bluuebunny/crossref_metadata_2025_split huggingface dataset:
Opioid Use Disorder and Associated Infectious Disease: The Role of the Laboratory in Addressing Health Disparities
Authors: Farnsworth Christopher W , Lloyd Matthew , Jean Sophonie 
Published: August 2020

Abstract

Background
Opioid use disorder, defined as a pattern of problematic opioid use leading to clinically significant impairment, has resulted in considerable morbidity and mortality throughout the world. This is due, at least in part, to the marginalized status of patients with opioid use disorder, limiting their access to appropriate laboratory testing, diagnosis, and treatment. Infections have long been associated with illicit drug use and contribute considerably to morbidity and mortality. However, barriers to testing and negative stigmas associated with opioid use disorder present unique challenges to infectious disease testing in this patient population.

Content
This review addresses the associations between opioid use disorder and infectious organisms, highlighting the health disparities encountered by patients with opioid use disorder, and the important role of laboratory testing for diagnosing and managing these patients.

Summary
Infections are among the most frequent and adverse complications among patients with opioid use disorder. As a result of health disparities and systemic biases, patients that misuse opioids are less likely to receive laboratory testing and treatment. However, laboratories play a crucial in identifying patients that use drugs illicitly and infections associated with illicit drug use.
Survival in patients with glioblastoma at a first progression does not correlate with isocitrate dehydrogenase (IDH)1 gene mutation status
Authors: Tabei Yusuke , Kobayashi Keiichi , Saito Kuniaki , Shimizu Saki , Suzuki Kaori , Sasaki Nobuyoshi , Shiokawa Yoshiaki , Nagane Motoo 
Published: August 2020

Abstract

Backgrounds
Mutations in the isocitrate dehydrogenase (IDH)1 gene are favourable prognostic factors in newly diagnosed diffuse gliomas, whereas it remains controversial in the recurrent glioblastoma setting.

Methods
A total of 171 patients with newly diagnosed glioblastoma, either ‘primary’ glioblastoma or ‘secondary’ glioblastoma, treated at Kyorin University Hospital or Japanese Red Cross Medical Center from 2000 to 2015 were included. Patients with confirmed IDH1 status and O6-methylguanine-DNA methyltransferase promoter methylation status were retrospectively analysed for overall survival from the initial diagnosis (n = 147) and after the first progression (n = 122).

Results
IDH1 mutation but not IDH2 was noted in 19 of 147 patients with glioblastoma (12.9%). In patients with ‘primary’ glioblastoma (n = 136), median overall survival after the first progression was 13.5 and 10.5 months for mutant IDH1 and wild-type IDH1 glioblastoma, respectively (P = 0.747). Multivariate analysis revealed O6-methylguanine-DNA methyltransferase promoter methylation, and Karnofsky Performance status 60 or higher, were independent prognostic factors for better overall survival after the first progression. When ‘primary’ glioblastoma and ‘secondary’ glioblastoma were combined, median overall survival from the first progression was not significantly different between the mutant IDH1 group (10.1 months) and wild-type IDH1 group (10.5 months) (P = 0.559), whereas median overall survival from the initial diagnosis was significantly different (47.5 months vs.18.3 months, respectively; P = 0.035).

Conclusions
These results suggest that IDH1 mutation may not be a prognostic factor for survival at the first progression of patients with ‘primary’ glioblastoma and pretreated ‘secondary’ glioblastoma, and further warrant investigation in prospective studies.
Incidence Trends and Burden of Human Papillomavirus-Associated Cancers Among Women in the United States, 2001-2017
Authors: Deshmukh Ashish A , Suk Ryan , Shiels Meredith S , Damgacioglu Haluk , Lin Yueh-Yun , Stier Elizabeth A , Nyitray Alan G , Chiao Elizabeth Y , Nemutlu Gizem S , Chhatwal Jagpreet , Schmeler Kathleen , Sigel Keith , Sonawane Kalyani 
Published: August 2020

Abstract
Human papillomavirus (HPV)-associated anal and oropharyngeal cancer incidence has increased in recent years among US women. However, trends in incidence and burden (annual number of cases) of noncervical HPV-associated cancers relative to cervical cancer remain unclear. Using the 2001-2017 US cancer statistics dataset, we evaluated contemporary incidence trends and burden (annual number of cases) of HPV-associated cancers among women by anatomic site, race or ethnicity, and age. Overall, cervical cancer incidence plateaued among White women but continued to decline among Black and Hispanic women. Anal cancer incidence surpassed cervical cancer incidence among White women aged 65-74 years of age (8.6 and 8.2 per 100 000 in 2015) and 75 years or older (6.2 and 6.0 per 100 000 in 2014). The noncervical cancer burden (n  =  11 871) surpassed the cervical cancer burden (n  =  11 527) in 2013. Development of efficacious screening strategies for noncervical cancers and continued improvement in cervical cancer prevention are needed to combat HPV-associated cancers among women.
Illness-Related Parenting Stress and Maladjustment in Congenital Heart Disease: Mindfulness as a Moderator
Authors: Bishop Meredith , Cohen Lindsey L , Robbertz Abigail S 
Published: August 2020

