Miracle-dz/UniFAR-FTUs huggingface dataset:
Asynchronous, online spaced-repetition training alleviates word-finding difficulties in aphasia

ABSTRACT Word-finding difficulties for naming everyday objects are often prevalent in aphasia. Traditionally, treating these difficulties has involved repeated drilling of troublesome items with a therapist. Spaced repetition schedules can improve the efficiency of such training. However, spaced repetition in a therapy environment can be both difficult to implement and time-consuming. The current study evaluated the potential utility of automated, asynchronous, online spaced repetition training for the treatment of word-finding difficulties in individuals with aphasia. Twenty-one participants completed a two-week training study, completing approximately 60 minutes per day of asynchronous online drilling. The training items were identified using a pretest, and word-finding difficulties were evaluated both at the end of training (i.e., a post-test) and four weeks later (i.e., a retention test). The trained items were separated into three different spaced-repetition schedules: (1) Short-spacing; (2) Long-spacing; and (3) Adaptive-spacing. At the retention-test, all trained items outperformed non-trained items in terms of accuracy and reaction time. Further, preliminary evidence suggested a potential reaction time advantage for the adaptive-spacing condition. Overall, online, asynchronous spaced repetition training appears to be effective in treating word-finding difficulties in aphasia. Further research will be required to determine if different spaced repetition schedules can be leveraged to enhance this effect.
THE EFFECT OF PROGENITOR AGE AND METALLICITY ON LUMINOSITY AND 56Ni YIELD IN TYPE Ia SUPERNOVAE

Timmes et al. found that metallicity variations could theoretically account for a 25% variation in the mass of 56Ni synthesized in Type Ia supernovae (SNe Ia), and thus account for a large fraction of the scatter in observed SN Ia luminosities. Higher-metallicity progenitors are more neutron rich, producing more stable burning products relative to radioactive 56Ni. We develop a new method for estimating bolometric luminosity and 56Ni yield in SNe Ia and use it to test the theory with data from the Supernova Legacy Survey. We find that the average 56Ni yield does drop in SNe Ia from high-metallicity environments, but the theory can only account for 7%–10% of the dispersion in SN Ia 56Ni mass, and thus luminosity. This is because the effect is dominant at metallicities significantly above solar, whereas we find that SN hosts have predominantly subsolar or only moderately above-solar metallicities. We also show that allowing for changes in O/Fe with the metallicity [Fe/H] does not have a major effect on the theoretical prediction of Timmes et al., so long as one is using the O/H as the independent variable. Age may have a greater effect than metallicity—we find that the luminosity-weighted age of the host galaxy is correlated with 56Ni yield, and thus more massive progenitors give rise to more luminous explosions. This is hard to understand if most SNe Ia explode when the primaries reach the Chandrasekhar mass. Finally, we test the findings of Gallagher et al. that the residuals of SNe Ia from the Hubble diagram are correlated with host galaxy metallicity, and we find no such correlation.
Clonally related composite chronic lymphocytic leukaemia and mantle cell lymphoma

Chronic lymphocytic leukaemia (CLL) is the most common adult leukaemia in the Western world, accounting for 25% of adult leukaemias. Morphologically, CLL cells are small with clumped chromatin and scant cytoplasm. Immunophenotypically, CLL cells are monotypic B cells that express CD5, CD19, CD20(dim), and CD23. Mantle cell lymphoma (MCL), accounting for 6% of all nonHodgkin Bcell lymphomas (NHL), is usually associated with a more aggressive disease course compared with CLL. Morphologically, MCL cells are heterogeneous with a diffuse, nodular, or mantle zone growth pattern in the tissue or leukaemic phase. In some cases, MCL cells are pleomorphic or blastoid, while in the majority of cases, they are small and monomorphic and are similar to CLL cells. Immunophenotypically, MCL cells have a brighter expression of Bcell markers including CD20, CD22, CD79a, and Received: 31 August 2022 | Accepted: 2 November 2022
Assessing Student Perceptions of Blended and Online Learning Courses in Pharmacoeconomics, Management, and Leadership

