Miracle-dz/UniFAR-FTUs huggingface dataset:
Ab Initio Simulations of a Supernova-driven Galactic Dynamo in an Isolated Disk Galaxy

We study the magnetic field evolution of an isolated spiral galaxy, using isolated Milky Way–mass galaxy formation simulations and a novel prescription for magnetohydrodynamic (MHD) supernova feedback. Our main result is that a galactic dynamo can be seeded and driven by supernova explosions, resulting in magnetic fields whose strength and morphology are consistent with observations. In our model, supernovae supply thermal energy and a low-level magnetic field along with their ejecta. The thermal expansion drives turbulence, which serves a dual role by efficiently mixing the magnetic field into the interstellar medium and amplifying it by means of a turbulent dynamo. The computational prescription for MHD supernova feedback has been implemented within the publicly available ENZO code and is fully described in this paper. This improves upon ENZO's existing modules for hydrodynamic feedback from stars and active galaxies. We find that the field attains microgauss levels over gigayear timescales throughout the disk. The field also develops a large-scale structure, which appears to be correlated with the disk’s spiral arm density structure. We find that seeding of the galactic dynamo by supernova ejecta predicts a persistent correlation between gas metallicity and magnetic field strength. We also generate all-sky maps of the Faraday rotation measure from the simulation-predicted magnetic field, and we present a direct comparison with observations.
Do all QSOs have the same black hole mass

Quasi-stellar objects (QSOs) from SDSS, 2QZ and 2SLAQ covering an order of magnitude in luminosity at fixed redshift exhibit similar amplitudes of clustering, with the brightest sample showing a clustering length only 11 ± 9 per cent higher than the faintest sample. In addition, QSO clustering evolution at z > 0.5 is well fitted by a model that assumes a fixed host halo mass. If halo and black hole (BH) masses are related, then this may imply that QSOs occur in a relatively narrow range of halo masses with a correspondingly narrow range of BH mass. Hubble Space Telescope and Gemini high-resolution imaging of QSOs covering a large range in luminosity also show a relatively narrow range in QSO host galaxy luminosity. We argue that the slow evolution of early-type galaxies out to z≈ 1–2 may also provide further support for a slow evolution of QSO host BH masses. The result would mean that if high-z QSOs radiate at Eddington rates then low-z type 1 Seyfert galaxy must radiate at ≈100 times less than Eddington. We discuss the consequences in terms of four empirical models where (i) QSOs radiate at a fixed fraction of LEdd, (ii) QSO luminosity ‘flickers’ over time, (iii) QSOs have a single BH mass and (iv) QSOs are long lived and evolve via pure luminosity evolution (PLE). We conclude that the LEdd model requires MBH and Mhalo to be decoupled to circumvent the clustering results. While the single BH mass and flickering models fit the z > 0.5 clustering results, they appear to be rejected by the MBH–L relation found from reverberation mapping at z≈ 0. We find that the inclusion of z < 0.5 QSO clustering data improves the fit of a long-lived QSO model and suggest that the predictions of the PLE model for QSO BH masses agree reasonably with ultraviolet bump and reverberation estimates.
The importance of side branches of glycosylphosphatidylinositol anchors: a molecular dynamics perspective

Abstract Many proteins are anchored to the cell surface of eukaryotes using a unique family of glycolipids called glycosylphosphatidylinositol (GPI) anchors. These glycolipids also exist without a covalently bound protein, in particular on the cell surfaces of protozoan parasites where they are densely populated. GPIs and GPI-anchored proteins participate in multiple cellular processes such as signal transduction, cell adhesion, protein trafficking and pathogenesis of Malaria, Toxoplasmosis, Trypanosomiasis and prion diseases, among others. All GPIs share a common conserved glycan core modified in a cell-dependent manner with additional side glycans or phosphoethanolamine residues. Here, we use atomistic molecular dynamic simulations and perform a systematic study to evaluate the structural properties of GPIs with different side chains inserted in lipid bilayers. Our results show a flop-down orientation of GPIs with respect to the membrane surface and the presentation of the side chain residues to the solvent. This finding agrees well with experiments showing the role of the side residues as active epitopes for recognition of GPIs by macrophages and induction of GPI-glycan-specific immune responses. Protein-GPI interactions were investigated by attaching parasitic GPIs to Green Fluorescent Protein. GPIs are observed to recline on the membrane surface and pull down the attached protein close to the membrane facilitating mutual contacts between protein, GPI and the lipid bilayer. This model is efficient in evaluating the interaction of GPIs and GPI-anchored proteins with membranes and can be extended to study other parasitic GPIs and proteins and develop GPI-based immunoprophylaxis to treat infectious diseases.
The RMS Survey: Ammonia and water maser analysis of massive star forming regions. ⋆