AbstractObjectiveCongenital heart disease (CHD) is characterized by structural defects to the heart or the coronary blood vessels and often requires surgical repair. Raising an infant or toddler with CHD can be challenging and lead to high parenting stress and maladjustment. The parenting literature suggests that mindfulness may buffer parenting stress. The purpose of this study was to examine whether mindfulness might moderate the relationship between illness-related parenting stress and maladjustment in parents of infants and toddlers with CHD.MethodsParents of infants and toddlers with CHD attending an outpatient clinic provided background information and completed measures of illness-related parenting stress, mindfulness, and maladjustment.ResultsResults indicated that illness-related parenting stress was associated with maladjustment, and mindfulness moderated this relationship. Specifically, illness-related parenting stress was related to maladjustment at low and average levels of mindfulness; at high mindfulness, there was no association between illness-related parenting stress and maladjustment.ConclusionsConsistent with the broader literatures, our sample of parents of infants and toddlers with CHD reported high illness-related parenting stress and maladjustment. Building on other studies demonstrating the benefits of mindful parenting, our results suggest that engaging in mindfulness might thwart the association between illness-related parenting stress and maladjustment in parents of infants and toddlers with CHD.
Convective differential rotation in stars and planets – I. Theory
Authors: Jermyn Adam S , Chitre Shashikumar M , Lesaffre Pierre , Tout Christopher A 
Published: August 2020

ABSTRACT
We derive the scaling of differential rotation in both slowly and rapidly rotating convection zones using order of magnitude methods. Our calculations apply across stars and fluid planets and all rotation rates, as well as to both magnetized and purely hydrodynamic systems. We find shear |R∇Ω| of order the angular frequency Ω for slowly rotating systems with Ω ≪ |N|, where N is the Brünt–Väisälä frequency, and find that it declines as a power law in Ω for rapidly rotating systems with Ω ≫ |N|. We further calculate the meridional circulation rate and baroclinicity and examine the magnetic field strength in the rapidly rotating limit. Our results are in general agreement with simulations and observations and we perform a detailed comparison with those in a companion paper.
The absolute proper motions of the Arches and Quintuplet clusters
Authors: Libralato Mattia , Fardal Mark , Lennon Daniel , van der Marel Roeland P , Bellini Andrea 
Published: August 2020

ABSTRACT
Arches and Quintuplet are two young, massive clusters projected near the Galactic Centre. To date, studies focused on understanding their origin have been based on proper motions (PMs) derived in the clusters’ reference frames and required some assumptions about their 3D motion. In this paper, we combine public PM catalogues of these clusters with the Gaia DR2 catalogue and, for the first time, transform the relative PMs of the Arches and Quintuplet clusters on to an absolute reference system. We find that the absolute PM of the Arches is (μαcos δ, μδ) = (−1.45 ± 0.23, −2.68 ± 0.14) mas yr−1 and that of the Quintuplet is (μαcos δ, μδ) = (−1.19 ± 0.09, −2.66 ± 0.18) mas yr−1. These values suggest that these systems are moving almost parallel to the Galactic plane. A measurement of the clusters’ distances is still required to meaningfully constrain the clusters’ orbits and shed light on the origin of the Arches and Quintuplet.
Cosmic flows in the nearby Universe: new peculiar velocities from SNe and cosmological constraints
Authors: Boruah Supranta S , Hudson Michael J , Lavaux Guilhem 
Published: August 2020

