Miracle-dz/UniFAR-FTUs huggingface dataset:
The Bárány Society position on ‘Cervical Dizziness’

This paper describes the Bárány Society Classification OverSight Committee (COSC) position on Cervical Dizziness, sometimes referred to as Cervical Vertigo. This involved an initial review by a group of experts across a broad range of fields, and then subsequent review by the Bárány Society COSC. Based upon the so far published literature, the Bárány Society COSC takes the view that the evidence supporting a mechanistic link between an illusory sensation of self-motion (i.e. vertigo – spinning or otherwise) and neck pathology and/or symptoms of neck pain - either by affecting the cervical vertebrae, soft tissue structures or cervical nerve roots - is lacking. When a combined head and neck movement triggers an illusory sensation of spinning, there is either an underlying common vestibular condition such as migraine or BPPV or less commonly a central vestibular condition including, when acute in onset, dangerous conditions (e.g. a dissection of the vertebral artery with posterior circulation stroke and, exceedingly rarely, a vertebral artery compression syndrome). The Committee notes, that migraine, including vestibular migraine, is by far, the commonest cause for the combination of neck pain and vestibular symptoms. The committee also notes that since head movement aggravates symptoms in almost any vestibular condition, the common finding of increased neck muscle tension in vestibular patients, may be linked as both cause and effect, to reduced head movements. Additionally, there are theoretical mechanisms, which have not been explored, whereby cervical pain may promote vaso-vagal, cardio-inhibitory reflexes and hence by presyncopal mechanisms, elicit transient disorientation and/or imbalance. The committee accepts that further research is required to answer the question as to whether those rare cases in which neck muscle spasm is associated with a vague sense of spatial disorientation and/or imbalance, is indeed linked to impaired neck proprioception. Future studies should ideally be placebo controlled and double-blinded where possible, with strict inclusion and exclusion criteria that aim for high specificity at the cost of sensitivity. To facilitate further studies in “cervical dizziness/vertigo”, we provide a narrative view of the important confounds investigators should consider when designing controlled mechanistic and therapeutic studies. Hence, currently, the Bárány COSC refrains from proposing any preliminary diagnostic criteria for clinical use outside a research study. This position may change as new research evidence is provided.
Application of top-down holographic thermal QCD at finite coupling

Using the UV-complete top-down type IIB holographic dual of large-$N$ thermal QCD as constructed in arXiv:hep-th/0902.1540, in arXiv:1507.02692[hep-th], the type IIB background of arXiv:hep-th/0902.1540 was shown to be thermodynamically stable. We also showed that the temperature dependence of DC electrical conductivity mimics a one-dimensional Luttinger liquid, and the requirement of the Einstein relation to be satisfied requires a specific dependence of the Ouyang embedding parameter on the horizon radius. In arXiv:1606.04949[hep-th], we obtained the speed of sound, the shear mode diffusion constant and the shear viscosity $\eta$ (and $\frac{\eta}{s}$) upto (N)ext to (L)eading (O)rder in $N$ by looking at the scalar, vector and tensor modes of metric perturbations and solve Einstein's equation involving appropriate gauge-invariant combination of perturbations as constructed in arXiv:hep-th/0506184. Another interesting result for the temperature dependence of the thermal (and electrical) conductivity and the consequent deviation from the Wiedemann-Franz law, upon comparison with arXiv:0903.3054[cond-mat], was obtained at leading order in $N$. The results for the above qualitatively mimic a 1+1-dimensional Luttinger liquid with impurities. Also we obtained the QCD deconfinement temperature compatible with lattice results. On the holographic phenomenology side, in arXiv:1703.01306 [hep-th], we computed the masses of the $0^{++}, 0^{-+},0^{--}, 1^{++}, 2^{++}$ `glueball' states in the same aforementioned backgrounds. All these calculations were done both for a thermal background with an IR cut-off $r_0$ and a black hole background with horizon radius $r_h$. We used WKB quantization conditions on one hand and imposed Neumann/Dirichlet boundary conditions at $r_0$/$r_h$ on the solutions to the equations of motion on the other.
Why current-carrying magnetic flux tubes gobble up plasma and become thin as a result

