bluuebunny/crossref_metadata_2025_split huggingface dataset:
A Systematic Review and Aggregated Analysis on the Impact of Amyloid PET Brain Imaging on the Diagnosis, Diagnostic Confidence, and Management of Patients being Evaluated for Alzheimer’s Disease
Authors: Fantoni Enrico R. , Chalkidou Anastasia , O’ Brien John T. , Farrar Gill , Hammers Alexander 
Published: April 2018

Background: Amyloid PET (aPET) imaging could improve patient outcomes in clinical practice, but the extent of impact needs quantification. Objective: To provide an aggregated quantitative analysis of the value added by aPET in cognitively impaired subjects. Methods: Systematic literature searches were performed in Embase and Medline until January 2017. 1,531 cases over 12 studies were included (1,142 cases over seven studies in the primary analysis where aPET was the key biomarker; the remaining cases included as defined groups in the secondary analysis). Data was abstracted by consensus among two observers and assessed for bias. Clinical utility was measured by diagnostic change, diagnostic confidence, and patient management before and after aPET. Three groups were further analyzed: control patients for whom feedback of aPET scan results was delayed; aPET Appropriate Use Criteria (AUC+) cases; and patients undergoing additional FDG/CSF testing. Results: For 1,142 cases with only aPET, 31.3% of diagnoses were revised, whereas 3.2% of diagnoses changed in the delayed aPET control group ( p < 0.0001). Increased diagnostic confidence following aPET was found for 62.1% of 870 patients. Management changes with aPET were found in 72.2% of 740 cases and in 55.5% of 299 cases in the control group ( p < 0.0001). The diagnostic value of aPET in AUC+ patients or when FDG/CSF were additionally available did not substantially differ from the value of aPET alone in the wider population. Conclusions: Amyloid PET contributed to diagnostic revision in almost a third of cases and demonstrated value in increasing diagnostic confidence and refining management plans.
Diabetic macular edema grading in retinal images using vector quantization and semi-supervised learning
Authors: Ren Fulong , Cao Peng , Zhao Dazhe , Wan Chao 
Published: April 2018

BACKGROUND: Diabetic macular edema (DME) is one of the severe complication of diabetic retinopathy causing severe vision loss and leads to blindness in severe cases if left untreated. OBJECTIVE: To grade the severity of DME in retinal images. METHODS: Firstly, the macular is localized using its anatomical features and the information of the macula location with respect to the optic disc. Secondly, a novel method for the exudates detection is proposed. The possible exudate regions are segmented using vector quantization technique and formulated using a set of feature vectors. A semi-supervised learning with graph based classifier is employed to identify the true exudates. Thirdly, the disease severity is graded into different stages based on the location of exudates and the macula coordinates. RESULTS: The results are obtained with the mean value of 0.975 and 0.942 for accuracy and F1-scrore, respectively. CONCLUSION: The present work contributes to macula localization, exudate candidate identification with vector quantization and exudate candidate classification with semi-supervised learning. The proposed method and the state-of-the-art approaches are compared in terms of performance, and experimental results show the proposed system overcomes the challenge of the DME grading and demonstrate a promising effectiveness.
Rotation of Low-mass Stars in Upper Scorpius and ρ Ophiuchus with K2
Authors: Rebull L. M. , Stauffer J. R. , Cody A. M. , Hillenbrand L. A. , David T. J. , Pinsonneault M. 
Published: April 2018

