bluuebunny/crossref_metadata_2025_split huggingface dataset:
Efficacy of Fecal Microbiota Transplantation for Recurrent C. Difficile Infection in Inflammatory Bowel Disease
Authors: Tariq Raseen , Disbrow Molly B , Dibaise John K , Orenstein Robert , Saha Srishti , Solanky Dipesh , Loftus Edward V , Pardi Darrell S , Khanna Sahil 
Published: December 2019

AbstractBackgroundClostridioides difficile infection (CDI) is associated with poor outcomes in inflammatory bowel disease (IBD) patients. Data are scarce on efficacy of fecal microbiota transplant (FMT) for recurrent CDI in IBD patients.MethodsWe reviewed health records of IBD patients (18 years of age or older) with recurrent CDI who underwent FMT. Outcomes of FMT for CDI were assessed on the basis of symptoms and stool test results.ResultsWe included 145 patients (75 women [51.7%]; median age, 46 years). Median IBD duration was 8 (range, 0–47) years, 36.6% had Crohn disease, 61.4% had ulcerative colitis, and 2.1% had indeterminate colitis. Median number of prior CDI episodes was 3 (range, 3–20), and 61.4% had received vancomycin taper. Diarrhea resolved after FMT in 48 patients (33.1%) without further testing. Ninety-five patients (65.5%) underwent CDI testing owing to post-FMT recurrent diarrhea; 29 (20.0%) had positive results. After FMT, 2 patients received empiric treatment of recurrent CDI without symptom resolution, suggesting IBD was the cause of symptoms. The overall cure rate of CDI after FMT was 80.0%, without CDI recurrence at median follow-up of 9.3 (range, 0.1–51) months. Forty-three patients (29.7%) had planned IBD therapy escalation after CDI resolution; none de-escalated or discontinued IBD therapy. Overall, 7.6% had worsening IBD symptoms after FMT that were treated as new IBD flares. No clinical predictors of FMT failure were identified.ConclusionsFew patients had new IBD flare after FMT. Fecal microbiota transplantation effectively treats recurrent CDI in IBD patients but has no apparent beneficial effect on the IBD course.
On Smooth Projective D-Affine Varieties
Authors: Langer Adrian 
Published: December 2019

Abstract
We show various properties of smooth projective D-affine varieties. In particular, any smooth projective D-affine variety is algebraically simply connected and its image under a fibration is D-affine. In characteristic 0 such D-affine varieties are also uniruled. We also show that (apart from a few small characteristics) a smooth projective surface is D-affine if and only if it is isomorphic to either ${{\mathbb{P}}}^2$ or ${{\mathbb{P}}}^1\times{{\mathbb{P}}}^1$. In positive characteristic, a basic tool in the proof is a new generalization of Miyaoka’s generic semipositivity theorem.
Current Understanding of Cytomegalovirus Reactivation in Critical Illness
Authors: Imlay Hannah , Limaye Ajit P 
Published: December 2019

Abstract
Cytomegalovirus (CMV) reactivation has been described in adults with critical illness caused by diverse etiologies, especially severe sepsis, and observational studies have linked CMV reactivation with worse clinical outcomes in this setting. In this study, we review observational clinical data linking development of CMV reactivation with worse outcomes in patients in the intensive care unit, discuss potential biologically plausible mechanisms for a causal association, and summarize results of initial interventional trials that examined the effects of CMV prevention. These data, taken together, highlight the need for a randomized, placebo-controlled efficacy trial (1) to definitively determine whether prevention of CMV reactivation improves clinical outcomes of patients with critical illness and (2) to define the underlying mechanism(s).
Comparative Effectiveness of Combined Favipiravir and Oseltamivir Therapy Versus Oseltamivir Monotherapy in Critically Ill Patients With Influenza Virus Infection
Authors: Wang Yeming , Fan Guohui , Salam Alex , Horby Peter , Hayden Frederick G , Chen Cheng , Pan Jianguang , Zheng Jing , Lu Binghuai , Guo Liping , Wang Chen , Cao Bin 
Published: December 2019

Abstract

Background
A synergistic effect of combination therapy with favipiravir and oseltamivir has been reported in preclinical models of influenza. However, no data are available on the clinical effectiveness of combination therapy in severe influenza.