Suppose an electric current I flows along a magnetic flux tube that has poloidal flux psi and radius a = a(z), where z is the axial position along the flux tube. This current creates a toroidal magnetic field Bphi. It is shown that, in such a case, nonlinear, nonconservative J×B forces accelerate plasma axially from regions of small a to regions of large a and that this acceleration is proportional to [partial-derivative]I2/[partial-derivative]z. Thus, if a current-carrying flux tube is bulged at, say, z = 0 and constricted at, say, z = ±h, then plasma will be accelerated from z = ±h towards z = 0 resulting in a situation similar to two water jets pointed at each other. The ingested plasma convects embedded, frozen-in toroidal magnetic flux from z = ±h to z = 0. The counterdirected flows collide and stagnate at z = 0 and in so doing (i) convert their translational kinetic energy into heat, (ii) increase the plasma density at z[approximate]0, and (iii) increase the embedded toroidal flux density at z[approximate]0. The increase in toroidal flux density at z[approximate]0 increases Bphi and hence increases the magnetic pinch force at z[approximate]0 and so causes a reduction of a(0). Thus, the flux tube develops an axially uniform cross section, a decreased volume, an increased density, and an increased temperature. This model is proposed as a likely hypothesis for the long-standing mystery of why solar coronal loops are observed to be axially uniform, hot, and bright. It is furthermore argued that a small number of tail particles bouncing between the approaching counterstreaming plasma jets should be Fermi accelerated to extreme energies. Finally, analytic solution of the Grad–Shafranov equation predicts that a flux tube becomes axially uniform when the ingested plasma becomes hot and dense enough to have 2µ0nkappaT/B pol 2 = (µ0Ia(0)/psi)2/2; observed coronal loop parameters are in reasonable agreement with this relationship which is analogous to having betapol = 1 in a tokamak.
Color-selected Galaxies at z ≈ 6 in the Great Observatories Origins Deep Survey

We report early results on galaxies at z ~ 6 selected from Hubble Space Telescope imaging for the Great Observatories Origins Deep Survey. Spectroscopy of one object with the Advanced Camera for Surveys grism and from the Keck and Very Large Telescope observatories shows a strong continuum break and asymmetric line emission, identified as Lyα at z = 5.83. We find only five spatially extended candidates with signal-to-noise ratios greater than 10, two of which have spectroscopic confirmation. This is much fewer than would be expected if galaxies at z = 6 had the same luminosity function as those at z = 3. There are many fainter candidates, but we expect substantial contamination from foreground interlopers and spurious detections. Our best estimates favor a z = 6 galaxy population with fainter luminosities, higher space density, and similar comoving ultraviolet emissivity to that at z = 3, but this depends critically on counts at fluxes fainter than those reliably probed by the current data.
Relations between photoionization cross sections and photon radius

The relations between photoionization cross sections and photon radius are obtained on basis of quantum mechanics and the particle-like properties of a photon. The photoionization cross sections of H atom and H-like ions, He atom and He like ions, alkali metal atoms, and Rydberg atoms are calculated using the relations. The calculation results are found to be good agreement with the known experimental data. The results show that the photoionization cross section is always smaller than the cross section of the photon to ionize the atom or ion and can be expressed as the product of the cross section of the photon and the probability that electron meets with the photon. These provide the intuitive understanding for the photoionization phenomena and open a new avenue of research on interaction between a photon and an atom or ion.
Surface and bulk effects of K in highly efficient Cu$_{1-x}$K$_x$InSe$_2$ solar cells