Abstract
We present an analysis of K2 light curves (LCs) for candidate members of the young Upper Sco (USco) association (∼8 Myr) and the neighboring ρ Oph embedded cluster (∼1 Myr). We establish ∼1300 stars as probable members, ∼80% of which are periodic. The phased LCs have a variety of shapes which can be attributed to physical causes ranging from stellar pulsation and stellar rotation to disk-related phenomena. We identify and discuss a number of observed behaviors. The periods are ∼0.2–30 days with a peak near 2 days and the rapid period end nearing breakup velocity. M stars in the young USco region rotate systematically faster than GK stars, a pattern also present in K2 data for the older Pleiades and Praesepe systems. At higher masses (types FGK), the well-defined period–color relationship for slowly rotating stars seen in the Pleiades and Praesepe systems is not yet present in USco. Circumstellar disks are present predominantly among the more slowly rotating M stars in USco, with few disks in the subday rotators. However, M dwarfs with disks rotate faster on average than FGK systems with disks. For four of these disked M dwarfs, we provide direct evidence for disk locking based on the K2 LC morphologies. Our preliminary analysis shows a relatively mass-independent spin-up by a factor of ∼3.5 between USco and the Pleiades, then mass-dependent spin-down between Pleiades and Praesepe.
The HOSTS Survey—Exozodiacal Dust Measurements for 30 Stars
Authors: Ertel S. , Defrère D. , Hinz P. , Mennesson B. , Kennedy G. M. , Danchi W. C. , Gelino C. , Hill J. M. , Hoffmann W. F. , Rieke G. , Shannon A. , Spalding E. , Stone J. M. , Vaz A. , Weinberger A. J. , Willems P. , Absil O. , Arbo P. , Bailey V. P. , Beichman C. , Bryden G. , Downey E. C. , Durney O. , Esposito S. , Gaspar A. , Grenz P. , Haniff C. A. , Leisenring J. M. , Marion L. , McMahon T. J. , Millan-Gabet R. , Montoya M. , Morzinski K. M. , Pinna E. , Power J. , Puglisi A. , Roberge A. , Serabyn E. , Skemer A. J. , Stapelfeldt K. , Su K. Y. L. , Vaitheeswaran V. , Wyatt M. C. 
Published: April 2018

Abstract
The Hunt for Observable Signatures of Terrestrial Systems survey searches for dust near the habitable zones (HZs) around nearby, bright main-sequence stars. We use nulling interferometry in the N band to suppress the bright stellar light and to probe for low levels of HZ dust around the 30 stars observed so far. Our overall detection rate is 18%, including four new detections, among which are the first three around Sun-like stars and the first two around stars without any previously known circumstellar dust. The inferred occurrence rates are comparable for early-type and Sun-like stars, but decrease from

% for stars with previously detected cold dust to

% for stars without such excess, confirming earlier results at higher sensitivity. For completed observations on individual stars, our sensitivity is five to ten times better than previous results. Assuming a lognormal excess luminosity function, we put upper limits on the median HZ dust level of 13 zodis (95% confidence) for a sample of stars without cold dust and of 26 zodis when focusing on Sun-like stars without cold dust. However, our data suggest that a more complex luminosity function may be more appropriate. For stars without detectable Large Binocular Telescope Interferometer (LBTI) excess, our upper limits are almost reduced by a factor of two, demonstrating the strength of LBTI target vetting for future exo-Earth imaging missions. Our statistics are limited so far, and extending the survey is critical to informing the design of future exo-Earth imaging surveys.
Far-ultraviolet Spectroscopy of Recent Comets with the Cosmic Origins Spectrograph on the Hubble Space Telescope
Authors: Feldman Paul D. , Weaver Harold A. , A’Hearn Michael F. , Combi Michael R. , Russo Neil Dello 
Published: April 2018

Abstract
Since its launch in 1990, the Hubble Space Telescope (HST) has served as a platform with unique capabilities for remote observations of comets in the far-ultraviolet region of the spectrum. Successive generations of imagers and spectrographs have seen large advances in sensitivity and spectral resolution enabling observations of the diverse properties of a representative number of comets during the past 25 years. To date, four comets have been observed in the far-ultraviolet by the Cosmic Origins Spectrograph (COS), the last spectrograph to be installed in HST, in 2009: 103P/Hartley 2, C/2009 P1 (Garradd), C/2012 S1 (ISON), and C/2014 Q2 (Lovejoy). COS has unprecedented sensitivity, but limited spatial information in its 2.″5 diameter circular aperture, and our objective was to determine the CO production rates from measurements of the CO Fourth Positive system in the spectral range of 1400–1700 Å. In the two brightest comets, 19 bands of this system were clearly identified. The water production rates were derived from nearly concurrent observations of the OH (0,0) band at 3085 Å by the Space Telescope Imaging Spectrograph. The derived CO/