ABSTRACT
The peculiar velocity field offers a unique way to probe dark matter density field on large scales at low redshifts. In this work, we have compiled a new sample of 465 peculiar velocities from low redshift ($z$ &lt; 0.067) Type Ia supernovae. We compare the reconstructed velocity field derived from the 2M++ galaxy redshift compilation to the supernovae, the SFI++ and the 2MTF Tully–Fisher distance catalogues. We used a forward method to jointly infer the distances and the velocities of distance indicators by comparing the observations to the reconstruction. Comparison of the reconstructed peculiar velocity fields to observations allows us to infer the cosmological parameter combination fσ8, and the bulk flow velocity arising from outside the survey volume. The residual bulk flow arising from outside the 2M++ volume is inferred to be $171^{+11}_{-11}$ km s−1 in the direction l = 301° ± 4° and b = 0° ± 3°. We obtain fσ8 = 0.400 ± 0.017, equivalent to S8 ≈ σ8(Ωm/0.3)0.55 = 0.776 ± 0.033, which corresponds to an approximately $4{{\ \rm per\ cent}}\,$ statistical uncertainty on the value of fσ8. Our inferred value is consistent with other low redshift results in the literature.
Galaxy properties in the cosmic web of EAGLE simulation
Authors: Xu Wenxiao , Guo Qi , Zheng Haonan , Gao Liang , Lacey Cedric , Gu Qing , Liao Shihong , Shao Shi , Mao Tianxiang , Zhang Tianchi , Chen Xuelei 
Published: August 2020

ABSTRACT
We investigate the dependence of the galaxy properties on cosmic web environments using the most up-to-date hydrodynamic simulation: Evolution and Assembly of Galaxies and their Environments (EAGLE). The baryon fractions in haloes and the amplitudes of the galaxy luminosity function decrease going from knots to filaments to sheets to voids. Interestingly, the value of L* varies dramatically in different cosmic web environments. At z = 0, we find a characteristic halo mass of $10^{12}\, {\rm h}^{-1}\rm M_{\odot }$, below which the stellar-to-halo mass ratio is higher in knots, while above which it reverses. This particular halo mass corresponds to a characteristic stellar mass of $1.8\times 10^{10} \,{\rm h}^{-1}\rm M_{\odot }$. Below the characteristic stellar mass, central galaxies have redder colours, lower sSFRs, and higher metallicities in knots than those in filaments, sheets and voids, while above this characteristic stellar mass, the cosmic web environmental dependences either reverse or vanish. Such dependences can be attributed to the fact that the active galaxy fraction decreases along voids, sheets, filaments, and knots. The cosmic web dependences get weaker towards higher redshifts for most of the explored galaxy properties and scaling relations, except for the gas metallicity versus stellar mass relation.
Exoplanet validation with machine learning: 50 new validated Kepler planets
Authors: Armstrong David J , Gamper Jevgenij , Damoulas Theodoros 
Published: August 2020

ABSTRACT
Over 30 per cent of the $\sim$4000 known exoplanets to date have been discovered using ‘validation’, where the statistical likelihood of a transit arising from a false positive (FP), non-planetary scenario is calculated. For the large majority of these validated planets calculations were performed using the vespa algorithm. Regardless of the strengths and weaknesses of vespa, it is highly desirable for the catalogue of known planets not to be dependent on a single method. We demonstrate the use of machine learning algorithms, specifically a Gaussian process classifier (GPC) reinforced by other models, to perform probabilistic planet validation incorporating prior probabilities for possible FP scenarios. The GPC can attain a mean log-loss per sample of 0.54 when separating confirmed planets from FPs in the Kepler Threshold-Crossing Event (TCE) catalogue. Our models can validate thousands of unseen candidates in seconds once applicable vetting metrics are calculated, and can be adapted to work with the active Transiting Exoplanet Survey Satellite (TESS) mission, where the large number of observed targets necessitate the use of automated algorithms. We discuss the limitations and caveats of this methodology, and after accounting for possible failure modes newly validate 50 Kepler candidates as planets, sanity checking the validations by confirming them with vespa using up to date stellar information. Concerning discrepancies with vespa arise for many other candidates, which typically resolve in favour of our models. Given such issues, we caution against using single-method planet validation with either method until the discrepancies are fully understood.
Swift unveils the orbital period of IGR J18214-1318
Authors: Cusumano G , D’Aì A , Segreto A , La Parola V , Del Santo M 
Published: August 2020

