bluuebunny/crossref_metadata_2025_split huggingface dataset:
Understanding the management of heart failure with preserved ejection fraction: a qualitative multiperspective study
Authors: Sowden Emma , Hossain Muhammad , Chew-Graham Carolyn , Blakeman Tom , Tierney Stephanie , Wellwood Ian , Rosa Francesca , Deaton Christi 
Published: November 2020

BackgroundAbout half of all people with heart failure have heart failure with preserved ejection fraction (HFpEF), in which the heart is stiff. This type of heart failure is more common in older people with a history of hypertension, obesity, and diabetes mellitus. Patients with HFpEF are often managed in primary care, sometimes in collaboration with specialists. Knowledge about how best to manage this growing population is limited, and there is a pressing need to improve care for these patients.AimTo explore clinicians’ and patients’/carers’ perspectives and experiences about the management of HFpEF to inform the development of an improved model of care.Design and settingA multiperspective qualitative study involving primary and secondary care settings across the east of England, Greater Manchester, and the West Midlands.MethodSemi-structured interviews and focus groups were conducted. Transcribed data were analysed using framework analysis and informed by the normalisation process theory (NPT).ResultsIn total, 50 patients, nine carers/relatives, and 73 clinicians were recruited. Difficulties with diagnosis, unclear illness perceptions, and management disparity were identified as important factors that may influence management of HFpEF. The NPT construct of coherence reflected what participants expressed about the need to improve the identification, understanding, and awareness of this condition in order to improve care.ConclusionThere is a pressing need to raise the public and clinical profile of HFpEF, develop a clear set of accepted practices concerning its management, and ensure that systems of care are accessible and attuned to the needs of patients with this condition.
Healthcare practitioner views and experiences of patients self-monitoring blood pressure: a vignette study
Authors: Andrews Jacob A , Weiner Kate , Will Catherine M , Henwood Flis , Dickson Jon M 
Published: November 2020

BackgroundHome self-monitoring of blood pressure is widely used in primary care to assist in the diagnosis of hypertension, as well as to improve clinical outcomes and support adherence to medication. The National Institute for Health and Care Excellence (NICE) care pathways for hypertension recommend specific guidelines, although they lack detail on supporting patients to self-monitor.AimTo elicit primary care practitioners’ experiences of managing patients’ home blood pressure self-monitoring, across surgeries located in different socioeconomic areas.Design & settingA qualitative focus group study was conducted with a total of 21 primary care professionals.MethodParticipants were GPs and practice nurses (PNs), purposively recruited from surgeries in areas of low and high deprivation, according to the English indices of multiple deprivation. Six vignettes were developed featuring data from interviews with people who self-monitor and these were used in five focus groups. Results were thematically analysed.ResultsThemes derived in the thematic analysis largely reflected topics covered by the vignettes. These included: advice on purchase of a device; supporting home monitoring; mitigating patient anxiety experienced as a result of home monitoring; valuing patients’ data; and effect of socioeconomic factors.ConclusionThe work provides an account of methods used by primary care practitioners in the management of home blood pressure self-monitoring, where guidance may be lacking and primary care practitioners act on their own judgement. Findings complement recent policy documentation, which recognises the need to adopt new ways of working to empower patients (for example, additional support from healthcare assistants), but lacks detail on how this should be done.
Evaluating a cardiovascular disease risk management care continuum within a learning healthcare system: a prospective cohort study
Authors: Groenhof T Katrien J , Lely A Titia , Haitjema Saskia , Nathoe Hendrik M , Kortekaas Marlous F , Asselbergs Folkert W , Bots Michiel L , Hollander Monika 
Published: November 2020