The Red MSX Source (RMS) survey has identified a sample of∼1200 massive young stellar objects (MYSOs), compact and ultra compact Hii regions from a sample of∼2000 MSX and 2MASS colour selected sources. We have used the 100-m Green Bank telescope to search for 22-24 GHz water maser and ammonia (1,1), (2,2) and (3,3) emission towards∼600 RMS sources located within the northern Galactic plane. We have identified 308 H 2O masers which corresponds to an overall detection rate of∼50 per cent. We find no significant di fference in the detection rate for Hii regions and MYSOs which would suggest that the conditions required to produce maser emission are equally likely in both phases. Comparing the detection rates as a function of luminosity we find the H 2O detection rate has a positive dependence on the source luminosity, with the detection rate increasing with increasing luminosity. We detect ammonia emission towards 479 of these massive young stars, which corresponds to∼80 per cent. Ammonia is an excellent probe of high density gas allowing us to measure key parameters such as gas temperatures, opacities, and column densities, as well as providing an insight into the gas kinematics. The average kinetic temperature, FWHM line width and total NH3 column density for the sample are approximately 22 K, 2 km s −1 and 2× 10 15 cm −2 , respectively. We find that the NH 3 (1,1) line width and kinetic temperature are correlated with luminosity and finding no underlying dep endence of these parameters on the evolutionary phase of the embedded sources, we conclude that the observed trends in the derived parameters are more likely to be due to the energy output of the central source and/or the line width-clump mass relationship. The velocities of the peak H2O masers and the NH3 emission are in excellent agreement with each other, which would strongly suggest an association between the dense gas and the maser emission. Moreover, we find the bolometric luminosity of the embedded source and the isotropic luminosity of the H2O maser are also correlated. We conclude from the correlations of the cloud and water maser velocities and the bolometric and maser luminosity that there is a strong dynamical relationship between the embedded young massive star and the H2O maser.
Influence of genetic variants on remifentanil sensitivity in Chinese women

Significant individual differences have been observed in pain sensitivity and analgesic effect of opioids. Previous studies have shown that genetic factors contributed to analgesics requirement obviously. Therefore, we investigated the role of genetic polymorphisms in the sensitivity to the analgesic effect of remifentanil in this study.
RADIATION-HYDRODYNAMIC SIMULATIONS OF PROTOSTELLAR OUTFLOWS: SYNTHETIC OBSERVATIONS AND DATA COMPARISONS

We present results from three-dimensional, self-gravitating, radiation-hydrodynamic simulations of low-mass protostellar outflows. We construct synthetic observations in 12CO in order to compare with observed outflows and evaluate the effects of beam resolution and outflow orientation on inferred outflow properties. To facilitate the comparison, we develop a quantitative prescription for measuring outflow opening angles. Using this prescription, we demonstrate that, in both simulations and synthetic observations, outflow opening angles broaden with time similarly to observed outflows. However, the interaction between the outflowing gas and the turbulent core envelope produces significant asymmetry between the redshifted and blueshifted outflow lobes. We find that applying a velocity cutoff may result in outflow masses that are underestimated by a factor five or more, and masses derived from optically thick CO emission further underpredict the mass of the high-velocity gas by a factor of 5–10. Derived excitation temperatures indicate that outflowing gas is hotter than the ambient gas with temperature rising over time, which is in agreement with the simulation gas temperatures. However, excitation temperatures are otherwise not well correlated with the actual gas temperature.
Adapting community child and family health service models for rural and other diverse settings: A modified Delphi study to identify key elements

