Miracle-dz/UniFAR-FTUs huggingface dataset:
‘You can’t walk through water without getting wet’ UK nurses’ distress and psychological health needs during the Covid-19 pandemic: A longitudinal interview study the Impact of Covid On Nurses (ICON) Survey Research Group

s Background: Pre-COVID-19 research highlighted the nursing profession worldwide as being at high risk from symptoms of burnout, post-traumatic stress disorder (PTSD) and suicide. The World Health Organization declared a pandemic on 11th March 2020 due to the sustained risk of further global spread of COVID-19. The high healthcare burden associated with COVID-19 has increased nurses’ trauma and workload, thereby exacerbating pressure on an already strained workforce and causing additional psychological distress for staff. Objectives: The Impact of COVID-19 on Nurses (ICON) interview study examined the impacts of the pan- demic on frontline nursing staff’s psychosocial and emotional wellbeing. Design: Longitudinal qualitative interview study. Settings: Nurses who had completed time 1 and 2 of the ICON survey were sampled to include a range of UK work settings including acute, primary and community care and care homes. Interviewees were purposively sampled for maximum variation to cover a broad range of personal and professional factors, and experiences during the COVID-19 pandemic, including redeployment. Methods: Nurses participated in qualitative in-depth narrative interviews after the ﬁrst wave of COVID-19 in July 2020 ( n = 27) and again at the beginning of the second wave in December 2020 ( n = 25) via video and audio platform software. Rigorous qualitative narrative analysis was undertaken both cross-sectionally (within wave) and longitudinally (cross wave) to explore issues of consistency and change. Results: The terms moral distress, compassion fatigue, burnout and PTSD describe the emotional states reported by the majority of interviewees leading many to consider leaving the profession. Causes of this identiﬁed included care delivery challenges; insuﬃcient staff and training; PPE challenges and frustrations. Four themes were identiﬁed: (1) ‘Deathscapes’ and impoverished care (2) Systemic challenges and self-preservation (3) Emotional exhaustion and (4) (Un)helpful support. Conclusions: Nurses have been deeply affected by what they have experienced and report being forever altered with the impacts of COVID-19 persisting and deeply felt. There is an urgent need to tackle stigma to create a psychologically safe working environment and for a national COVID-19 nursing workforce recovery strategy to help restore nurse’s well-being and demonstrate a valuing of the nursing workforce and therefore support retention.
Utilizing Astrometric Orbits to Obtain Coronagraphic Images of Extrasolar Planets

We present an approach for utilizing astrometric orbit information to improve the yield of planetary images and spectra from a follow-on direct-detection mission. This approach is based on the notion—strictly hypothetical—that if a particular star could be observed continuously, the instrument would in time observe all portions of the habitable zone so that no planet residing therein could be missed. This strategy could not be implemented in any realistic mission scenario. But if an exoplanet’s orbit is known from astrometric observation, then it may be possible to plan and schedule a sequence of imaging observations that is the equivalent of continuous observation. A series of images—optimally spaced in time—could be recorded to examine contiguous segments of the orbit. In time, all segments would be examined, leading to the inevitable detection of the planet. In this article, we show how astrometric orbit information can be used to construct such a sequence. We apply this methodology to seven stars taken from the target lists of proposed astrometric and direct-detection missions. In addition, we construct this sequence for the Sun-Earth system as it would appear from a distance of 10 pc. In constructing these sequences, we have assumed that the imaging instrument has an inner working angle (IWA) of 75 mas and that the planets are visible whenever they are separated from their host stars by ≥IWA and are in quarter-phase or greater. In addition, we have assumed that the planets orbit at a distance of 1 AU scaled to luminosity and that the inclination of the orbit plane is 60°. For the individual stars in this target pool, we find that the number of observations in this sequence ranges from two to seven, representing the maximum number of observations required to find the planet. The probable number of observations ranges from 1.5 to 3.1. These results suggest that a direct-detection mission using astrometric orbits would find all eight exoplanets in this target pool with a probability of unity and that the maximum number of visits required (i.e., the worst case) is 36 visits. The probable number of visits is considerably smaller, about 18. This is a dramatic improvement in efficiency over previous methods proposed for utilizing astrometric orbits. We examine how the implementation of this approach is complicated and limited by operational constraints and how it is impacted by formal errors. We find that it can be fully implemented for internal coronagraph and visual nuller missions, with a success rate approaching 100%. External occulter missions will also benefit, but to a lesser degree.
Influence of external fields and environment on the dynamics of a phase-qubit-resonator system