BackgroundMany patients now present with multimorbidity and chronicity of disease. This means that multidisciplinary management in a care continuum, integrating primary care and hospital care services, is needed to ensure high quality care.AimTo evaluate cardiovascular risk management (CVRM) via linkage of health data sources, as an example of a multidisciplinary continuum within a learning healthcare system (LHS).Design & settingIn this prospective cohort study, data were linked from the Utrecht Cardiovascular Cohort (UCC) to the Julius General Practitioners' Network (JGPN) database. UCC offers structured CVRM at referral to the University Medical Centre (UMC) Utrecht. JGPN consists of electronic health record (EHR) data from referring GPs.MethodThe cardiovascular risk factors were extracted for each patient 13 months before referral (JGPN), at UCC inclusion, and during 12 months follow-up (JGPN). The following areas were assessed: registration of risk factors; detection of risk factor(s) requiring treatment at UCC; communication of risk factors and actionable suggestions from the specialist to the GP; and change of management during follow-up.ResultsIn 52% of patients, ≥1 risk factors were registered (that is, extractable from structured fields within routine care health records) before UCC. In 12%–72% of patients, risk factor(s) existed that required (change or start of) treatment at UCC inclusion. Specialist communication included the complete risk profile in 67% of letters, but lacked actionable suggestions in 86%. In 29% of patients, at least one risk factor was registered after UCC. Change in management in GP records was seen in 21%–58% of them.ConclusionEvaluation of a multidisciplinary LHS is possible via linkage of health data sources. Efforts have to be made to improve registration in primary care, as well as communication on findings and actionable suggestions for follow-up to bridge the gap in the CVRM continuum.
Evaluating a clinical tool (FAMCAT) for identifying familial hypercholesterolaemia in primary care: a retrospective cohort study
Authors: Akyea Ralph K , Qureshi Nadeem , Kai Joe , de Lusignan Simon , Sherlock Julian , McGee Christopher , Weng Stephen 
Published: November 2020

BackgroundFamilial hypercholesterolaemia (FH) is an inherited lipid disorder causing premature heart disease, which is severely underdiagnosed. Improving the identification of people with FH in primary care settings would help to reduce avoidable heart attacks and early deaths.AimTo evaluate the accuracy of the familial hypercholesterolaemia case ascertainment identifcation tool (FAMCAT) for identifying FH in primary care.Design & settingA retrospective cohort study of 1 030 183 patients was undertaken. Data were extracted from the UK Royal College of General Practitioners (RCGP) Research and Surveillance Centre (RSC) database. Patient were aged >16 years.MethodThe FAMCAT algorithm was compared with methods of FH detection recommended by national guidelines (Simon Broome diagnostic criteria, Dutch Lipid Clinic Network [DLCN] Score, and cholesterol levels >99th centile). Discrimination and calibration were assessed by area under the receiver operating curve (AUC) and by comparing observed versus predicted cases.ResultsA total of 1707 patients had a diagnosis of FH. FAMCAT showed a high level of discrimination (AUC = 0.844, 95% confidence interval [CI] = 0.834 to 0.854), performing significantly better than Simon Broome criteria (AUC = 0.730, 95% CI = 0.719 to 0.741), DLCN Score (AUC = 0.766, 95% CI = 0.755 to 0.778), and screening cholesterols >99 th centile (AUC = 0.579, 95% CI = 0.571 to 0.588). Inclusion of premature myocardial infarction (MI) and fitting cholesterol as a continuous variable improved the accuracy of FAMCAT (AUC = 0.894, 95% CI = 0.885 to 0.903).ConclusionBetter performance of the FAMCAT algorithm, compared with other approaches for case finding of FH in primary care, such as Simon Broome criteria, DLCN criteria or very high cholesterol levels, has been confirmed in a large population cohort.
Reflected Light Observations of the Galilean Satellites from Cassini: A Test Bed for Cold Terrestrial Exoplanets
Authors: Mayorga L. C. , Charbonneau David , Thorngren D. P. 
Published: November 2020

Abstract
For terrestrial exoplanets with thin or no atmospheres, the surface contributes light to the reflected light signal of the planet. Measurement of the variety of disk-integrated brightnesses of bodies in the solar system and the variation with illumination and wavelength is essential for both planning imaging observations of directly imaged exoplanets and interpreting the eventual data sets. Here we measure the change in brightness of the Galilean satellites as a function of planetocentric longitude, illumination phase angle, and wavelength. The data span a range of wavelengths from 400 to 950 nm and predominantly phase angles from 0° to 25°, with some constraining observations near 60°–140°. Despite the similarity in size and density between the moons, surface inhomogeneities result in significant changes in the disk-integrated reflectivity with planetocentric longitude and phase angle. We find that these changes are sufficient to determine the rotational periods of the moon. We also find that at low phase angles, the surface can produce reflectivity variations of 8%–36%, and the limited high phase angle observations suggest variations will have proportionally larger amplitudes at higher phase angles. Additionally, all of the Galilean satellites are darker than predicted by an idealized Lambertian model at the phases most likely to be observed by direct imaging missions. If Earth-sized exoplanets have surfaces similar to that of the Galilean moons, we find that future direct imaging missions will need to achieve precisions of less than 0.1 ppb. Should the necessary precision be achieved, future exoplanet observations could exploit similar observation schemes to deduce surface variations, determine rotation periods, and potentially infer surface composition.
Dynamical Mass Estimates of the β Pictoris Planetary System through Gaussian Process Stellar Activity Modeling
Authors: Vandal Thomas , Rameau Julien , Doyon René 
Published: November 2020

