bluuebunny/crossref_metadata_2025_split huggingface dataset:
Antiretroviral drug exposure in urethral and glans surface sampling of the penis
Authors: Haaland Richard E. , Fountain Jeffrey , Dinh Chuong , Lupo L. Davis , Martin Amy , Conway-Washington Christopher , Hall LaShonda , Kelley Colleen F. , Garcia-Lerma J. Gerardo , Heneine Walid 
Published: April 2021

Abstract

Background
HIV exposure to penile tissues provides a risk of acquisition among men, yet studies evaluating penile antiretroviral (ARV) drug distribution have been lacking. We measured ARVs on urethral and glans surface swabs collected following a dose of tenofovir alafenamide, emtricitabine, elvitegravir, darunavir and cobicistat.

Methods
Thirty-five HIV-negative male participants provided urethral swabs, glans swabs, rectal swabs, blood and urine up to 96 h following a single dose of tenofovir alafenamide/emtricitabine/elvitegravir/cobicistat and darunavir. ARVs were measured by liquid chromatography–mass spectrometry with a lower limit of detection (LOD) of 1 ng/swab for swabs and 10 ng/mL for plasma and urine. Concentrations are reported as median and range.

Results
Urethral swab emtricitabine and darunavir concentrations peaked at 4 h for emtricitabine (36 ng/swab; 3–307 ng/swab) and 8 h for darunavir (25 ng/swab; 2–52 ng/swab). Glans swab emtricitabine and darunavir concentrations peaked 24 h after dosing (emtricitabine 14 ng/swab, &lt;LOD–328 ng/swab; darunavir 6 ng/swab, &lt;LOD–149 ng/swab). Estimated peak urethral secretion emtricitabine and darunavir concentrations are between 10 and 20 μg/mL, similar to rectal secretions, 4-fold greater than in plasma, but 2-fold lower than in urine. Tenofovir and elvitegravir were detected on less than 20% of urethral or glans swabs collected within 24 h of dosing.

Conclusions
We document ARV dosing in the urethra and on the glans surface with high drug concentrations noted for emtricitabine and darunavir and lower tenofovir and elvitegravir concentrations. Data suggest a potential protective role of urethral emtricitabine or darunavir against penile HIV acquisition.
Medical Summary Template for the Transfer of Patients with Inflammatory Bowel Disease from Pediatric to Adult Care
Authors: Benchimol Eric I , Afif Waqqas , Plamondon Sophie , Newhook Dennis , Nicholls Stuart G , Lévesque Dominique 
Published: April 2021

Abstract

Background
The transfer of information is a key aspect of the transition of adolescent patients with inflammatory bowel disease (IBD) from pediatric to adult care. This is typically accomplished through the use of a consultation letter with a medical summary of the patient being transferred. To improve the quality and completeness of information included in a transfer letter, we developed a standardized medical summary template by integrating the feedback of adult and pediatric health care providers.

Methods
To develop the letter template, we purposively sampled gastroenterologists or nurse practitioners caring for patients with IBD in four Canadian cities and invited them to take part in focus group discussions. Using a semi-structured approach, we explored the items deemed essential for inclusion in a transfer summary. Using the conventional content analysis framework, the focus group discussions were inductively coded to identify areas of priority for inclusion in the template.

Results
Four focus groups were conducted, comprising 17 health care providers of 30 invited (56.7% participation). The resulting medical summary template included the following major headings: patient/disease characteristics, therapeutics history (including medications and surgeries), clinical history and current status, noteworthy investigations, history of complications (including hospitalizations), family history, immunization history and psychosocial history. The template also addressed health system process factors (i.e., urgency of transfer, mode of delivery and confidentiality) to ensure a seamless transfer to adult care.