Abstract Inequity in health outcomes is pervasive, with poorer health outcomes identified in rural, regional and remote communities. An international call to action emphasises the need for service models adapted for less well‐resourced settings. The aim of this study was to identify key elements of a framework for the adaptation of specialist community‐based child and family health (CFH) service models for rural and other under‐resourced settings. A modified Delphi study was undertaken with a 12‐person expert panel in CFH including Australian and international professionals and parents from rural and remote communities. The study was informed by the WHO Framework for Strengthening Health Service Systems building blocks, the outcomes of an integrative review of literature and a Participatory Action Research study. Experts assessed 107 potential elements for service model development and rated them for importance when adapting service models for different contexts. Round 1 of the Delphi generated considerable consensus with 80 of the 107 potential elements identified as necessary for the service model adaptation framework. A further 17 elements for CFH service models were added in round 2. While multiple varied elements are important for adapting CFH service models for diverse settings, some elements had common themes. Experts highlighted the importance of community engagement and participation; utilising both data and local knowledge to develop a robust understanding of the community context; and the need for a flexible approach to funding and modes of service delivery to address barriers to implementation and access.
STAR FORMATION IN SELF-GRAVITATING TURBULENT FLUIDS

We present a model of star formation in self-gravitating turbulent gas in which the turbulent velocity, vT, is a dynamical variable and is adiabatically heated by the collapse. The theory predicts the run of density, infall, and turbulent velocity and the rate of star formation in compact massive clouds. The adiabatic heating ensures that the turbulent pressure is dynamically important at all radii. The system evolves toward a coherent spatial structure with a fixed run of density, &rgr; r , t → &rgr; r ? > ; mass flows through this structure onto the central star or star cluster. We define the sphere of influence of the accreted matter by m * = M g r * ? > , where m* is the stellar plus disk mass in the nascent star cluster and Mg(r) is the gas mass inside radius r. Both vT and the infall velocity, ∣ u r ∣ , ? > decrease with decreasing r for r > r * ? > ; v T r ∼ r p ? > , the size–line-width relation, with p ≈ 0.2 − 0.3 ? > , explaining the observation that Larson’s Law is altered in massive star-forming regions. The infall velocity is generally smaller than the turbulent velocity at r > r * ? > . For r < r * ? > , the infall and turbulent velocities are again similar, and both increase with decreasing r as r − 1 / 2 ? > , with a magnitude about half of the free-fall velocity. The accreted (stellar) mass grows superlinearly with time, M ˙ * = φ M cl t / τ ff 2 ? > , with ϕ a dimensionless number somewhat less than unity, M cl ? > the clump mass, and τ ff ? > the free-fall time of the clump. We suggest that small values of p can be used as a tracer of convergent collapsing flows.
Error bounds and exponential improvements for the asymptotic expansions of the gamma function and its reciprocal

In 1994 Boyd derived a resurgence representation for the gamma function, exploiting the 1991 reformulation of the method of steepest descents by Berry and Howls. Using this representation, he was able to derive a number of properties of the asymptotic expansion for the gamma function, including explicit and realistic error bounds, the smooth transition of the Stokes discontinuities and asymptotics for the late coefficients. The main aim of this paper is to modify Boyd’s resurgence formula, making it suitable for deriving better error estimates for the asymptotic expansions of the gamma function and its reciprocal. We also prove the exponentially improved versions of these expansions complete with error terms. Finally, we provide new (formal) asymptotic expansions for the coefficients appearing in the asymptotic series and compare their numerical efficacy with the results of earlier authors.
A comparison of multiband and multiband multiecho gradient‐echo EPI for task fMRI at 3 T