Methods
Data from 2 separate prospective studies of influenza adults were used to compare outcomes between combination and oseltamivir monotherapy. Outcomes included rate of clinical improvement (defined as a decrease of 2 categories on a 7-category ordinal scale) and viral RNA detectability over time. Subhazard ratios (sHRs) were estimated by the Fine and Gray model for competing risks.

Results
In total, 40 patients were treated with combination therapy and 128 with oseltamivir alone. Clinical improvement on day 14 in the combination group was higher than in the monotherapy group (62.5% vs 42.2%; P = .0247). The adjusted sHR for combination therapy was 2.06 (95% confidence interval, 1.30–3.26). The proportion of undetectable viral RNA at day 10 was higher in the combination group than the oseltamivir group (67.5% vs 21.9%; P &lt; .01). No significant differences were observed in mortality or other outcomes.

Conclusions
Favipiravir and oseltamivir combination therapy may accelerate clinical recovery compared to oseltamivir monotherapy in severe influenza, and this strategy should be formally evaluated in a randomized controlled trial.
Validation of a novel hip arthroscopy simulator: establishing construct validity
Authors: Cychosz Christopher , Khazi Zain M , Karam Matthew , Duchman Kyle , Willey Michael , Westermann Robert 
Published: December 2019

AbstractHip arthroscopy (HA) is technically demanding and associated with a prolonged learning curve. Recently, arthroscopic simulators have been developed to anatomically model various joints including the knee, shoulder and hip. The purpose of this study is to validate a novel HA simulator. Twenty trainees and one sports medicine fellowship-trained orthopaedic surgeon at a single academic institution were recruited to perform a diagnostic HA procedure using the VirtaMed ArthroS hip simulator. Trainee characteristics, including level of training, general arthroscopy experience and hip specific arthroscopy experience, were gathered via questionnaire. For the purpose of this study, participants were categorized as novice (&lt;25), intermediate (25–74) or experienced (≥75) based on the number of prior arthroscopies performed. Various performance metrics, including composite score, time and camera path length were recorded for each attempt. Metrics were analyzed categorically using ANOVA tests with significance set to P &lt; 0.05. Composite performance score in the novice cohort was 114.5 compared with 146.4 and 151.5 in the intermediate and experienced cohorts (P = 0.0019), respectively. Novice arthroscopists performed the simulated diagnostic arthroscopy procedure in an average time of 321 s compared with 202 s and 181 s in the intermediate and experienced cohorts (P &lt; 0.002), respectively. Cartilage damage and simulator safety score did not differ significantly between groups (P = 0.775). Simulator composite score and procedure time showed strong correlation with year of training (r = 0.65 and −0.70, respectively) and number of arthroscopies performed (r = 0.65 and −0.72). The ArthroS hip simulator shows good construct validity and performance correlates highly with total number of arthroscopic cases reported during training.
Incidence and Risk Factors of Upper Extremity Injuries in Young Adult Men: A Nationwide Registry-Based Study of 128,714 Conscripts
Authors: Pihlajamäki Harri , Silvennoinen Arttu , Kuikka Paavo-Ilari , Luukkaala Tiina , Kröger Heikki , Kyröläinen Heikki 
Published: December 2019

AbstractIntroductionInjuries are the major cause of morbidity and loss of active training days in military populations. Previous investigations have mainly focused on lower extremities. This study evaluated the incidence, diagnosis, and risk factors of upper extremity injuries requiring hospitalization in a large cohort of Finnish conscripts during a 5-year period.Materials and MethodsA total of 128,714 male military conscripts, who served 6–12 months in compulsory military service, were studied. Injury hospitalization data were obtained from the National Hospital Discharge Register. The main outcome variables were hospitalization due to any injuries to the upper extremity and hospitalization due to traumatic shoulder dislocation. Background variables for risk factor analysis included length of military service, age, body height and weight, body mass index, and physical fitness.ResultsOverall person-based incidence rate for hospitalization due to upper extremity injury was 743 (95% confidence interval [CI]: 697–791) per 100,000 conscripts per year. Shoulder joint dislocation was the most common injury: incidence rate of 103 (95% CI: 86–122) per 100,000 conscripts per year. Trend during follow-up years 1998–2002 was decreasing concerning on any upper extremity injuries (odd ratios [OR] 0.90; 95% CI: 0.86–0.95, P &lt; 0.001). Body mass index &gt; 25 increased a risk for any injuries of the upper extremity (OR 1.29; CI 95%: 1.10–1.51) and, especially, for shoulder joint dislocation (OR 1.88; CI 95%: 1.26–2.80).ConclusionsOverweight young men were at greater risk for upper extremity injuries. The incidence rate of traumatic shoulder joint dislocation was considerably higher than reported previously. In conclusion, preventive measures such as reducing the body weight of overweight young men should play an important role in reducing the incidence of upper extremity injuries.
ALMA and ROSINA detections of phosphorus-bearing molecules: the interstellar thread between star-forming regions and comets
Authors: Rivilla V M , Drozdovskaya M N , Altwegg K , Caselli P , Beltrán M T , Fontani F , van der Tak F F S , Cesaroni R , Vasyunin A , Rubin M , Lique F , Marinakis S , Testi L ,   the ROSINA team, Balsiger H , Berthelier J J , De Keyser J , Fiethe B , Fuselier S A , Gasc S , Gombosi T I , Sémon T , Tzou C-Y 
Published: December 2019