Conclusions
The standardized medical summary template should be used by pediatric providers to ensure that essential patient information and disease characteristics are sent to an adult provider.
Effect of Chilling on Quality Control Parameters of Sterile Queensland Fruit Fly (Diptera: Tephritidae)
Authors: Gaire Sushil K , Biswas Md Jamil Hossain , Benelli Maurizio , Rempoulakis Polychronis , Taylor Phillip W , Mainali Bishwo P 
Published: April 2021

AbstractQueensland fruit fly (Q-fly), Bactrocera tryoni (Froggatt), presents a major threat to Australian fruit production and trade. The sterile insect technique (SIT) is increasingly employed to manage Q-fly. Quality of sterile males released in SIT programs, and hence program efficacy, can be affected by pre- and post-production processes, such as mass rearing, packing, irradiation, transportation, and release. Given long distances from rear-out facilities to release sites, adult flies are usually chilled to reduce metabolism and stress during transportation. To guide SIT procedures, it is important to understand the impact of such practices on performance of sterile Q-fly. The present study assesses the effect of chilling temperature and exposure period on quality parameters of sterile Q-fly. We considered the effects of two temperature regimes (4 and 6°C) and six exposure periods (0, 1, 2, 4, 6, and 12 h) on chill-coma recovery time, flight ability, survival under nutritional stress, and longevity of both males and females. Flies chilled at 4°C took longer to recover than that those chilled at 6°C. Flight ability, survival under nutritional stress, and longevity all decreased as chilling period increased but did not differ between the two tested temperatures. We recommend that periods of chilling during transportation from rear-out facilities to release sites be minimized in order to retain quality of sterile Q-fly and that increased release rates be considered when longer chilling periods are required.
Topical Review: Medical Trauma During Early Childhood
Authors: De Young Alexandra C , Paterson Rebecca S , Brown Erin A , Egberts Marthe R , Le Brocque Robyne M , Kenardy Justin A , Landolt Markus A , Marsac Meghan L , Alisic Eva , Haag Ann-Christin 
Published: April 2021

Abstract

Objective
Early childhood is a high-risk period for exposure to traumatic medical events due to injury/illness. It is also one of the most important and vulnerable periods due to rapid development in neurobiological systems, attachment relationships, cognitive and linguistic capacities, and emotion regulation. The aim of this topical review is to evaluate empirical literature on the psychological impact of medical trauma during early childhood (0–6 years) to inform models of clinical care for assessing, preventing, and treating traumatic stress following injury/illness.

Methods
Topical review of empirical and theoretical literature on pediatric medical traumatic stress (PMTS) during early childhood.

Results
There are important developmental factors that influence how infants and young children perceive and respond to medical events. The emerging literature indicates that up to 30% of young children experience PMTS within the first month of an acute illness/injury and between 3% and 10% develop posttraumatic stress disorder. However, significant knowledge gaps remain in our understanding of psychological outcomes for infants and young children, identification of risk-factors and availability of evidence-based interventions for medical trauma following illness.

Conclusions
This topical review on medical trauma during early childhood provides: (a) definitions of key medical trauma terminology, (b) discussion of important developmental considerations, (c) summary of the empirical literature on psychological outcomes, risk factors, and interventions, (d) introduction to a stepped-model-of-care framework to guide clinical practice, and (e) summary of limitations and directions for future research.
Andexanet Alfa Use for Small Bowel Obstruction Patient With History of Sugiura Procedure
Authors: Brust Adam K , LeCourt Amarateedha P , Benham Derek A , Gower Jonathan R , Birmingham Sean D 
Published: April 2021

ABSTRACT
This case report is about a 51-year-old active duty male with JAK2 mutation and medical history significant for prehepatic portal hypertension from portal vein thrombus on lifelong anticoagulation with rivaroxaban, an oral factor Xa inhibitor, presenting with closed-loop small bowel obstruction requiring emergent laparotomy. We present this surgical case as it required emergent reversal of the oral factor Xa inhibitor with andexanet alfa.
Galaxy zoo builder: Morphological dependence of spiral galaxy pitch angle
Authors: Lingard Timothy , Masters Karen L , Krawczyk Coleman , Lintott Chris , Kruk Sandor , Simmons Brooke , Keel William , Nichol Robert C , Baeten Elisabeth 
Published: April 2021