Objective. Blended learning combines traditional face-to-face education with online instruction. This learner-centered approach has been shown to improve student engagement, critical thinking, and performance outcomes. The objective of this study was to assess and trend student pharmacist perceptions of blended and online learning used to teach pharmacy management, leadership, and economics within a Doctor of Pharmacy (PharmD) curriculum. Methods. Qualitative methods were employed using in-depth, semistructured interviews. Second- and third-year student pharmacists were recruited by purposeful and snowball sampling and interviewed to a point of saturation. The interview guide was based on social cognitive theory. Themes identified through initial deductive thematic analysis were categorized by the three domains of social cognitive theory: cognitive, behavioral, and environmental factors. The coding team additionally analyzed the transcripts using inductive thematic analysis to ensure no themes outside of social cognitive theory were missed. Results. Twenty students were interviewed. Themes reveal perceptions that blended learning facilitated greater understanding of course material, increased motivation among learners, provided more flexibility in workload completion, and was a more enjoyable way to learn compared to traditional didactic instruction. Furthermore, blended learning offered additional distinct advantages over traditional and online-only pedagogies. Conclusion. Student pharmacists perceived blended and online learning positively and acceptable for the delivery of a pharmacy course on management, leadership, and economics over traditional didactic instruction. Blended learning may enhance innovation, leadership, management, and economics content delivery and the student learning experience.
Mass-loss rates for transiting exoplanets

Exoplanets at small orbital distances from their host stars are submitted to intense levels of energetic radiations, X-rays, and extreme ultraviolet (EUV). Depending on the masses and densities of the planets and on the atmospheric heating efficiencies, the stellar energetic inputs can lead to atmospheric mass loss. These evaporation processes are observable in the ultraviolet during planetary transits. The aim of the present work is to quantify the mass-loss rates ( u m), heating efficiencies (η), and lifetimes for the whole sample of transiting exoplanets, now including hot Jupiters, hot Neptunes, and hot super-Earths. The mass-loss rates and lifetimes are estimated from an “energy diagram” for exoplanets, which compares the planet gravitational potential energy to the stellar X/EUV energy deposited in the atmosphere. We estimate the mass-loss rates of all detected transiting planets to be within 10 6 to 10 13 gs −1 for various conservative assumptions. High heating efficiencies would imply that hot exoplanets such the gas giants WASP-12b and WASP-17b could be completely evaporated within 1 Gyr. We also show that the heating efficiency can be constrained when u m is inferred from observations and the stellar X/EUV luminosity is known. This leads us to suggest that η ≈ 100% in the atmosphere of the hot Jupiter HD 209458b, while it could be lower for HD 189733b. Simultaneous observations of transits in the ultraviolet and X-rays are necessary to further constrain the exospheric properties of exoplanets.
Weighted estimates for the discrete Laplacian on the cubic lattice

We consider the discrete Laplacian $\Delta$ on the cubic lattice $\mathbb Z^d$, and deduce estimates on the group $e^{it\Delta}$ and the resolvent $(\Delta-z)^{-1}$, weighted by $\ell^q(\mathbb Z^d)$-weights for suitable $q\geq 2$. We apply the obtained results to discrete Schr\"odinger operators in dimension $d\geq 3$ with potentials from $\ell^p(\mathbb Z^d)$ with suitable $p\geq 1$.
FULLY COUPLED SIMULATION OF COSMIC REIONIZATION. II. RECOMBINATIONS, CLUMPING FACTORS, AND THE PHOTON BUDGET FOR REIONIZATION