ABSTRACT
We analysed 13 yr of the Neil Gehrels Swift Observatory survey data collected on the high-mass X-ray binary IGR J18214-1318. Performing the timing analysis, we detected a periodic signal of 5.42 d. From the companion star characteristics, we derived an average orbital separation of $\sim 41 \rm R_{\odot }\simeq 2 R_{\star }$. The spectral type of the companion star (O9) and the tight orbital separation suggest that IGR J18214-1318 is a wind-accreting source with eccentricity lower than 0.17. The intensity profile folded at the orbital period shows a deep minimum compatible with an eclipse of the source by the companion star. In addition, we report on the broad-band 0.6–100 keV spectrum using data from XMM–Newton, NuSTAR, and Swift, applying self-consistent physical models. We find that the spectrum is well fitted either by a pure thermal Comptonization component, or, assuming that the source is a neutron star accreting above the critical regime, by a combined thermal and bulk motion Comptonization model. In both cases, the presence of a local neutral absorption (possibly related to the thick wind of the companion star) is required.
Testing an indirect method for identifying galaxies with high levels of Lyman continuum leakage
Authors: Yamanaka Satoshi , Inoue Akio K , Yamada Toru , Zackrisson Erik , Iwata Ikuru , Micheva Genoveva , Mawatari Ken , Hashimoto Takuya , Kubo Mariko 
Published: August 2020

ABSTRACT
Using a sample of galaxies at z ≈ 3 with detected Lyman Continuum (LyC) leakage in the SSA22 field, we attempt to verify a proposed indirect method for identifying cases with high LyC escape fraction fesc based on measurements of the H β equivalent width (EW) and the β slope of the UV continuum. To this end, we present Keck/MOSFIRE H β emission line flux measurements of LyC galaxies (LCGs) at spectroscopic redshifts zspec ∼ 3.3, Lyman break galaxies (LBGs) at photometric redshifts zphot = 2.7–3.7, and Ly α emitters at zphot = 3.1. We also reconfirm the spectroscopic redshifts and measure the H β emission-line fluxes from two LCGs and six LBGs. For the LCG in our sample with the most extreme fesc, as revealed by the direct detection of LyC photons, we find that the EW(H β)–β method gives a broadly consistent estimate for fesc, although the error bars remain very large. We also discuss how a combination of fesc measurements based on direct and indirect methods can shed light on the LyC escape mechanism and the anisotropy of the leakage.
An eclipsing M-dwarf close to the hydrogen burning limit from NGTS
Authors: Acton Jack S , Goad Michael R , Casewell Sarah L , Vines Jose I , Burleigh Matthew R , Eigmüller Philipp , Nielsen Louise D , Gänsicke Boris T , Bayliss Daniel , Bouchy François , Bryant Edward M , Gill Samuel , Gillen Edward , Günther Maximilian N , Jenkins James S , McCormac James , Moyano Maximiliano , Raynard Liam R , Tilbrook Rosanna H , Udry Stéphane , Watson Christopher A , West Richard G , Wheatley Peter J 
Published: August 2020

ABSTRACT
We present the discovery of NGTS J0930−18, an extreme mass ratio eclipsing M-dwarf binary system with an early M-dwarf primary and a late M-dwarf secondary close to the hydrogen burning limit. Global modelling of photometry and radial velocities reveals that the secondary component (NGTS J0930−18 B) has a mass of M* = $0.0818 ^{+0.0040}_{-0.0015}$ M⊙ and radius of R* = $0.1059 ^{+0.0023}_{-0.0021}$ R⊙, making it one of the lowest mass stars with direct mass and radius measurements. With a mass ratio of q = $0.1407 ^{+0.0065}_{-0.017}$, NGTS J0930−18 has the lowest mass ratio of any known eclipsing M-dwarf binary system, posing interesting questions for binary star formation and evolution models. The mass and radius of NGTS J0930−18 B is broadly consistent with stellar evolutionary models. NGTS J0930−18 B lies in the sparsely populated mass radius parameter space close to the substellar boundary. Precise measurements of masses and radii from single lined eclipsing binary systems of this type are vital for constraining the uncertainty in the mass–radius relationship – of importance due to the growing number of terrestrial planets being discovered around low-mass stars.
Gas trapping of hot dust around main-sequence stars
Authors: Pearce Tim D , Krivov Alexander V , Booth Mark 
Published: August 2020

ABSTRACT
In 2006, Vega was discovered to display excess near-infrared (NIR) emission. Surveys now detect this phenomenon for one fifth of main-sequence stars, across various spectral types and ages. The excesses are interpreted as populations of small, hot dust grains very close to their stars, which must originate from comets or asteroids. However, the presence of such grains in copious amounts is mysterious, since they should rapidly sublimate or be blown out of the system. Here, we investigate a potential mechanism to generate excesses: dust migrating inwards under radiation forces sublimates near the star, releasing modest quantities of gas that then traps subsequent grains. This mechanism requires neither specialized system architectures nor high dust supply rates, and could operate across diverse stellar types and ages. The model naturally reproduces many features of inferred dust populations, in particular their location, preference for small grains, steep size distribution, and dust location scaling with stellar luminosity. For Sun-like stars, the mechanism can produce ${2.2 \; \mu {\rm m}}$ excesses that are an order of magnitude larger than those at ${8.5 \; \mu {\rm m}}$, as required by observations. However, for A-type stars the simulated NIR excesses were only twice those in the mid-infrared; grains would have to be 5–10 times smaller than those trapped in our model to be able to explain observed NIR excesses around A stars. Further progress with any hot dust explanation for A stars requires a means for grains to become very hot without either rapidly sublimating or being blown out of the system.
On the precision of full-spectrum fitting of simple stellar populations – I. Well-sampled populations
Authors: Asa’d Randa , Goudfrooij Paul 
Published: August 2020