ABSTRACT
Spiral structure is ubiquitous in the Universe, and the pitch angle of arms in spiral galaxies provide an important observable in efforts to discriminate between different mechanisms of spiral arm formation and evolution. In this paper, we present a hierarchical Bayesian approach to galaxy pitch angle determination, using spiral arm data obtained through the Galaxy Builder citizen science project. We present a new approach to deal with the large variations in pitch angle between different arms in a single galaxy, which obtains full posterior distributions on parameters. We make use of our pitch angles to examine previously reported links between bulge and bar strength and pitch angle, finding no correlation in our data (with a caveat that we use observational proxies for both bulge size and bar strength which differ from other work). We test a recent model for spiral arm winding, which predicts uniformity of the cotangent of pitch angle between some unknown upper and lower limits, finding our observations are consistent with this model of transient and recurrent spiral pitch angle as long as the pitch angle at which most winding spirals dissipate or disappear is larger than 10°.
Good and proper: self-similarity of N-body simulations with proper force softening
Authors: Garrison Lehman H , Joyce Michael , Eisenstein Daniel J 
Published: April 2021

ABSTRACT
Analysis of self-similarity in scale-free N-body simulations reveals the spatial and temporal scales for which statistics measured in cosmological simulations are converged to the physical continuum limit. We examine how the range of scales in which the two-point correlation function is converged depends on the force softening length and whether it is held constant in comoving or proper coordinates. We find that a proper softening that reaches roughly 1/30th of the inter-particle spacing by the end of the simulation resolves the same spatial and temporal scales as a comoving softening of the same length while using a third fewer time-steps, for a range of scale factors typical to Lambda cold dark matter (ΛCDM) simulations. We additionally infer an inherent resolution limit, set by the particle mass and scaling as a−1/2, beyond which reducing the softening does not improve the resolution. We postulate a mapping of these results with spectral index n = −2 to ΛCDM simulations.
A light echo from the warm outflow in the ULIRG F01004-2237 following a major flare in its optical continuum emission
Authors: Tadhunter C , Patel M , Mullaney J 
Published: April 2021

ABSTRACT
Emission-line variability studies have the potential to provide key information about the structures of the near-nuclear outflow regions of active galactic nuclei (AGN). Here we present a VLT/Xshooter spectrum of the nucleus of the ULIRG F01004-2237 that was taken in 2018 August, about 8 yr after a major flare in its integrated optical emission. Compared with our WHT/ISIS spectrum from 2015 September, the broad, red wings of the emission lines most closely associated with the flaring event, including He iiλ4686, N iiiλλ4640,4100, and He iλ5876, have substantially declined in flux. In contrast, the broad, blue wings that dominate the [O iii], [Ne iii], [Ne v], and [O i] forbidden lines have increased in flux by a factor 1.4–4.4 (depending on the line). Moreover, the [Fe vii]λ6087 line is detected in the new spectrum for the first time. We interpret these results in terms of a light echo from the outflowing warm gas: the direct emission from the flaring event is continuing to fade, but due to light travel time effects we are only now observing the impact of the flare on the emission from the extended outflow region. Unless the outflow is confined to a small range of angles close to our line of sight, these observations imply that the outflow must be relatively compact (r &lt;50 pc). In terms of the nature of the flare event, we speculate that the properties of the F01004-2237 flare may be the result of a tidal disruption event occurring in an object with pre-existing AGN activity.
Hybrid analytic and machine-learned baryonic property insertion into galactic dark matter haloes
Authors: Moews Ben , Davé Romeel , Mitra Sourav , Hassan Sultan , Cui Weiguang 
Published: April 2021

ABSTRACT
While cosmological dark matter-only simulations relying solely on gravitational effects are comparably fast to compute, baryonic properties in simulated galaxies require complex hydrodynamic simulations that are computationally costly to run. We explore the merging of an extended version of the equilibrium model, an analytic formalism describing the evolution of the stellar, gas, and metal content of galaxies, into a machine learning framework. In doing so, we are able to recover more properties than the analytic formalism alone can provide, creating a high-speed hydrodynamic simulation emulator that populates galactic dark matter haloes in N-body simulations with baryonic properties. While there exists a trade-off between the reached accuracy and the speed advantage this approach offers, our results outperform an approach using only machine learning for a subset of baryonic properties. We demonstrate that this novel hybrid system enables the fast completion of dark matter-only information by mimicking the properties of a full hydrodynamic suite to a reasonable degree, and discuss the advantages and disadvantages of hybrid versus machine learning-only frameworks. In doing so, we offer an acceleration of commonly deployed simulations in cosmology.
Ionizing feedback from an O star formed in a filament
Authors: Whitworth A P , Priestley F D 
Published: April 2021