We use a fully coupled cosmological simulation including dark matter dynamics, multispecies hydrodynamics, nonequilibrium chemical ionization, flux-limited diffusion radiation transport, and a parameterized model of star formation and feedback (thermal and radiative) to investigate the epoch of hydrogen reionization in detail. In this paper, the first of several application papers, we investigate the mechanics of reionization from stellar sources forming in high-z galaxies, the utility of various formulations for the gas clumping factor on accurately estimating the effective recombination time in the intergalactic medium (IGM), and the photon budget required to achieve reionization. We also test the accuracy of the static and time-dependent models of Madau et al. as predictors of reionization completion/maintenance. We simulate a WMAP7 ΛCDM cosmological model in a 20 comoving Mpc cube, resolved with 8003 uniform fluid cells and dark matter particles. By tuning our star formation recipe to approximately match the observed high-redshift star formation rate density and galaxy luminosity function, we have created a fully coupled radiation hydrodynamical realization of hydrogen reionization, which begins to ionize at z ≈ 10 and is completed at z ≈ 5.8 without further tuning. We find that roughly two ionizing photons per H atom are required to convert the neutral IGM to a highly ionized state. After reionization concludes, we find that the quantity is ∼9 at z = 5, in rough agreement with measurements of the ionizing emissivity by Becker & Bolton. The complicated events during reionization that lead to this number can be generally described as inside-out, but in reality, the narrative depends on the level of ionization of the gas one attributes as being ionized. We find that the formula for the ionizing photon production rate needed to maintain the IGM in an ionized state derived by Madau et al. should not be used to predict the epoch of reionization completion because it ignores history-dependent terms in the global ionization balance which are not ignorable. We find that the time-dependent model for the ionized volume fraction QH ii is more predictive, but overestimates the redshift of reionization completion zreion by Δz ≈ 1. We propose a revised formulation of the time-dependent model that agrees with our simulation to a few percent accuracy. Finally, we use our simulation data to measure the absorption of ionizing radiation due to circumgalactic gas resolved on our mesh and find .
THE FAINT END OF THE LUMINOSITY FUNCTION AND LOW SURFACE BRIGHTNESS GALAXIES

Smithsonian Hectospec Lensing Survey (SHELS) is a dense redshift survey covering a 4 deg2 region to a limiting R = 20.6. In the construction of the galaxy catalog and in the acquisition of spectroscopic targets, we paid careful attention to the survey completeness for lower surface brightness dwarf galaxies. Thus, although the survey covers a small area, it is a robust basis for computation of the slope of the faint end of the galaxy luminosity function to a limiting MR = −13.3 + 5log h. We calculate the faint-end slope in the R band for the subset of SHELS galaxies with redshifts in the range 0.02 ⩽z < 0.1, SHELS0.1. This sample contains 532 galaxies with R < 20.6 and with a median surface brightness within the half-light radius of SB50, R = 21.82 mag arcsec−2. We used this sample to make one of the few direct measurements of the dependence of the faint end of the galaxy luminosity function on surface brightness. For the sample as a whole the faint-end slope, α = −1.31 ± 0.04, is consistent with both the Blanton et al. analysis of the Sloan Digital Sky Survey and the Liu et al. analysis of the COSMOS field. This consistency is impressive given the very different approaches of these three surveys. A magnitude-limited sample of 135 galaxies with optical spectroscopic redshifts with mean half-light surface brightness, SB50, R ⩾ 22.5 mag arcsec−2 is unique to SHELS0.1. The faint-end slope is α22.5 = −1.52 ± 0.16. SHELS0.1 shows that lower surface brightness objects dominate the faint-end slope of the luminosity function in the field, underscoring the importance of surface brightness limits in evaluating measurements of the faint-end slope and its evolution.
Lumbar Sympathetic Ganglion Block for Cancer-Associated Secondary Lower Limb Lymphedema: A Retrospective Study.

BACKGROUND Although lower limb lymphedema (LLL) is more or equally as frequent and harmful as upper limb lymphedema after cancer treatment, there are only a few studies on this topic. Cancer-related secondary LLL not only has physical implications, but also affects quality of life among patients who underwent gynecological cancer treatment. Despite numerous studies of various therapies, the optimal treatment for cancer-related LLL is still unknown. OBJECTIVES We aimed to investigate the efficacy of lumbar sympathetic ganglion block (LSGB) in patients with secondary LLL in the present study. STUDY DESIGN This study is a retrospective study. SETTING A single academic hospital, outpatient setting. METHODS A total of 30 patients with secondary unilateral LLL and failed complex decongestive treatment, from January 2017 through May 2021, were reviewed for inclusion in this study. The patients underwent fluoroscopy-guided LSGB 2 times with the help of digital subtraction angiography at 3-day intervals. Leg circumference was measured, and the volume of the leg was calculated before surgery, on the first day after the first surgery, on the first day after the second surgery, and on the seventh day after the second surgery. The World Health Organization Quality of Life Instrument Questionnaire scores were monitored before and after LSGB. RESULTS The leg circumference and volume decreased significantly from baseline after the treatment (P < 0.001). One week after 2 rounds of LSGB, the physical health score, psychological score, and social relationships score were higher than those before treatment (all P < 0.05). There was no difference in the environmental health score (P = 0.2731). LIMITATIONS This study was limited by its sample size and retrospective observational design. CONCLUSIONS LSGB can be a safe and effective treatment option for patients with secondary LLL after gynecological cancer treatment.
Invariance of deficiency indices of Hermitian subspaces under relatively bounded perturbations