ABSTRACT
To understand how phosphorus (P)-bearing molecules are formed in star-forming regions, we have analysed the Atacama Large Millimeter/Submillimeter Array (ALMA) observations of PN and PO towards the massive star-forming region AFGL 5142, combined with a new analysis of the data of the comet 67P/Churyumov–Gerasimenko taken with the Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) instrument onboard Rosetta. The ALMA maps show that the emission of PN and PO arises from several spots associated with low-velocity gas with narrow linewidths in the cavity walls of a bipolar outflow. PO is more abundant than PN in most of the spots, with the PO/PN ratio increasing as a function of the distance to the protostar. Our data favour a formation scenario in which shocks sputter phosphorus from the surface of dust grains, and gas-phase photochemistry induced by UV photons from the protostar allows efficient formation of the two species in the cavity walls. Our analysis of the ROSINA data has revealed that PO is the main carrier of P in the comet, with PO/PN &gt; 10. Since comets may have delivered a significant amount of prebiotic material to the early Earth, this finding suggests that PO could contribute significantly to the phosphorus reservoir during the dawn of our planet. There is evidence that PO was already in the cometary ices prior to the birth of the Sun, so the chemical budget of the comet might be inherited from the natal environment of the Solar system, which is thought to be a stellar cluster including also massive stars.
Following the crumbs: statistical effects of ram pressure in galaxies
Authors: Rodríguez S , Garcia Lambas D , Padilla N D , Troncoso-Iribarren P 
Published: December 2019

ABSTRACT
We analyse the presence of dust around galaxy group members through the reddening of background quasars. By taking into account quasar colour and their dependence on redshift and angular position, we derive mean quasar colours excess in projected regions around member galaxies and infer the associated dust mass. For disc-like galaxies perpendicular to the plane of the sky, and at groupcentric distances of the order of the virial radius, thus likely to reside in the infall regions of groups, we find systematic colour excess values e ∼ 0.009 ± 0.004 for g − r colour. Under the hypothesis of Milky Way dust properties, we derive dust masses of $5.8 \pm 2.5 \times 10^8 \, \mathrm{M}_{\odot }\, h^{-1}$, implying that a large fraction of dust is being stripped from galaxies in their path to groups. We also studied the photometry of member galaxies to derive a colour asymmetry relative to the group centre direction from a given galaxy. We conclude that the regions of galaxies facing the centre are bluer, consistent with the effects of gas compression and star formation. We also combine these two procedures finding that galaxies with a small colour asymmetry show the largest amounts of dust towards the external regions compared to a control sample. We conclude that dust removal is very efficient in galaxies on infall. The fact that galaxies redder towards groups centres are associated with the strongest reddening of background quasars suggest that gas removal induced by ram pressure stripping plays a key role in galaxy evolution and dust content.
A fast quadrature-based gravity model for the homogeneous polyhedron
Authors: Pearl Jason M , Hitt Darren L 
Published: December 2019