Abstract
Nearly 15 yr of radial velocity (RV) monitoring and direct imaging enabled the detection of two giant planets orbiting the young, nearby star β Pictoris. The δ Scuti pulsations of the star, which overwhelm planetary signals, need to be carefully suppressed. In this work, we independently revisit the analysis of the RV data following a different approach than available in the literature to model the activity of the star. We show that a Gaussian process (GP) with a stochastically driven damped harmonic oscillator kernel can model the δ Scuti pulsations. It provides similar results to parametric models but with a simpler framework, using only three hyperparameters. It also enables us to model poorly sampled RV data that were excluded from previous analyses, hence extending the RV baseline by nearly five years. Altogether, the orbit and mass of both planets can be constrained from RV only, which was not possible with the parametric modeling. To characterize the system more accurately, we also perform a joint fit of all available relative astrometry and RV data. Our orbital solutions for

b favor a low eccentricity of

and a relatively short period of

yr. The orbit of

c is eccentric with

with a period of 3.36 ± 0.03 yr. We find model-independent masses of 11.7 ± 1.4 and 8.5 ± 0.5

for

b and c, respectively, assuming coplanarity. The mass of

b is consistent with the hottest start evolutionary models, at an age of 25 ± 3 Myr. A direct detection of

c would provide a second calibration measurement in a coeval system.
Discovery of Extended Tidal Tails around the Globular Cluster Palomar 13
Authors: Shipp Nora , Price-Whelan Adrian M. , Tavangar Kiyan , Mateu Cecilia , Drlica-Wagner Alex 
Published: November 2020

Abstract
We use photometry from the DECam Legacy Survey to detect candidate tidal tails extending ∼5° on either side of the Palomar 13 globular cluster. The tails are aligned with the proper motion of Palomar 13 and are consistent with its old, metal-poor stellar population. We identify three RR Lyrae stars (RRLs) that are plausibly associated with the tails, in addition to four previously known in the cluster. From these RRLs, we find that the mean distance to the cluster and tails is 23.6 ± 0.2 kpc and estimate the total (initial) luminosity of the cluster to be

, consistent with previous claims that its initial luminosity was higher than its current luminosity. Combined with previously determined proper motion and radial velocity measurements of the cluster, we find that Palomar 13 is on a highly eccentric orbit (e ∼ 0.8) with a pericenter of ∼9 kpc and an apocenter of ∼69 kpc, and a recent pericentric passage of the cluster ∼75 Myr ago. We note a prominent linear structure in the interstellar dust map that runs parallel to the candidate tidal features, but conclude that reddening due to dust is unlikely to account for the structure that we observe. If confirmed, the Palomar 13 stellar stream would be one of very few streams with a known progenitor system, making it uniquely powerful for studying the disruption of globular clusters, the formation of the stellar halo, and the distribution of matter within our Galaxy.
Small-scale Magnetic Flux Ropes in the First Two Parker Solar Probe Encounters
Authors: Chen Yu , Hu Qiang , Zhao Lingling , Kasper Justin C. , Bale Stuart D. , Korreck Kelly E. , Case Anthony W. , Stevens Michael L. , Bonnell John W. , Goetz Keith , Harvey Peter R. , Klein Kristopher G. , Larson Davin E. , Livi Roberto , MacDowall Robert J. , Malaspina David M. , Pulupa Marc , Whittlesey Phyllis L. 
Published: November 2020

