = 3.98; and, SRS (Support reading strategies) M = 3.65. For the result of the Spearman Rho Coefficient showed that there is no correlation between EFL learners’ metacognitive awareness of reading strategy and reading comprehension (ρ value = .986).
Money’s predictive role in output: evidence from recent data

ABSTRACT We measure and assess the predictive performance of money in explaining output for the US, the UK, the Euro Area and Poland. Our approach, which uses more recent data and a larger set of areas, focuses on whether money ‘Granger causes’ output while taking into account the statistical properties of the data, which has implications for Granger causality tests. In addition to simple sum monetary aggregates, we use Divisia monetary aggregates, which are theoretically shown to be the actual measure of monetary services. Our results confirm that movements in money are still relevant in explaining movements in output, particularly when Divisia monetary aggregate is used. While the models using ‘narrow’ money, both simple sum and Divisia, provide mixed evidence of support, what appears to be robust across countries, is the predictive power of ‘broad Divisia’ in explaining output. Furthermore, our research finds no evidence that the statistical significance of money decreases as more variables are added to the model, or models with level variables produce more significant results than models with growth variables. In fact, rather than the level of money, it is the growth rate of money and the deviation of the growth rate of money from its time trend, which ‘Granger causes’ output.
Wave equations on the linear mass Vaidya metric

We discuss the near-singularity region of the linear mass Vaidya metric. In particular, we investigate the structure in the numerical solutions for the scattering of scalar and electromagnetic metric perturbations from the singularity. We observe that, around the total evaporation point, quasinormal-like oscillations appear, indicating that this may be an interesting model for the description of the end point of black hole evaporation.