This paper is concerned with the stability of deficiency indices of Hermitian subspaces (i.e., linear relations) under relatively bounded perturbations in Hilbert spaces. Several results about invariance of deficiency indices of Hermitian subspaces under relatively bounded perturbations are established. As a consequence, invariance of self-adjointness of Hermitian subspaces under relatively bounded perturbations is obtained. In addition, it is shown that the deficiency indices may shrink in the special case that the relative bound is equal to 1. The results obtained in the present paper generalize the corresponding results for symmetric operators to more general Hermitian subspaces.
Biderivations and commuting linear maps on Lie algebras

Let $L$ be a Lie algebra over a field of characteristic different from $2$. If $L$ is perfect and centerless, then every skew-symmetric biderivation $\delta:L\times L\to L$ is of the form $\delta(x,y)=\gamma([x,y])$ for all $x,y\in L$, where $\gamma\in{\rm Cent}(L)$, the centroid of $L$. Under a milder assumption that $[c,[L,L]]=\{0\}$ implies $c=0$, every commuting linear map from $L$ to $L$ lies in ${\rm Cent}(L)$. These two results are special cases of our main theorems which concern biderivations and commuting linear maps having their ranges in an $L$-module. We provide a variety of examples, some of them showing the necessity of our assumptions and some of them showing that our results cover several results from the literature.
AN UNBIASED METHOD OF MODELING THE LOCAL PECULIAR VELOCITY FIELD WITH TYPE Ia SUPERNOVAE

We apply statistically rigorous methods of nonparametric risk estimation to the problem of inferring the local peculiar velocity field from nearby Type Ia supernovae (SNIa). We use two nonparametric methods—weighted least squares (WLS) and coefficient unbiased (CU)—both of which employ spherical harmonics to model the field and use the estimated risk to determine at which multipole to truncate the series. We show that if the data are not drawn from a uniform distribution or if there is power beyond the maximum multipole in the regression, a bias is introduced on the coefficients using WLS. CU estimates the coefficients without this bias by including the sampling density making the coefficients more accurate but not necessarily modeling the velocity field more accurately. After applying nonparametric risk estimation to SNIa data, we find that there are not enough data at this time to measure power beyond the dipole. The WLS Local Group bulk flow is moving at 538 ± 86 km s−1 toward (l, b) = (258° ± 10°, 36° ± 11°) and the CU bulk flow is moving at 446 ± 101 km s−1 toward (l, b) = (273° ± 11°, 46° ± 8°). We find that the magnitude and direction of these measurements are in agreement with each other and previous results in the literature.
KINEMATICS OF THE STELLAR HALO AND THE MASS DISTRIBUTION OF THE MILKY WAY USING BLUE HORIZONTAL BRANCH STARS

Here, we present a kinematic study of the Galactic halo out to a radius of ∼60 kpc, using 4664 blue horizontal branch stars selected from the SDSS/SEGUE survey to determine key dynamical properties. Using a maximum likelihood analysis, we determine the velocity dispersion profiles in spherical coordinates (σr, σθ, σϕ) and the anisotropy profile (β). The radial velocity dispersion profile (σr) is measured out to a galactocentric radius of r ∼ 60 kpc, but due to the lack of proper-motion information, σθ, σϕ, and β could only be derived directly out to r ∼ 25 kpc. From a starting value of β ≈ 0.5 in the inner parts (9 < r/kpc < 12), the profile falls sharply in the range r ≈ 13–18 kpc, with a minimum value of β = −1.2 at r = 17 kpc, rising sharply at larger radius. In the outer parts, in the range 25 < r/kpc < 56, we predict the profile to be roughly constant with a value of β ≈ 0.5. The newly discovered kinematic anomalies are shown not to arise from halo substructures. We also studied the anisotropy profile of simulated stellar halos formed purely by accretion and found that they cannot reproduce the sharp dip seen in the data. From the Jeans equation, we compute the stellar rotation curve (vcirc) of the Galaxy out to r ∼ 25 kpc. The mass of the Galaxy within r ≲ 25 kpc is determined to be 2.1 × 1011 M☉, and with a three-component fit to vcirc(r), we determine the virial mass of the Milky Way dark matter halo to be Mvir = 0.9+0.4−0.3 × 1012 M☉ (Rvir = 249+34−31 kpc).
A CO LINE AND INFRARED CONTINUUM STUDY OF THE ACTIVE STAR-FORMING COMPLEX W51