Abstract
Small-scale magnetic flux ropes (SFRs) are a type of structure in the solar wind that possess helical magnetic field lines. In a recent report we presented the radial variations of the properties of SFRs from 0.29 to 8 au using in situ measurements from the Helios, Advanced Composition Explorer/WIND (ACE/Wind), Ulysses, and Voyager spacecrafts. With the launch of the Parker Solar Probe (PSP), we extend our previous investigation further into the inner heliosphere. We apply a Grad–Shafranov-based algorithm to identify SFRs during the first two PSP encounters. We find that the number of SFRs detected near the Sun is much less than at larger radial distances, where magnetohydrodynamic (MHD) turbulence may act as the local source to produce these structures. The prevalence of Alfvénic structures significantly suppresses the detection of SFRs at closer distances. We compare the SFR event list with other event identification methods, yielding a dozen well-matched events. The cross-section maps of two selected events confirm the cylindrical magnetic flux-rope configuration. The power-law relation between the SFR magnetic field and heliocentric distances seems to hold down to 0.16 au.
On the Correlation between L Dwarf Optical and Infrared Variability and Radio Aurorae
Authors: Richey-Yowell Tyler , Kao Melodie M. , Pineda J. Sebastian , Shkolnik Evgenya L. , Hallinan Gregg 
Published: November 2020

Abstract
Photometric variability attributed to cloud phenomena is common in L/T transition brown dwarfs. Recent studies show that such variability may also trace aurorae, suggesting that localized magnetic heating may contribute to observed brown dwarf photometric variability. We assess this potential correlation with a survey of 17 photometrically variable brown dwarfs using the Karl G. Jansky Very Large Array at 4–8 GHz. We detect quiescent and highly circularly polarized flaring emission from one source, 2MASS J17502484-0016151, which we attribute to auroral electron cyclotron maser emission. The detected auroral emission extends throughout the frequency band at ∼5–25σ, and we do not detect evidence of a cutoff. Our detection confirms that 2MASS J17502484-0016151 hosts a magnetic field strength of ≥2.9 kG, similar to those of other radio-bright ultracool dwarfs. We show that Hα emission continues to be an accurate tracer of auroral activity in brown dwarfs. Supplementing our study with data from the literature, we calculate the occurrence rates of quiescent emission in L dwarfs with low- and high-amplitude variability and conclude that high-amplitude optical and infrared variability does not trace radio magnetic activity in L dwarfs.
Progenitors of Type IIb Supernovae. II. Observable Properties
Authors: Sravan Niharika , Marchant Pablo , Kalogera Vassiliki , Milisavljevic Dan , Margutti Raffaella 
Published: November 2020

Abstract
Type IIb supernovae (SNe IIb) present a unique opportunity for investigating the evolutionary channels and mechanisms governing the evolution of stripped-envelope SN progenitors due to a variety of observational constraints. Comparison of these constraints with the full distribution of theoretical properties not only helps determine the prevalence of observed properties in nature, but can also reveal currently unobserved populations. In this follow-up paper, we use the large grid of models presented in Sravan et al. to derive distributions of single and binary SNe IIb progenitor properties and compare them to constraints from three independent observational probes: multiband SN light curves, direct progenitor detections, and X-ray/radio observations. Consistent with previous work, we find that while current observations exclude single stars as SN IIb progenitors, SN IIb progenitors in binaries can account for them. We also find that the distributions indicate the existence of an unobserved dominant population of binary SNe IIb at low metallicity that arise due to mass transfer initiated on the Hertzsprung Gap. In particular, our models indicate the existence of a group of highly stripped (envelope mass ∼0.1–0.2M
☉) progenitors that are compact (<50R
☉) and blue (T
eff ≲ 105 K) with ∼104.5–105.5
L
☉ and low-density circumstellar mediums. As discussed in Sravan et al., this group is necessary to account for SN IIb fractions and likely exist regardless of metallicity. The detection of the unobserved populations indicated by our models would support weak stellar winds and inefficient mass transfer in SN IIb progenitors.
Black Hole Mergers from Hierarchical Triples in Dense Star Clusters
Authors: Martinez Miguel A. S. , Fragione Giacomo , Kremer Kyle , Chatterjee Sourav , Rodriguez Carl L. , Samsing Johan , Ye Claire S. , Weatherford Newlin C. , Zevin Michael , Naoz Smadar , Rasio Frederic A. 
Published: November 2020