production rate ratio ranged from ∼0.3% for Hartley 2 to ∼22% for Garradd. In addition, strong partially resolved emission features due to multiplets of S i, centered at 1429 Å and 1479 Å, and of C i at 1561 Å and 1657 Å, were observed in all four comets. Weak emission from several lines of the

Lyman band system, excited by solar Lyα and Lyβ pumped fluorescence, were detected in comet Lovejoy.
Ion Traps at the Sun: Implications for Elemental Fractionation
Authors: Fleishman Gregory D. , Musset Sophie , Bommier Véronique , Glesener Lindsay 
Published: April 2018

Abstract
Why the tenuous solar outer atmosphere, or corona, is much hotter than the underlying layers remains one of the greatest challenges for solar modeling. Detailed diagnostics of the coronal thermal structure come from extreme ultraviolet (EUV) emission. The EUV emission is produced by heavy ions in various ionization states and depends on the amount of these ions and on plasma temperature and density. Any nonuniformity of the elemental distribution in space or variability in time affects thermal diagnostics of the corona. Here we theoretically predict ionized chemical element concentrations in some areas of the solar atmosphere, where the electric current is directed upward. We then detect these areas observationally, by comparing the electric current density with the EUV brightness in an active region. We found a significant excess in EUV brightness in the areas with positive current density rather than negative. Therefore, we report the observational discovery of substantial concentrations of heavy ions in current-carrying magnetic flux tubes, which might have important implications for the elemental fractionation in the solar corona known as the first ionization potential effect. We call such areas of heavy ion concentration the “ion traps.” These traps hold enhanced ion levels until they are disrupted by a flare, whether large or small.
Suppression of AGN-driven Turbulence by Magnetic Fields in a Magnetohydrodynamic Model of the Intracluster Medium
Authors: Bambic Christopher J. , Morsony Brian J. , Reynolds Christopher S. 
Published: April 2018

Abstract
We investigate the role of active galactic nucleus (AGN) feedback in turbulent heating of galaxy clusters. Specifically, we analyze the production of turbulence by g-modes generated by the supersonic expansion and buoyant rise of AGN-driven bubbles. Previous work that neglects magnetic fields has shown that this process is inefficient, with less than 1% of the injected energy ending up in turbulence. This inefficiency primarily arises because the bubbles are shredded apart by hydrodynamic instabilities before they can excite sufficiently strong g-modes. Using a plane-parallel model of the intracluster medium (ICM) and 3D ideal magnetohydrodynamics (MHD) simulations, we examine the role of a large-scale magnetic field that is able to drape around these rising bubbles, preserving them from hydrodynamic instabilities. We find that while magnetic draping appears better able to preserve AGN-driven bubbles, the driving of g-modes and the resulting production of turbulence is still inefficient. The magnetic tension force prevents g-modes from transitioning into the nonlinear regime, suppressing turbulence in our model ICM. Our work highlights the ways in which ideal MHD is an insufficient description for the cluster feedback process, and we discuss future work such as the inclusion of anisotropic viscosity as a means of simulating high β plasma kinetic effects. These results suggest the hypothesis that other mechanisms of heating the ICM plasma such as sound waves or cosmic rays may be responsible for the observed feedback in galaxy clusters.
RATIR Follow-up of LIGO/Virgo Gravitational Wave Events
Authors: Golkhou V. Zach , Butler Nathaniel R. , Strausbaugh Robert , Troja Eleonora , Kutyrev Alexander , Lee William H. , Román-Zúñiga Carlos G. , Watson Alan M. 
Published: April 2018