We analyze the dynamics of a qubit-resonator system coupled with a thermal bath and external electromagnetic fields. Using the evolution equations for the set of Heisenberg operators that describe the whole system, we derive an expression for the resonator field, accounting for the resonator-drive, -bath, and -qubit interaction. The renormalization of the resonator frequency caused by the qubit-resonator interaction is accounted for. Using solutions for the resonator field, we derive the equation describing qubit dynamics. The influence of the qubit evolution during measurement time on the fidelity of a single-shot measurement is studied. The relation between fidelity and measurement time is shown explicitly. Also, an expression describing relaxation of the superposition qubit state toward its stationary value is derived. The possibility of controlling this state by varying the amplitude and frequency of drive is shown.
Induction of tolerance with salicylic acid in sour passion fruit irrigated with water of different cationic compositions

This study aimed to evaluate the physiological indices, growth, and seedling quality of the sour passion fruit cv. BRS SC1 as a function of irrigation with water of different cationic natures and exogenous application of salicylic acid. The experiment was conducted under plant nursery conditions at the CCTA/UFCG, Campus Pombal-PB, using a randomized block design set up in a 6 × 4 factorial arrangement referring to six cationic compositions of irrigation water (S 1 – control, S 2 - Na + , S 3 - Ca 2+ , S 4 - Na + + Ca 2+ , S 5 - Mg 2+ , and S 6 - Na + + Ca 2+ + Mg 2+ ) and four concentrations of salicylic acid - SA (0, 1.0, 2.0, and 3.0 mM), with three replications and two plants per plot. In the control treatment (S 1 ), the plants were irrigated with the electrical conductivity level of 0.3 dS m -1 , whereas the other treatments (S 2 , S 3 , S 4 , S 5, and S 6 ) used water with 4.0 dS m -1 obtained based on different cations, all in the form of chloride. The exogenous application of salicylic acid increased the content of chlorophyll b in the sour passion fruit seedlings. Salt stress negatively affected seedling growth. Seedling quality was affected by the electrical conductivity of irrigation water regardless of the cationic nature. Although showing reductions, the seedlings produced under high salinity showed a satisfactory Dickson quality index. The genotype cv. BRS SC1 is considered tolerant to salinity when irrigated with water salinized by Na + , Ca 2+ , Na + + Ca 2+ , and Na + + Ca 2+ + Mg 2+ , and moderately tolerant when irrigated with water salinized by Mg 2+ .
Chiral condensate from renormalization group optimized perturbation

Our recently developed variant of variationnally optimized perturbation (OPT), in particular consistently incorporating renormalization group properties (RGOPT), is adapted to the calculation of the QCD spectral density of the Dirac operator and the related chiral quark condensate $\langle \bar q q \rangle$ in the chiral limit, for $n_f=2$ and $n_f=3$ massless quarks. The results of successive sequences of approximations at two-, three-, and four-loop orders of this modified perturbation, exhibit a remarkable stability. We obtain $\langle \bar q q\rangle^{1/3}_{n_f=2}(2\, {\rm GeV}) = -(0.833-0.845) \bar\Lambda_2 $, and $ \langle\bar q q\rangle^{1/3}_{n_f=3}(2\, {\rm GeV}) = -(0.814-0.838) \bar\Lambda_3 $ where the range spanned by the first and second numbers (respectively four- and three-loop order results) defines our theoretical error, and $\bar\Lambda_{n_f}$ is the basic QCD scale in the $\overline{MS}$-scheme. We obtain a moderate suppression of the chiral condensate when going from $n_f=2$ to $n_f=3$. We compare these results with some other recent determinations from other nonperturbative methods (mainly lattice and spectral sum rules).
Structure of neutron-scattering peaks in both s++ -wave and s± -wave states of an iron pnictide superconductor