To advance knowledge of K bonding in Cu(In,Ga)(Se,S)2 (CIGS) photovoltaic (PV) absorbers, recent Cu-K-In-Se phase growth studies have been extended to PV performance. First, the effect of distributing K throughout bulk Cu1-xKxInSe2 absorbers at low K/(K+Cu) compositions (0 <= x <= 0.30) was studied. Efficiency, open-circuit voltage (VOC), and fill factor (FF) were greatly enhanced for x ~ 0.07, resulting in an officially-measured 15.0%-efficient solar cell, matching to the world record CuInSe2 efficiency. The improvements were a result of reduced interface and bulk recombination, relative to CuInSe2 (x ~ 0). However, higher x compositions had reduced efficiency, short-circuit current density (JSC), and FF due to greatly increased interface recombination, relative to the x ~ 0 baseline. Next, the effect of confining K at the absorber/buffer interface at high K/(K+Cu) compositions (0.30 <= x <= 0.92) was researched. Previous work showed that these surface layer growth conditions produced CuInSe2 with a large phase fraction of KInSe2. After optimization (75 nm surface layer with x ~ 0.41), these KInSe2 surface samples exhibited increased efficiency (officially 14.9%), VOC, and FF as a result of decreased interface recombination. The KInSe2 surfaces had features similar to previous reports for KF post-deposition treatments (PDTs) used in world record CIGS solar cells-taken as indirect evidence that KInSe2 can form during these PDTs. Both the bulk and surface growth processes greatly reduced interface recombination. However, the KInSe2 surface had higher K levels near the surface, greater lifetimes, and increased inversion near the buffer interface, relative to the champion bulk CKIS absorber. These characteristics demonstrate that K may benefit PV performance by different mechanisms at the surface and in the absorber bulk.
A REMARKABLE NEW GYNODIOECIOUS SPECIES OF OCOTEA (LAURACEAE) FROM THE BRAZILIAN ATLANTIC RAIN FOREST, AND ITS PHYLOGENETIC PLACEMENT IN THE OCOTEA COMPLEX

Ocotea bilocellata Baitello, D.B. O.S. Cardoso & P.L. R.Moraes, a species of Lauraceae that is new to science and from the Atlantic rain forest of the state of São Paulo, Brazil, is described and illustrated. The newly described species does not fit in any of the traditionally circumscribed disporangiate Lauraceae genera; rather, we show that it is phylogenetically placed within the Ocotea minarum group, as revealed by nuclear ribosomal ITS and plastid psbA–trnH sequence data.
Too hot to handle? Analytic solutions for massive neutrino or warm dark matter cosmologies

Author(s): Slepian, Z; Portillo, SKN | Abstract: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. We obtain novel closed-form solutions to the Friedmann equation for cosmological models containing a component whose equation of state is that of radiation (w =1/3) at early times and that of cold pressureless matter (w=0) at late times. The equation of state smoothly transitions from the early- to late-time behaviour and exactly describes the evolution of a species with a Dirac delta function distribution inmomentum magnitudes | p0| (i.e. all particles have the same | p0|). Such a component, here termed 'hot matter', is an approximate model for both neutrinos and warm dark matter. We consider it alone and in combination with cold matter and with radiation, also obtaining closed-form solutions for the growth of superhorizon perturbations in each case. The idealized model recovers t(a) to better than 1.5 per cent accuracy for all a relative to a Fermi-Dirac distribution (as describes neutrinos). We conclude by adding the second moment of the distribution to our exact solution and then generalizing to include all moments of an arbitrary momentum distribution in a closed-form solution.
Multisensory Teaching-Learning Approach in Reading for Pupils at Risk of Dropping Out (PARDO)

The multisensory approach refers to any learning activity that combines two or more sensory strategies to take in or express information, and these have been particularly valuable in literacy and language learning. This study utilized a multisensory approach to reading to motivate visual, auditory, tactile, and kinesthetic (VAK) learners and assess the five-month reading intervention program for the pupils who are at risk of dropping out. It used documentary analysis, oral diagnostic tests for the Grade I Pupils At Risk of Dropping-Out (PARDO). Such was conducted on a one-on-one basis to assess the reading skills of the pupils, and the results were subjected to a t-test. The normative-descriptive method was employing a self-made questionnaire to gather information regarding the facilitators’ profile and their perceptions regarding the program. There was a significant leap in the performance of the subjects between the pretest and posttest. A significant improvement was observed in the performance of the pupils in the posttest. The program is very helpful to young learners; it encourages them in continuing their studies, especially those who are considered slow learners.
Ioffe-Regel criterion for Anderson localization in the model of resonant point scatterers