ABSTRACT
To date several probes have been sent to explore the Solar system’s asteroids and comets. These bodies are often irregular in shape and to safely navigate probes in their vicinity accurate gravity models are required. For an arbitrarily shaped constant-density body, the gravitational field can be determined from the surface topology and bulk properties. This is achieved by replacing the body’s true geometry with a polyhedron that closely resembles it and for which analytic equations for the gravitational field exist. For some applications however, these equations are too computationally expensive and it can be beneficial to replace them with numerically amenable approximations. In this work, a numerical-quadrature-based model for the gravitational field of a polyhedron consisting of triangular facets is derived. The proposed approximate model is found to be faster than its analytic counterpart. The error of the approximation is found to be negligible for the potential and Laplacian calculations. The approximate model introduces singularities to the surface of the acceleration calculation degrading the solution at altitudes less than the average edge length of the polyhedron.
On reverberation mapping lag uncertainties
Authors: Yu Z , Kochanek C S , Peterson B M , Zu Y , Brandt W N , Cackett E M , Fausnaugh M M , McHardy I M 
Published: December 2019

ABSTRACTWe broadly explore the effects of systematic errors on reverberation mapping lag uncertainty estimates from javelin and the interpolated cross-correlation function (ICCF) method. We focus on simulated light curves from random realizations of the light curves of five intensively monitored AGNs. Both methods generally work well even in the presence of systematic errors, although javelin generally provides better error estimates. Poorly estimated light-curve uncertainties have less effect on the ICCF method because, unlike javelin , it does not explicitly assume Gaussian statistics. Neither method is sensitive to changes in the stochastic process driving the continuum or the transfer function relating the line light curve to the continuum. The only systematic error we considered that causes significant problems is if the line light curve is not a smoothed and shifted version of the continuum light curve but instead contains some additional sources of variability.
Renormalization of linear halo bias in N-body simulations
Authors: Werner Kim F , Porciani Cristiano 
Published: December 2019

ABSTRACT
The interpretation of redshift surveys requires modelling the relationship between large-scale fluctuations in the observed number density of tracers, δh, and the underlying matter density, δ. Bias models often express δh as a truncated series of integro-differential operators acting on δ, each weighted by a bias parameter. Due to the presence of ‘composite operators’ (obtained by multiplying fields evaluated at the same spatial location), the linear bias parameter measured from clustering statistics does not coincide with that appearing in the bias expansion. This issue can be cured by re-writing the expansion in terms of ‘renormalized’ operators. After providing a pedagogical and comprehensive review of bias renormalization in perturbation theory, we generalize the concept to non-perturbative dynamics and successfully apply it to dark-matter haloes extracted from a large suite of N-body simulations. When comparing numerical and perturbative results, we highlight the effect of the window function employed to smooth the random fields. We then measure the bias parameters as a function of halo mass by fitting a non-perturbative bias model (both before and after applying renormalization) to the cross spectrum $P_{\delta _\mathrm{h}\delta }(k)$. Finally, we employ Bayesian model selection to determine the optimal operator set to describe $P_{\delta _\mathrm{h}\delta }(k)$ for $k\lt 0.2\, h$ Mpc−1 at redshift z = 0. We find that it includes δ, ∇2δ, δ2 and the square of the traceless tidal tensor, s2. Considering higher order terms (in δ) leads to overfitting as they cannot be precisely constrained by our data. We also notice that next-to-leading-order perturbative solutions are inaccurate for k ≳ 0.1 h Mpc−1.
Warm dark matter chills out: constraints on the halo mass function and the free-streaming length of dark matter with eight quadruple-image strong gravitational lenses
Authors: Gilman Daniel , Birrer Simon , Nierenberg Anna , Treu Tommaso , Du Xiaolong , Benson Andrew 
Published: December 2019