We study the neutron-scattering spectrum in iron pnictides based on the random-phase approximation in the five-orbital model for fully gapped $s$-wave states with sign reversal $({s}_{\ifmmode\pm\else\textpm\fi{}})$ and without sign reversal $({s}_{++})$. In the ${s}_{++}$-wave state, we find that a prominent hump structure appears just above the spectral gap by taking account of the quasiparticle damping $\ensuremath{\gamma}$ due to strong electron-electron correlation: as the superconductivity develops, the reduction in $\ensuremath{\gamma}$ gives rise to the large overshoot in the spectrum above the gap. The obtained hump structure looks similar to the resonance peak in the ${s}_{\ifmmode\pm\else\textpm\fi{}}$-wave state, although the height and weight of the peak in the latter state is much larger. In the present study, experimentally observed broad spectral peak in iron pnictides is naturally reproduced by assuming the ${s}_{++}$-wave state.
The Carbon Cycle as the Main Determinant of Glacial-Interglacial Transitions

An intriguing problem in climate science is the existence of Earth's glacial cycles. We show that it is possible to generate these periodic changes in climate by means of the Earth's carbon cycle as the main determinant factor. The carbon exchange between the Ocean, the Continent and the Atmosphere is modeled by means of a tridimensional Lotka-Volterra system and the resulting atmospheric carbon cycle is used as the unique radiative forcing mechanism. It is shown that the carbon dioxide (CO$_{2}$) and temperature anomaly curves, which are thus obtained, have the same first-order structure as the 100 kyr glacial--interglacial cycles depicted by the Vostok ice core data, reproducing the asymmetries of rapid heating--slow cooling, and short interglacial--long glacial ages.
The Public Option and Optimal Redistribution∗

I develop a model of redistribution with a public option to study how and when to optimally do so. The allocations of the public option and private goods are determined in equilibrium. Consequently, while the public option directly benefits individuals who consume it, it might also indirectly affect others due to its effect on private good prices. I characterize incentive constraints to determine whom the public option directly benefits. I derive the optimal mechanism for allocating the public option and show how the trade-off between its direct and indirect effects provides a novel justification for rationing. Finally, I incorporate externalities, imperfect competition, and additional policy instruments. JEL classification: C61, D47, D61, D63, D82
The CGF dark matter ﬂuid

The cosmological gauge ﬁeld (CGF) is a classical solution of SU(2)-weak gauge theory oscillating rapidly in time. It is the dark matter driving the CGF cosmology. A general, local, mathematically natural construction of the CGF is given here. The macroscopic properties are derived. The CGF is an irrotational perfect ﬂuid. It provides a synchronized global time coordinate and a global rest frame. There is a conserved number density. The energy density and pressure are related by the same equation of state as derived in the CGF cosmology and used in the TOV stellar structure equations for stars made of CGF dark matter. The present construction justiﬁes the TOV solution. Some possible routes towards testing the theory are suggested at the end.
Breaking Edge Shackles: Infrastructure-Free Collaborative Mobile Augmented Reality

Collaborative AR applications are gaining popularity, but have heavy computing requirements for identifying and tracking AR devices and objects in the ecosystem. Prior AR frameworks typically rely on edge infrastructure to offload AR's compute-heavy tasks. However, such infrastructure may not always be available, and continuously running AR computations on user devices can rapidly drain battery and impact application longevity. In this work, we enable infrastructure-free mobile AR with a low energy footprint, by using collaborative time slicing to distribute compute-heavy AR tasks across user devices. Realizing this idea is challenging because distributed execution can result in inconsistent synchronization of the AR virtual overlays. Our framework, FreeAR, tackles this with novel lightweight techniques for tightly synchronized virtual overlay placements across user views, and low latency recovery upon disruptions. We prototype FreeAR on Android and show that it can improve the virtual overlay positioning accuracy (with respect to the IOU metric) by up to 78%, relative to state-of-the-art collaborative AR systems, while also reducing power by up to 60% relative to a direct application of those prior solutions.
Formation and evolution of molecular hydrogen in disc galaxies with different masses and Hubble types