Abstract
Hierarchical triples are expected to be produced by the frequent binary-mediated interactions in the cores of globular clusters. In some of these triples, the tertiary companion can drive the inner binary to merger following large eccentricity oscillations, as a result of the eccentric Kozai–Lidov mechanism. In this paper, we study the dynamics and merger rates of black hole (BH) hierarchical triples, formed via binary–binary encounters in the CMC Cluster Catalog, a suite of cluster simulations with present-day properties representative of the Milky Way’s globular clusters. We compare the properties of the mergers from triples to the other merger channels in dense star clusters, and show that triple systems do not produce significant differences in terms of mass and effective spin distribution. However, they represent an important pathway for forming eccentric mergers, which could be detected by LIGO–Virgo/KAGRA (LVK), and future missions such as LISA and the DECi-hertz Interferometer Gravitational wave Observatory. We derive a conservative lower limit for the merger rate from this channel of 0.35 Gpc−3 yr−1 in the local universe and up to

∼
9
%

of these events may have a detectable eccentricity at LVK design sensitivity. Additionally, we find that triple systems could play an important role in retaining second-generation BHs, which can later merge again in the core of the host cluster.
Supernova X-Ray Database (SNaX) Updated to Ensure Long-term Stability
Authors: Nisenoff Alexandra , Dwarkadas Vikram V. , Ross Mathias C. 
Published: November 2020

Abstract
The Supernova X-Ray Database was established a few years ago to make X-ray data on supernovae (SNe) publicly available via an elegant searchable web interface. The database has recently been updated to PhP7, had security updates done, and moved to a new server, ensuring its long-term stability. We urge astronomers to continue to download the data as needed for their work. Those with X-ray data on SNe are requested to upload it to the database via the easily fillable spreadsheet, making it accessible to everyone.
Evidence That HR 6990 Is a Spectroscopic Binary Hosting a Chemically Peculiar Late B-type star
Authors: Monier Richard 
Published: November 2020

Abstract
The archival IUE spectra of the late B giant HR 6990 are used to show that the absorption lines undergo large radial velocity variations in 2 spectra taken 4 months and 10 days apart. These large RV variations confirm that HR 6990 is a spectroscopic binary. The detection of strong lines of P ii, Ga ii, Ga iii and Hg ii show that the brightest member of the system, HR 6990 A, is not a normal late B-type giant but a newly discovered Chemically Peculiar star, probably a phosphorus and gallium enriched main sequence star. The two high resolution IUE spectra do not allow us to elucidate the nature of the companion, HR 6990 B.
A new freshwater snail (Gastropoda, Pomatiopsidae) endemic to Fuxian Lake (Yunnan, China) identified, based on morphological and DNA evidence
Authors: Shi Ling , Shu Yu , Qiang Chen , Xu Ping , Tian Ying , Chang Yaqing 
Published: November 2020

LacunopsisDeshayes, 1876 is restricted to South Asia and shows a remarkable regional distribution. Fifteen species have been reported from the lower Mekong River area of Laos, Cambodia, Thailand and Vietnam. Two species,Lacunopsis aurisY.-Y. Liu, Y.-X. Wang &amp; W.-Z. Zhang, 1980 andL. yunnanensisY.-Y. Liu, Y.-X. Wang &amp; W.-Z. Zhang, 1980 occur in the Yunnan Province of China. The most recent treatments ofLacunopsisdate back to the 1970s and 1980s, therefore detailed information on anatomy and DNA analysis is lacking.A new species of freshwater snail (Gastropoda, Pomatiopsidae),L. yuxiensissp. nov., is described, based on samples collected from Fuxian Lake (Yunnan, China). The new species is characterised by a solid and dark red shell with yellow spiral ribs on the whorls, reminiscent of marine gastropods of the family Trochidae. In addition to a description of the shell morphology and radula, molecular data are presented for the first time. This compilation of faunal and taxonomic data provides relevant information for use in conservation efforts. Additional molecular data may prove helpful for both reﬁning current knowledge on the morphological variability within this species and verifying the degree of cryptic diversity of this genus.