ABSTRACTThe free-streaming length of dark matter depends on fundamental dark matter physics, and determines the abundance and concentration of dark matter haloes on sub-galactic scales. Using the image positions and flux ratios from eight quadruply imaged quasars, we constrain the free-streaming length of dark matter and the amplitude of the subhalo mass function (SHMF). We model both main deflector subhaloes and haloes along the line of sight, and account for warm dark matter free-streaming effects on the mass function and mass–concentration relation. By calibrating the scaling of the SHMF with host halo mass and redshift using a suite of simulated haloes, we infer a global normalization for the SHMF. We account for finite-size background sources, and marginalize over the mass profile of the main deflector. Parametrizing dark matter free-streaming through the half-mode mass mhm, we constrain the thermal relic particle mass mDM corresponding to mhm. At $95 \, {\rm per\, cent}$ CI: mhm &lt; 107.8 M⊙ ($m_{\rm {DM}} \gt 5.2 \ \rm {keV}$). We disfavour $m_{\rm {DM}} = 4.0 \,\rm {keV}$ and $m_{\rm {DM}} = 3.0 \,\rm {keV}$ with likelihood ratios of 7:1 and 30:1, respectively, relative to the peak of the posterior distribution. Assuming cold dark matter, we constrain the projected mass in substructure between 106 and 109 M⊙ near lensed images. At $68 \, {\rm per\, cent}$ CI, we infer $2.0{-}6.1 \times 10^{7}\, {{\rm M}_{\odot }}\,\rm {kpc^{-2}}$, corresponding to mean projected mass fraction $\bar{f}_{\rm {sub}} = 0.035_{-0.017}^{+0.021}$. At $95 \, {\rm per\, cent}$ CI, we obtain a lower bound on the projected mass of $0.6 \times 10^{7} \,{{\rm M}_{\odot }}\,\rm {kpc^{-2}}$, corresponding to $\bar{f}_{\rm {sub}} \gt 0.005$. These results agree with the predictions of cold dark matter.
Effects of photoevaporation on protoplanetary disc ‘isochrones’
Authors: Somigliana Alice , Toci Claudia , Lodato Giuseppe , Rosotti Giovanni , Manara Carlo F 
Published: December 2019

ABSTRACT
Protoplanetary discs are the site of star and planet formation, and their evolution and consequent dispersal deeply affect the formation of planetary systems. In the standard scenario they evolve on time-scales ∼Myr due to the viscous transport of angular momentum. The analytical self-similar solution for their evolution predicts specific disc isochrones in the accretion rate–disc mass plane. However, photoevaporation by radiation emitted by the central star is likely to dominate the gas disc dispersal of the innermost region, introducing another (shorter) time-scale for this process. In this paper, we include the effect of internal (X and EUV) photoevaporation on the disc evolution, finding numerical solutions for a population of protoplanetary discs. Our models naturally reproduce the expected quick dispersal of the inner region of discs when their accretion rates match the rate of photoevaporative mass loss, in line with previous studies. We find that photoevaporation preferentially removes the lightest discs in the sample. The net result is that, counter-intuitively, photoevaporation increases the average disc mass in the sample, by dispersing the lightest discs. At the same time, photoevaporation also reduces the mass accretion rate by cutting the supply of material from the outer to the inner disc. In a purely viscous framework, this would be interpreted as the result of a longer viscous evolution, leading to an overestimate of the disc age. Our results thus show that photoevaporation is a necessary ingredient to include when interpreting observations of large disc samples with measured mass accretion rates and disc masses. Photoevaporation leaves a characteristic imprint on the shape of the isochrone. Accurate data of the accretion rate–disc mass plane in the low disc mass region therefore give clues on the typical photoevaporation rate.
The impact of non-dipolar magnetic fields in core-collapse supernovae
Authors: Bugli M , Guilet J , Obergaulinger M , Cerdá-Durán P , Aloy M A 
Published: December 2019

ABSTRACT
The magnetic field is believed to play an important role in at least some core-collapse supernovae (CCSN) if its magnitude reaches $10^{15}\, \rm {G}$, which is a typical value for a magnetar. In the presence of fast rotation, such a strong magnetic field can drive powerful jet-like explosions if it has the large-scale coherence of a dipole. The topology of the magnetic field is, however, probably much more complex with strong multipolar and small-scale components and the consequences for the explosion are so far unclear. We investigate the effects of the magnetic field topology on the dynamics of CCSN and the properties of the forming proto-neutron star (PNS) by comparing pre-collapse fields of different multipolar orders and radial profiles. Using axisymmetric special relativistic MHD simulations and a two-moment neutrino transport, we find that higher multipolar magnetic configurations lead to generally less energetic explosions, slower expanding shocks, and less collimated outflows. Models with a low order multipolar configuration tend to produce more oblate PNS, surrounded in some cases by a rotationally supported toroidal structure of neutron-rich material. Moreover, magnetic fields which are distributed on smaller angular scales produce more massive and faster rotating central PNS, suggesting that higher order multipolar configurations tend to decrease the efficiency of the magnetorotational launching mechanism. Even if our dipolar models systematically display a far more efficient extraction of the rotational energy of the PNS, fields distributed on smaller angular scales are still capable of powering magnetorotational explosions and shape the evolution of the central compact object.