We investigate the physical properties of molecular hydrogen (H2) in isolated and interacting disk galaxies with different masses and Hubble types by using chemodynamical simulations with H2 formation on dust grains and dust growth and destruction in interstellar medium (ISM). We particularly focus on the dependences of H2 gas mass fractions (f_H2), spatial distributions of HI and H2, and local H2-scaling relations on initial halo masses (M_h), baryonic fractions (f_bary), gas mass fractions (f_g), and Hubble types. The principal results are as follows. The final f_H2 can be larger in disk galaxies with higher M_h, f_bary, and f_g. Some low-mass disk models with M_h smaller than 10^10 M_sun show extremely low f_H2 and thus no/little star formation, even if initial f_g is quite large (>0.9). Big galactic bulges can severely suppress the formation of H2 from HI on dust grains whereas strong stellar bars can not only enhance f_H2 but also be responsible for the formation of H2-dominated central rings. The projected radial distributions of H2 are significantly more compact than those of HI and the simulated radial profiles of H2-to-HI-ratios (R_mol) follow roughly R^-1.5 in MW-type disk models. Galaxy interaction can significantly increase f_H2 and total H2 mass in disk galaxies. The local surface mass densities of H2 can be correlated with those of dust in a galaxy. The observed correlation between R_mol and gas pressure (R_mol ~ P_g^0.92) can be well reproduced in the simulated disk galaxies.
High-precision phase diagram of spin glasses from duality analysis with real-space renormalization and graph polynomials

We propose a duality analysis for obtaining the critical manifold of two-dimensional spin glasses. Our method is based on the computation of quenched free energies with periodic and twisted periodic boundary conditions on a finite basis. The precision can be systematically improved by increasing the size of the basis, leading to very fast convergence towards the thermodynamic limit. We apply the method to obtain the phase diagrams of the random-bond Ising model and q-state Potts gauge glasses. In the Ising case, the Nishimori point is found at p N = 0.10929 ± 0.00002 ? > , in agreement with and improving on the precision of existing numerical estimations. Similar precision is found throughout the high-temperature part of the phase diagram. Finite-size effects are substantially larger in the low-temperature region, below the Nishimori point, but our results remain compatible with the known features of the phase diagram.
Choice of basic variables in current-density-functional theory

The selection of basic variables in current-density-functional theory and formal properties of the resulting formulations are critically examined. Focus is placed on the extent to which the Hohenberg-Kohn theorem, constrained-search approach, and Lieb’s formulation (in terms of convex and concave conjugation) of standard density-functional theory can be generalized to provide foundations for current-density-functional theory. For the well-known case with the gauge-dependent paramagnetic current density as a basic variable, we find that the resulting total energy functional is not concave. It is shown that a simple redefinition of the scalar potential restores concavity and enables the application of convex analysis and convex (or concave) conjugation. As a result, the solution sets arising in potential-optimization problems can be given a simple characterization. We also review attempts to establish theories with the physical current density as a basic variable. Despite the appealing physical motivation behind this choice of basic variables, we find that the mathematical foundations of the theories proposed to date are unsatisfactory. Moreover, the analogy to standard density-functional theory is substantially weaker as neither the constrained-search approach nor the convex analysis framework carry over to a theory making use of the physical current density.
The ATLASGAL survey: The sample of young massive cluster progenitors