We present the results of an extensive observational study of the active star-forming complex W51 that was observed in the J = 2 − 1 transition of the 12CO and 13CO molecules over a 1. °25 × 1. °00 region with the University of Arizona Heinrich Hertz Submillimeter Telescope. We use a statistical equilibrium code to estimate physical properties of the molecular gas. We compare the molecular cloud morphology with the distribution of infrared (IR) and radio continuum sources and find associations between molecular clouds and young stellar objects (YSOs) listed in Spitzer IR catalogs. The ratios of CO lines associated with H ii regions are different from the ratios outside the active star-forming regions. We present evidence of star formation triggered by the expansion of the H ii regions and by cloud–cloud collisions. We estimate that about 1% of the cloud mass is currently in YSOs.
H i CONTENT AND OPTICAL PROPERTIES OF FIELD GALAXIES FROM THE ALFALFA SURVEY. II. MULTIVARIATE ANALYSIS OF A GALAXY SAMPLE IN LOW-DENSITY ENVIRONMENTS

This is the second paper of two reporting results from a study of the H i content and stellar properties of nearby galaxies detected by the Arecibo Legacy Fast ALFA blind 21 cm line survey and the Sloan Digital Sky Survey in a 2160 deg2 region of high galactic latitude sky covered by both surveys, in the general Virgo direction. Here, we analyze a complete H i flux-limited subset of 1624 objects with homogeneously measured 21 cm and multi-wavelength optical attributes extracted from the control sample of H i emitters in environments of low local galactic density assembled by Toribio et al. (Paper I). Strategies of multivariate data analysis are applied to this data set in order to (i) investigate the correlation structure of the space defined by an extensive set of potentially independent observables describing gas-rich systems, (ii) identify the intrinsic parameters that best define their neutral gas content, and (iii) explore the scaling relations arising from the joint distributions of the quantities most strongly correlated with the H i mass. The principal component analysis performed over a set of five galaxy properties reveals that they are strongly interrelated, supporting previous claims that nearby H i emitters show a high degree of correlation. The best predictors for the expected value of MH i are the diameter of the stellar disk, D25,r, followed by the total luminosity (both in the r band), and the maximum rotation speed, while morphological proxies such as color show only a moderately strong correlation with the gaseous content attenuated by observational error. Among the various inferred prescriptions, the simplest and most accurate is log(MH i/M☉) = 8.72 + 1.25 log(D25,r/kpc). We find a slope of −8.2 ± 0.5 for the relation between optical magnitude and log rotation speed, in good agreement with Tully–Fisher studies, as well as a log slope of 1.55 ± 0.06 for the H i mass–optical galaxy size relation. Given the homogeneity of the measurements and the completeness of our data set, the latter outcome suggests that the constancy of the average (hybrid) H i surface density advocated by some authors for the spiral population is just a crude approximation.
On isotropic cloaking and interior transmission eigenvalue problems

This paper is concerned with the invisibility cloaking in acoustic wave scattering from a new perspective. We are especially interested in achieving the invisibility cloaking by completely regular and isotropic mediums. It is shown that an interior transmission eigenvalue problem arises in our study, which is the one considered theoretically in Cakoni et al. (Transmission eigenvalues for inhomogeneous media containing obstacles, Inverse Problems and Imaging, 6 (2012), 373–398). Based on such an observation, we propose a cloaking scheme that takes a three-layer structure including a cloaked region, a lossy layer and a cloaking shell. The target medium in the cloaked region can be arbitrary but regular, whereas the mediums in the lossy layer and the cloaking shell are both regular and isotropic. We establish that if a certain non-transparency condition is satisfied, then there exists an infinite set of incident waves such that the cloaking device is nearly invisible under the corresponding wave interrogation. The set of waves is generated from the Herglotz approximation of the associated interior transmission eigenfunctions. We provide both theoretical and numerical justifications.