Abstract
We have recently witnessed the first multi-messenger detection of colliding neutron stars through gravitational waves (GWs) and electromagnetic (EM) waves (GW 170817) thanks to the joint efforts of LIGO/Virgo and Space/Ground-based telescopes. In this paper, we report on the RATIR follow-up observation strategies and show the results for the trigger G194575. This trigger is not of astrophysical interest; however, it is of great interest to the robust design of a follow-up engine to explore large sky-error regions. We discuss the development of an image-subtraction pipeline for the six-color, optical/NIR imaging camera RATIR. Considering a two-band (i and r) campaign in the fall of 2015, we find that the requirement of simultaneous detection in both bands leads to a factor ∼10 reduction in false alarm rate, which can be further reduced using additional bands. We also show that the performance of our proposed algorithm is robust to fluctuating observing conditions, maintaining a low false alarm rate with a modest decrease in system efficiency that can be overcome utilizing repeat visits. Expanding our pipeline to search for either optical or NIR detections (three or more bands), considering separately the optical riZ and NIR YJH bands, should result in a false alarm rate ≈1% and an efficiency ≈90%. RATIR’s simultaneous optical/NIR observations are expected to yield about one candidate transient in the vast 100 deg2 LIGO error region for prioritized follow-up with larger aperture telescopes.
Discovery of a New Classical Nova Shell Around a Nova-like Cataclysmic Variable
Authors: Guerrero Martín A. , Sabin Laurence , Tovmassian Gagik , Santamaría Edgar , Michel Raul , Ramos-Larios Gerardo , Alarie Alexandre , Morisset Christophe , Bustamante Luis C. Bermúdez , González Chantal P. , Wright Nicholas J. 
Published: April 2018

Abstract
The morphology and optical spectrum of IPHASX J210204.7+471015, a nebula classified as a possible planetary nebula are, however, strikingly similar to those of AT Cnc, a classical nova shell around a dwarf nova. To investigate its true nature, we have obtained high-resolution narrowband [O iii] and [N ii] images and deep optical spectra. The nebula shows an arc of [N ii]-bright knots notably enriched in nitrogen, while an [O iii]-bright bow shock is progressing throughout the ISM. Diagnostic line ratios indicate that shocks are associated with the arc and bow shock. The central star of this nebula has been identified by its photometric variability. Time-resolved photometric and spectroscopic data of this source reveal a period of 4.26 hr, which is attributed to a binary system. The optical spectrum is notably similar to that of RW Sex, a cataclysmic variable star (CV) of the UX UMa nova-like (NL) type. Based on these results, we propose that IPHASX J210204.7 + 471015 is a classical nova shell observed around a CV-NL system in quiescence.
Estimating the Mass of the Milky Way Using the Ensemble of Classical Satellite Galaxies
Authors: Patel Ekta , Besla Gurtina , Mandel Kaisey , Sohn Sangmo Tony 
Published: April 2018

Abstract
High precision proper motion (PM) measurements are available for approximately 20% of all known dwarf satellite galaxies of the Milky Way (MW). Here we extend the Bayesian framework of Patel et al. to include all MW satellites with measured 6D phase-space information and apply it with the Illustris-Dark simulation to constrain the MW’s mass. Using the properties of each MW satellite individually, we find that the scatter among mass estimates is reduced when the magnitude of specific orbital angular momentum (j) is adopted, rather than their combined instantaneous positions and velocities. We also find that high j satellites (i.e., Leo II) constrain the upper limits for the MW’s mass and low j satellites, rather than the highest speed satellites (i.e., Leo I and Large Magellanic Cloud), set the lower mass limits. When j of all classical satellites is used to simultaneously estimate the MW’s mass, we conclude the halo mass is 0.85+0.23
−0.26 × 1012