A multiband (MB) echo‐planar imaging (EPI) sequence is compared to a multiband multiecho (MBME) EPI protocol to investigate differences in sensitivity for task functional magnetic resonance imaging (fMRI) at 3 T. Multiecho sampling improves sensitivity in areas where single‐echo‐EPI suffers from dropouts. However, It requires in‐plane acceleration to reduce the echo train length, limiting the slice acceleration factor and the temporal and spatial resolution Data were acquired for both protocols in two sessions 24 h apart using an adapted color‐word interference Stroop task. Besides protocol comparison statistically, we performed test–retest reliability across sessions for different protocols and denoising methods. We evaluated the sensitivity of two different echo‐combination strategies for MBME‐EPI. We examined the performance of three different data denoising approaches: “Standard,” “AROMA,” and “FIX” for MB and MBME, and assessed whether a specific method is preferable. We consider using an appropriate autoregressive model order within the general linear model framework to correct TR differences between the protocols. The comparison between protocols and denoising methods showed at group level significantly higher mean z‐scores and the number of active voxels for MBME in the motor, subcortical and medial frontal cortices. When comparing different echo combinations, our results suggest that a contrast‐to‐noise ratio weighted echo combination improves sensitivity in MBME compared to simple echo‐summation. This study indicates that MBME can be a preferred protocol in task fMRI at spatial resolution (≥2 mm), primarily in medial prefrontal and subcortical areas.
CBTRUS Statistical Report: Primary Brain and Other Central Nervous System Tumors Diagnosed in the United States in 2015-2019.

The Central Brain Tumor Registry of the United States (CBTRUS), in collaboration with the Centers for Disease Control and Prevention and the National Cancer Institute, is the largest population-based registry focused exclusively on primary brain and other central nervous system (CNS) tumors in the United States (US) and represents the entire US population. This report contains the most up-to-date population-based data on primary brain tumors available and supersedes all previous reports in terms of completeness and accuracy. All rates are age-adjusted using the 2000 US standard population and presented per 100,000 population. The average annual age-adjusted incidence rate (AAAIR) of all malignant and non-malignant brain and other CNS tumors was 24.71 per 100,000 population (malignant AAAIR=7.02 and non-malignant AAAIR=17.69). This overall rate was higher in females compared to males (27.62 versus 21.60 per 100,000) and non-Hispanic persons compared to Hispanic persons (25.09 versus 22.95 per 100,000). The most commonly occurring malignant brain and other CNS histopathology was glioblastoma (14.2% of all tumors and 50.1% of all malignant tumors), and the most common non-malignant histopathology was meningioma (39.7% of all tumors and 55.4% of all non-malignant tumors). Glioblastoma was more common in males, and meningiomas were more common in females. In children and adolescents (ages 0-19 years), the incidence rate of all primary brain and other CNS tumors was 6.20 per 100,000 population. An estimated 93,470 new cases of malignant and non-malignant brain and other CNS tumors are expected to be diagnosed in the US population in 2022 (26,670 malignant and 66,806 non-malignant). There were 84,264 deaths attributed to malignant brain and other CNS tumors between 2015 and 2019. This represents an average annual mortality rate of 4.41 per 100,000 population and an average of 16,853 deaths per year. The five-year relative survival rate following diagnosis of a malignant brain and other CNS tumor was 35.7%, while for non-malignant brain and other CNS tumors the five-year relative survival rate was 91.8%.
Experimental evidence for the correlation between RNA structural fluctuations and the frequency of beneficial mutations

RNA has been used as a model molecule to understand the adaptive evolution process owing to the simple relationship between the structure (i.e., phenotype) and sequence (i.e., genotype). RNA usually forms multiple substructures with similar thermodynamic stabilities, called structural fluctuations. Ancel and Fontana theoretically proposed that structural fluctuation is directly related to the ease of change in structures by mutations and thus works as a source of adaptive evolution; however, experimental verification is limited. Here, we analyzed 76 RNA genotypes that appeared in our previous in vitro evolution to examine whether (i) RNA fluctuation decreases as adaptive evolution proceeds and (ii) RNAs that have larger fluctuations tend to have higher frequencies of beneficial mutations. We first computationally estimated the structural fluctuations of all RNAs and observed that they tended to decrease as their fitness increased. We next measured the frequency of beneficial mutations for 10 RNA genotypes and observed that the total number of beneficial mutations was correlated with the size of the structural fluctuations. These results consistently support the idea that the structural fluctuation of RNA, at least those evaluated in our study, works as a source of adaptive evolution.
Ground-state properties of one-dimensional anyon gases