ABSTRACT
We investigate the precision of the ages and metallicities of 21 000 mock simple stellar populations (SSPs) determined through full-spectrum fitting. The mock SSPs cover an age range of 6.8 &lt; log (age/yr) &lt; 10.2, for three wavelength ranges in the optical regime, using both Padova and MIST isochrone models. Random noise is added to the model spectra to achieve S/N ratios between 10 and 100 per wavelength pixel. We find that for S/N ≥ 50, this technique can yield ages of SSPs to an overall precision of ∆log (age/yr)∼01 for ages in the ranges 7.0 ≤ log (age/yr) ≤ 8.3 and 8.9 ≤ log (age/yr) ≤ 9.4. For the age ranges of 8.3 ≤ log (age/yr) ≤ 8.9 and log (age/yr) ≥ 9.5, which have significant flux contributions from asymptotic giant branch and red giant branch stars, respectively, the age uncertainty rises to about ±0.3 dex. The precision of age and metallicity estimation using this method depends significantly on the S/N and the wavelength range used in the fitting. We quantify the systematic differences in age predicted by the MIST and Padova isochrone models, due to their different assumptions about stellar physics in various important (i.e. luminous) phases of stellar evolution, which needs to be taken in consideration when comparing ages of star clusters obtained using these popular models. Knowing the strengths and limitations of this technique is crucial in interpreting the results obtained for real star clusters and for deciding the optimal instrument set-up before performing the observations.
Formation of superstrong horizontal magnetic field in delta-type sunspot in radiation magnetohydrodynamic simulations
Authors: Hotta H , Toriumi S 
Published: August 2020

ABSTRACT
We perform a series of radiative magnetohydrodynamic simulations to understand the amplification mechanism of the exceptionally strong horizontal magnetic field in delta-type sunspots. In the simulations, we succeed in reproducing the delta-type sunspot and resulting strong magnetic field exceeding 6000 G in a light bridge between the positive and negative polarities. Our conclusions in this study are summarized as follows: (1) The essential amplification mechanism of the strong horizontal magnetic field is the shear motion caused by the rotation of two spots. (2) The strong horizontal magnetic field remains the force-free state. (3) The peak strength of the magnetic fields does not depend on the spatial resolution, top boundary condition, or Alfvén speed limit. The origin of the rotating motion is rooted in the deep convection zone. Therefore, the magnetic field in the delta-spot light bridge can be amplified to the superequipartition values in the photosphere.
Magnetizing the circumgalactic medium of disc galaxies
Authors: Pakmor Rüdiger , van de Voort Freeke , Bieri Rebekka , Gómez Facundo A , Grand Robert J J , Guillet Thomas , Marinacci Federico , Pfrommer Christoph , Simpson Christine M , Springel Volker 
Published: August 2020

ABSTRACT
The circumgalactic medium (CGM) is one of the frontiers of galaxy formation and intimately connected to the galaxy via accretion of gas on to the galaxy and gaseous outflows from the galaxy. Here, we analyse the magnetic field in the CGM of the Milky Way-like galaxies simulated as part of the auriga project that constitutes a set of high-resolution cosmological magnetohydrodynamical zoom simulations. We show that before z = 1 the CGM becomes magnetized via galactic outflows that transport magnetized gas from the disc into the halo. At this time, the magnetization of the CGM closely follows its metal enrichment. We then show that at low redshift an in situ turbulent dynamo that operates on a time-scale of Gigayears further amplifies the magnetic field in the CGM and saturates before z = 0. The magnetic field strength reaches a typical value of $0.1\, \mu \mathrm{ G}$ at the virial radius at z = 0 and becomes mostly uniform within the virial radius. Its Faraday rotation signal is in excellent agreement with recent observations. For most of its evolution, the magnetic field in the CGM is an unordered small-scale field. Only strong coherent outflows at low redshift are able to order the magnetic field in parts of the CGM that are directly displaced by these outflows.