We establish a phase diagram of a model in which scalar waves are scattered by resonant point scatterers (atoms) pinned at random positions in the free three-dimensional (3D) space. A transition to Anderson localization takes place in a narrow frequency band near the resonance frequency provided that the number density of scatterers $\rho$ exceeds a critical value $\rho_c \simeq 0.08 k_0^{3}$, where $k_0$ is the wave number in the free space. The localization condition $\rho > \rho_c$ can be rewritten as $k_0 \ell_0 < 1$, where $\ell_0$ is the on-resonance mean free path in the independent-scattering approximation. At mobility edges, the decay of the average amplitude of a monochromatic plane wave is not purely exponential and the growth of its phase is nonlinear with the propagation distance. This makes it impossible to define the mean free path $\ell$ and the effective wave number $k$ in a usual way. If the latter are defined as an effective decay length of the intensity and an effective growth rate of the phase of the average wave field, the Ioffe-Regel parameter $(k\ell)_c$ at the mobility edges can be calculated and takes values from 0.4 to 1.1 depending on $\rho$. Thus, the Ioffe-Regel criterion of localization $k\ell < (k\ell)_c = \mathrm{const} \sim 1$ is valid only qualitatively and cannot be used as a quantitative condition of Anderson localization in 3D.
Direct probe of dark energy through gravitational lensing effect

We show that gravitational lensing can provide a direct method to probe the nature of dark energy at astrophysical scales. For lensing system as an isolated astrophysical object, we derive the dark energy contribution to gravitational potential as a repulsive power-law term, containing a generic equation of state parameter w. We find that it generates w-dependent and position-dependent modification to the conventional light orbital equation of w=−1. With post-Newtonian approximation, we compute its direct effect for an isolated lensing system at astrophysical scales and find that the dark energy force can deflect the path of incident light rays. We demonstrate that the dark-energy-induced deflection angle ΔαDE∝ M(1+1/3w) (with 1+1/3w > 0), which increases with the lensing mass M and consistently approaches zero in the limit M→ 0. This effect is distinctive because dark energy tends to diffuse the rays and generates concave lensing effect. This is in contrast to the conventional convex lensing effect caused by both visible and dark matter. Measuring such concave lensing effect can directly probe the existence and nature of dark energy. We estimate this effect and show that the current gravitational lensing experiments are sensitive to the direct probe of dark energy at astrophysical scales. For the special case w=−1, our independent study favors the previous works that the cosmological constant can affect light bending, but our prediction qualitatively and quantitatively differ from the literature, including our consistent realization of ΔαDE → 0 (under 0M→ ) at the leading order.
Identifying mental illness and monitoring mental health in probation service settings

There is a need to improve a) identification and monitoring of people with mental illness on probation and b) understanding of the impact of interventions on mental health outcomes for the probation population. If data were routinely collected using validated screening tools and shared between agencies, this could inform practice and commissioning decisions, and ultimately it could improve health outcomes for people under supervision. The literature was reviewed to identify brief screening tools and outcome measures that have been used in prevalence and outcome studies conducted with adults on probation in Europe. This paper shares findings from the UK-based studies in which 20 brief screening tools and measures were identified. Recommendations are made based on this literature regarding suitable tools for use in probation to routinely identify a need for contact with mental health and/or substance misuse services and to measure change in mental health outcomes.
Stellar density distribution along the minor axis of the Large Magellanic Cloud

We studied the spatial distribution of young and old stellar populations along the western half part of the minor axis of the Large Magellanic Cloud (LMC) using Washington MT1 photometry of selected fields, which span a deprojected distance range from the LMC bar centre out to ~ 31.6 kpc. We found that both stellar populations share a mean LMC limiting radius of 8.9+-0.4 kpc; old populations are three times more dense that young populations at that LMC limit. When comparing this result with recent values for the LMC extension due to north, the old populations resulted significantly more elongated than the young ones. Bearing in mind previous claims that the elongation of the outermost LMC regions may be due to the tidal effects of the Milky Way (MW), our findings suggest that such a tidal interaction should not have taken place recently. The existence of young populations in the outermost western regions also supports previous results about ram pressure stripping effects of the LMC gaseous disc due to the motion of the LMC in the MW halo.
The Detection of Crystalline Silicates in Ultraluminous Infrared Galaxies