We investigate the ground state of the one-dimensional interacting anyonic system based on the exact Bethe ansatz solution for arbitrary coupling constant (0 <= c <= infinity) and statistics parameter (0 <= K <= pi). It is shown that the density of state in quasimomentum k space and the ground-state energy are determined by the renormalized coupling constant c '. The effect induced by the statistics parameter K exhibits in the momentum distribution in two aspects: Besides the effect of renormalized coupling, the anyonic statistics results in the nonsymmetric momentum distribution when the statistics parameter K deviates from 0 (Bose statistics) and pi (Fermi statistics) for any coupling constant c. The momentum distribution evolves from a Bose distribution to a Fermi one as K varies from 0 to pi. The asymmetric momentum distribution comes from the contribution of the imaginary part of the nondiagonal element of reduced density matrix, which is an odd function of K. The peak at positive momentum will shift to negative momentum if k is negative.
GAS DEPLETION IN LOCAL GROUP DWARFS ON ∼250 kpc SCALES: RAM PRESSURE STRIPPING ASSISTED BY INTERNAL HEATING AT EARLY TIMES

A recent survey of the Galaxy and M31 reveals that more than 90% of dwarf galaxies within 270 kpc of their host galaxy are deficient in H i gas. At such an extreme radius, the coronal halo gas is an order of magnitude too low to remove H i gas through ram pressure stripping for any reasonable orbit distribution. However, all dwarfs are known to have an ancient stellar population (≳ 10 Gyr) from early epochs of vigorous star formation which, through heating of H i, could allow the hot halo to remove this gas. Our model looks at the evolution of these dwarf galaxies analytically as the host-galaxy dark matter halo and coronal halo gas build up over cosmic time. The dwarf galaxies—treated as spherically symmetric, smooth distributions of dark matter and gas—experience early star formation, which sufficiently heats the gas, allowing it to be removed easily through tidal stripping by the host galaxy, or ram pressure stripping by a tenuous hot halo (nH = 3 × 10−4 cm−3 at 50 kpc). This model of evolution is able to explain the observed radial distribution of gas-deficient and gas-rich dwarfs around the Galaxy and M31 if the dwarfs fell in at high redshift (z ∼ 3–10).
Immediate flapless full‐arch rehabilitation of edentulous jaws on 4 or 6 implants according to the prosthetic‐driven planning and guided implant surgery: A retrospective study on clinical and radiographic outcomes up to 10 years of follow‐up

Abstract Objectives to retrospectively evaluate clinical and radiographic outcomes of immediate, flapless full‐arch prostheses, supported by 4/6 implants according to prosthetic‐driven planning and guided surgery. Materials and Methods The study involved 28 edentulous patients (20 female/8 males; average age 67.75 ± 8.627 years), 32 prostheses (17 all‐on‐4/15 all‐on‐6) and 164 implants. The Implants survival, prostheses success/survival, peri‐implant marginal bone loss, incidence of biological and prosthetic complications were evaluated. Multiple linear regression analysis was performed to analyze the influence of implant and patient characteristics on marginal bone loss. Results Cumulative implant survival rate was 89.7% for all‐on‐four (seven failures) and 99.0% for all‐on‐six (one failure) after a mean follow‐up of 6.46 ± 2.236 years (range 1–10 years). Cumulative prosthesis success rate was 51.5% (58.8% for all‐on‐four/ 43.8% for all‐on‐six). Prosthesis survival rate was 88.2% for all‐on‐four. No failure was registered in all‐on‐six. Mean value of marginal bone loss was 1.38 ± 0.1. 28 mm at 5‐year and 2.09 ± 0.56 mm at 10‐year follow‐up. No difference was found in the mean value of marginal bone resorption between all‐on‐four (1.56 ± 1.61 mm) and all‐on‐six (1.20 ± 0.85 mm) (p = 0.104) and between tilted (1.22 ± 1.29 mm) and axial implants (1.44 ± 1.27 mm) (p = 0.385) after 5‐year follow‐up. The incidence of biological complications was 1.0% in all‐on‐six (one mucositis) and 10.3% in all‐on‐four (two peri‐implantitis). Prosthetic complications affected teeth of final rehabilitations with 3 detachments, 10 chippings or fractures, and 3 severe occlusal wears. Conclusions Based on the results and within the limitations of the present study, the implant‐supported hybrid prosthesis according to prosthetic‐driven planning and guided surgery showed to be an efficient, safe, and effective approach to rehabilitate edentulous jaws.