ABSTRACT
We explore a simple semi-analytic model for what happens when an O star (or cluster of O stars) forms in an isolated filamentary cloud. The model is characterized by three configuration parameters: the radius of the filament, $R_{_{\rm FIL}}$, the mean density of H2 in the filament, $n_{_{\rm FIL}}$, and the rate at which the O star emits ionizing photons, $\dot{\cal N}_{_{\rm LyC}}$. We show that for a wide range of these configuration parameters, ionizing radiation from the O star rapidly erodes the filament, and the ionized gas from the filament disperses into the surroundings. Under these circumstances the distance, L, from the O star to the ionization front (IF) is given approximately by $L(t) \sim 5.2 {\rm pc} [R_{_{\rm FIL}}/0.2 {\rm pc}]^{-1/6} [n_{_{\rm FIL}}/10^4 {\rm cm^{-3}}]^{-1/3} [\dot{\cal N}_{_{\rm LyC}}/10^{49} {\rm s}^{-1}]^{1/6} [t/{\rm Myr}]^{2/3}$, and we derive similar simple power-law expressions for other quantities, for example the rate at which ionized gas boils off the filament, $\dot{M}_{_{\rm IF}}(t)$, and the mass, $M_{_{\rm SCL}}(t)$, of the shock-compressed layer that is swept up behind the IF. We show that a very small fraction of the ionizing radiation is expended locally, and a rather small amount of molecular gas is ionized and dispersed. We discuss some features of more realistic models, and the extent to which they might modify or invalidate the predictions of this idealized model. In particular we show that, for very large $R_{_{\rm FIL}}$ and/or large $n_{_{\rm FIL}}$ and/or low $\dot{\cal N}_{_{\rm LyC}}$, continuing accretion on to the filament might trap the ionizing radiation from the O star, slowing erosion of the filament even further.
Caught in the act: core-powered mass-loss predictions for observing atmospheric escape
Authors: Gupta Akash , Schlichting Hilke E 
Published: April 2021

ABSTRACT
Past studies have demonstrated that atmospheric escape by the core-powered mass-loss mechanism can explain a multitude of observations associated with the radius valley that separates the super-Earth and sub-Neptune planet populations. Complementing such studies, in this work, we present a shortlist of planets that could be losing their atmospheres today if their evolution is indeed primarily dictated by core-powered mass-loss. We use Bayesian inference analysis on our planet evolution and mass-loss model to estimate the posteriors of the parameters that encapsulate the current state of a given planet, given their published masses, radii, and host star properties. Our models predict that the following planets could be losing their atmospheres today at a rate ≳107 g s−1 at 50 per cent confidence level: pi Men c, Kepler-60 d, Kepler-60 b, HD 86226 c, EPIC 249893012 b, Kepler-107 c, HD 219134 b, Kepler-80 e, Kepler-138 d, and GJ 9827 d. As a by-product of our Bayesian inference analysis, we were also able to identify planets that most-likely harbour either secondary atmospheres abundant with high mean-molecular weight species, low-density interiors abundant with ices, or both. The planets belonging to this second category are WASP-47 e, Kepler-78 b, Kepler-10 b, CoRoT-7 b, HD 80653 b, 55 Cnc e, and Kepler-36 b. While the aforementioned lists are by no means exhaustive, we believe that candidates presented here can serve as useful input for target selection for future surveys and for testing the importance of core-powered mass-loss in individual planetary systems.
Characterization of lensing selection effects for LISA massive black hole binary mergers
Authors: Cusin Giulia , Tamanini Nicola 
Published: April 2021