The progenitors of high-mass stars and clusters are still challenging to recognise. Only unbiased surveys, sensitive to compact regions of high dust column density, can unambiguously reveal such a small population of particularly massive and cold clumps. Here we study a flux limited sample of compact sources from the ATLASGAL survey to identify a sample of candidate progenitors of massive clusters in the inner Galaxy. Sensitive mid-infrared data at 21-24 $\mu$m from the WISE and MIPSGAL surveys were explored to search for embedded objects, and complementary spectroscopic data were used to investigate their stability and star formation activity. Based on such ancillary data we identify an unbiased sample of infrared-quiet massive clumps in the Galaxy that potentially represent the earliest stages of massive cluster formation. An important fraction of this sample consists of sources that have not been studied in detail before. Comparing their properties to clumps hosting more evolved embedded objects, we find that they exhibit similar physical properties in terms of mass and size, suggesting that infrared-quiet massive clumps are not only capable of forming high-mass stars, but likely also follow a single evolutionary track leading to the formation of massive clusters. The majority of the sources are not in virial-equilibrium, suggesting collapse on the clump scale. This is in line with the low number of infrared-quiet massive clumps and earlier findings that star formation, in particular for high-mass objects is a fast, dynamic process. We propose a scenario in which massive clumps start to fragment and collapse before their final mass is accumulated indicating that strong self-gravity and global collapse is needed to build up rich clusters and the most massive stars.
Phase-sensitive terahertz imaging using room-temperature near-field nanodetector

Imaging applications in the terahertz (THz) frequency range are severely restricted by diffraction. Near-field scanning probe microscopy is commonly employed to enable mapping of the THz electromagnetic fields with sub-wavelength spatial resolution, allowing intriguing scientific phenomena to be explored, such as charge carrier dynamics in nanostructures and THz plasmon-polaritons in novel 2D materials and devices. High-resolution THz imaging, so far, has relied predominantly on THz detection techniques that require either an ultrafast laser or a cryogenically cooled THz detector. Here, we demonstrate coherent near-field imaging in the THz frequency range using a room-temperature nanodetector embedded in the aperture of a near-field probe, and an interferometric optical setup driven by a THz quantum cascade laser. By performing phase-sensitive imaging of strongly confined THz fields created by plasmonic focusing, we demonstrate the potential of our novel architecture for high-sensitivity coherent THz imaging with sub-wavelength spatial resolution.
THE EVOLUTION OF RADIO GALAXIES AND X-RAY POINT SOURCES IN COMA CLUSTER PROGENITORS SINCE z ∼ 1.2

Using Chandra imaging spectroscopy and Very Large Array (VLA) L-band radio maps, we have identified radio sources at P1.4 GHz ⩾ 5 × 1023 W Hz−1 and X-ray point sources (XPSs) at L0.3–8 keV ⩾ 5 × 1042 erg s−1 in L > L* galaxies in 12 high-redshift (0.4 < z < 1.2) clusters of galaxies. The radio galaxies and XPSs in this cluster sample, chosen to be consistent with Coma Cluster progenitors at these redshifts, are compared to those found at low-z analyzed in Hart et al. Within a projected radius of 1 Mpc of the cluster cores, we find 17 cluster radio galaxies (11 with secure redshifts, including one luminous FR II radio source at z = 0.826, and six more with host galaxy colors similar to cluster ellipticals). The radio luminosity function (RLF) of the cluster radio galaxies as a fraction of the cluster red-sequence (CRS) galaxies reveals significant evolution of this population from high-z to low-z, with higher power radio galaxies situated in lower temperature clusters at earlier epochs. Additionally, there is some evidence that cluster radio galaxies become more centrally concentrated than CRS galaxies with cosmic time. Within this same projected radius, we identify seven spectroscopically confirmed cluster XPSs, all with CRS host galaxy colors. Consistent with the results from Martini et al., we estimate a minimum X-ray active fraction of 1.4% ± 0.8% for CRS galaxies in high-z clusters, corresponding to an approximate 10-fold increase from 0.15% ± 0.15% at low-z. Although complete redshift information is lacking for several XPSs in z > 0.4 cluster fields, the increased numbers and luminosities of the CRS radio galaxies and XPSs suggest a substantial (9–10-fold) increase in the heat injected into high-redshift clusters by AGNs compared to the present epoch.