Silicates are an important component of interstellar dust, and the structure of these grains (amorphous or crystalline) is sensitive to the local physical conditions. We have studied the infrared spectra of a sample of ultraluminous infrared galaxies (ULIRGs). Here we report the discovery of weak, narrow absorption features at 11, 16, 19, 23, and 28 μm, characteristic of crystalline silicates, superimposed on the broad absorption bands at 10 and 18 μm due to amorphous silicates in a subset of this sample. These features betray the presence of forsterite (Mg2SiO4), the magnesium-rich end member of the olivines. Previously, crystalline silicates have only been observed in circumstellar environments. The derived fraction of forsterite to amorphous silicates is typically 0.1 in these ULIRGs. This is much larger than the upper limit for this ratio in the interstellar medium of the Milky Way, 0.01. These results suggest that the timescale for injection of crystalline silicates into the ISM is short in a merger-driven starburst environment (e.g., as compared to the total time to dissipate the gas), pointing toward massive stars as a prominent source of crystalline silicates. Furthermore, amorphization due to cosmic rays, which is thought to be of prime importance for the local ISM, lags in vigorous starburst environments.
Gemini and Lowell observations of 67P/Churyumov−Gerasimenko during the Rosetta mission

We present observations of comet 67P/Churyumov−Gerasimenko acquired in support of the Rosetta mission. We obtained usable data on 68 nights from 2014 September until 2016 May, with data acquired regularly whenever the comet was observable. We collected an extensive set of near-IR J, H and Ks data throughout the apparition plus visible-light images in g', r', i' and z' when the comet was fainter. We also obtained broad-band R and narrow-band CN filter observations when the comet was brightest using telescopes at Lowell Observatory. The appearance was dominated by a central condensation and the tail until 2015 June. From 2015 August onwards, there were clear asymmetries in the coma, which enhancements revealed to be due to the presence of up to three features (i.e. jets). The features were similar in all broad-band filters; CN images did not show these features but were instead broadly enhanced in the southeastern hemisphere. Modelling using the parameters from Vincent et al. replicated the dust morphology reasonably well, indicating that the pole orientation and locations of active areas have been relatively unchanged over at least the last three apparitions. The dust production, as measured by A(0°)fρ peaked ∼30 d after perihelion and was consistent with predictions from previous apparitions. A(0°)fρ as a function of heliocentric distance was well fitted by a power law with slope −4.2 from 35 to 120 d post-perihelion. We detected photometric evidence of apparent outbursts on 2015 August 22 and 2015 September 19, although neither was discernible morphologically in this data set.
Molecular Gas Contents and Scaling Relations for Massive, Passive Galaxies at Intermediate Redshifts from the LEGA-C Survey

A decade of study has established that the molecular gas properties of star-forming galaxies follow coherent scaling relations out to z ∼ 3, suggesting remarkable regularity of the interplay between molecular gas, star formation, and stellar growth. Passive galaxies, however, are expected to be gas-poor and therefore faint, and thus little is known about molecular gas in passive galaxies beyond the local universe. Here we present deep Atacama Large Millimeter/submillimeter Array observations of CO(2–1) emission in eight massive (Mstar ∼ 1011 M⊙) galaxies at z ∼ 0.7 selected to lie a factor of 3–10 below the star-forming sequence at this redshift, drawn from the Large Early Galaxy Astrophysics Census survey. We significantly detect half the sample, finding molecular gas fractions ≲0.1. We show that the molecular and stellar rotational axes are broadly consistent, arguing that the molecular gas was not accreted after the galaxies became quiescent. We find that scaling relations extrapolated from the star-forming population overpredict both the gas fraction and gas depletion time for passive objects, suggesting the existence of either a break or large increase in scatter in these relations at low specific star formation rate. Finally, we show that the gas fractions of the passive galaxies we have observed at intermediate redshifts are naturally consistent with evolution into local, massive early-type galaxies by continued low-level star formation, with no need for further gas accretion or dynamical stabilization of the gas reservoirs in the intervening 6 billion years.