ABSTRACT
We present a method to include lensing selection effects due to the finite horizon of a given detector when studying lensing of gravitational wave (GW) sources. When selection effects are included, the mean of the magnification distribution is shifted from one to higher values for sufficiently high-redshift sources. This introduces an irreducible (multiplicative) bias on the luminosity distance reconstruction, in addition to the typical source of uncertainty in the distance determination. We apply this method to study lensing of GWs emitted by massive black hole binary mergers at high redshift detectable by Laser Interferometer Space Antenna (LISA). We estimate the expected bias induced by selection effects on the luminosity distance reconstruction as function of cosmological redshift, and discuss its implications for cosmological and astrophysical analyses with LISA. We also reconstruct the distribution of lensing magnification as a function of the observed luminosity distance to a source, which is the observable quantity in the absence of an electromagnetic counterpart. Lensing provides the dominant source of errors in distance measurements of high-redshift GW sources. Its full characterization, including the impact of selection effects, is of paramount importance to correctly determine the astrophysical properties of the underlying source population and to be able to use GW sources as a new cosmological probe.
AGNs in small galaxy systems: comparing the main properties of active objects in pairs, triplets, and groups
Authors: Duplancic Fernanda , Lambas Diego G , Alonso Sol , Coldwell Georgina V 
Published: April 2021

ABSTRACT
We perform a comparative study of active galactic nuclei (AGNs) in pairs, triplets, and groups. To this end, we use the Duplancic et al. catalogue of small galaxy systems and consider BPT and WHAN diagnostic diagrams to select optical AGNs. Also, we identify mid-IR AGNs by using WISE data. We performed a comparison between the different AGN classification methodologies and study the AGN fraction in pairs, triplets, and groups with four to six members. We also analyse the main properties of Optical and mid-IR AGN hosts and the influence of environment on the active nuclei phenomena in these small galaxy systems. Our results show that, regardless the specifically adopted classification scheme, the fraction of AGN in pairs and triplets is always higher than the corresponding fraction in groups. Moreover, the fraction of powerful AGNs in pair and triplets is about twice the fraction of regular AGNs. We also find a remarkable difference between Optical and mid-IR AGNs in groups, where host galaxies of WISE AGNs are less massive and concentrated, with young stellar populations and blue colours. Also, all WISE AGNs in groups have a very close companions and reside in an intermediate global density environment. Galaxy triplets show a larger AGN fraction for galaxies with a close nearest neighbours, while pairs present a nearly constant AGN fraction regardless the distance to the nearest companion. Our studies highlight the important role of interactions, besides the global environment dependence, in the activation of the AGN phenomenon in small galaxy systems.
Protocluster detection in simulations of HSC–SSP and the 10-yr LSST forecast, using PCcones
Authors: Araya-Araya Pablo , Vicentin Marcelo C , Sodré Laerte , Overzier Roderik A , Cuevas Hector 
Published: April 2021

ABSTRACT
The progenitors of present-day galaxy clusters give important clues about the evolution of the large-scale structure, cosmic mass assembly, and galaxy evolution. Simulations are a major tool for these studies since they are used to interpret observations. In this work, we introduce a set of ‘protocluster-light-cones’, dubbed PCcones. They are mock galaxy catalogues generated from the Millennium Simulation with the L-GALAXIES semi-analytic model. These light-cones were constructed by placing a desired structure at the redshift of interest in the centre of the cone. This approach allows to adopt a set of observational constraints, such as magnitude limits and uncertainties in magnitudes and photometric redshifts (photo-zs) to produce realistic simulations of photometric surveys. We show that photo-zs obtained with PCcones are more accurate than those obtained directly with the Millennium Simulation, mostly due to the difference in how apparent magnitudes are computed. We apply PCcones in the determination of the expected accuracy of protocluster detection using photo-zs in the z = 1−3 range in the wide layer of HSC–SSP and the 10-yr LSST forecast. With our technique, we expect to recover only $\sim 38{{\ \rm per\ cent}}$ and $\sim 43{{\ \rm per\ cent}}$ of all massive galaxy cluster progenitors with more than 70 per cent of purity for HSC–SSP and LSST, respectively. Indeed, the combination of observational constraints and photo-z uncertainties affects the detection of structures critically for both emulations, indicating the need of spectroscopic redshifts to improve detection. We also compare our mocks of the Deep CFHTLS at z &lt; 1.5 with observed cluster catalogues, as an extra validation of the light-cones and methods.