(including Sagittarius dSph) and 0.96+0.29
−0.28 × 1012

(excluding Sagittarius dSph), cautioning that low j satellites on decaying orbits like Sagittarius dSph may bias the distribution. These estimates markedly reduce the current factor of two spread in the mass range of the MW. We also find a well-defined relationship between host halo mass and satellite j distribution, which yields the prediction that upcoming PMs for ultra-faint dwarfs should reveal j within 5 × 103–104 kpc km s−1. This is a promising method to significantly constrain the cosmologically expected mass range for the MW and eventually M31 as more satellite PMs become available.
La territorialisation du cyberespace : la fin de la mondialisation ?
Authors: de Lespinois Jérôme 
Published: April 2018

Hervé Coutau-Bégarie n’a pas spécifiquement réfléchi au cyberespace mais le processus actuel de territorialisation du cyberespace s’inscrit parfaitement dans le schéma décrit dans son ouvrage 2030, la fin de la mondialisation ? Cet article examine comment les États investissent le cyberespace pour y affirmer leur souveraineté. Il propose tout d’abord trois modèles théoriques de développement du cyberespace : libertarien, libéral ou westphalien. Puis, il montre comment le modèle westphalien prend l’ascendant sur le modèle libéral compte tenu du processus actuel de territorialisation des données numériques et de l’érection de frontières dans le cyberespace s’appuyant sur la territorialisation de l’infrastructure informationnelle.
Doubles explorations d’« identité (ipséité) » dans le cas de l’ Apologia pro vita sua
Authors: Kanno Kota 
Published: April 2018

Comment comprendre l’ Apologia pro vita sua de Newman ? Pour répondre à cette question, nous analysons cette œuvre au moyen de la notion ricœurienne d’ipséité. Cette notion, liée à celle d’identité narrative, permet d’élucider le motif rédactionnel de l’ Apologia en clarifiant sa cohérence, qui n’est pas formelle mais plutôt liée à un certain changement de vie. Par la suite, au moment où il réfléchit à sa conversion, une question s’impose à lui : comment comprendre le changement dans l’expression de la foi au sein de l’Église catholique ? C’est aussi une question d’identité, au sens non de « mêmeté », mais d’« ipséité ». Ainsi, dans l’ Apologia , il y a deux quêtes d’« ipséité » : par la narration, Newman recherche la cohérence substantielle de son parcours, avant de s’interroger sur la cohérence de l’Église catholique par le biais de l’« ipséité » du christianisme.
L’oubli du pluralisme dans la démocratie agonistique. Schmitt lu par Mouffe : une offensive manquée contre le libéralisme post-politique
Authors: Sommerer Erwan 
Published: April 2018

Nous démontrerons dans cet article l’échec de l’usage chez Chantal Mouffe de certains concepts de Carl Schmitt à des fins de contestation de la tendance post-politique du libéralisme. Plus précisément, nous constaterons que les carences que Mouffe dénonce dans la pensée libérale se retrouvent dans sa propre théorie de la démocratie agonistique : malgré ses attaques contre Rawls, cette philosophe met en œuvre une même tentative de neutralisation consensualiste du politique au profit d’un modèle de société anti-pluraliste d’où le conflit est évacué. Nous nous demanderons alors pour finir en quoi cet échec nous renseigne sur le prix à payer pour accomplir jusqu’au bout le geste théorique entamé par Mouffe, mais demeuré inachevé, pour réintroduire le politique dans l’espace public.
Comparative Evaluation of Standard ILM Peel With Inverted ILM Flap Technique In Large Macular Holes: A Prospective, Randomized Study
Authors: Manasa S. , Kakkar Prateek , Kumar Atul , Chandra Parijat , Kumar Vinod , Ravani Raghav 
Published: April 2018

BACKGROUND AND OBJECTIVE:
To compare the outcomes of inverted internal limiting membrane (ILM) flap technique (IFT) with the standard ILM peel (SIP) for large macular holes (MHs).

PATIENTS AND METHODS:
This is a prospective, randomized study in which 100 patients with idiopathic MHs with minimum linear dimension of 600 μm or greater were recruited. Group 1 underwent SIP and group 2 underwent IFT. Best-corrected visual acuity (BCVA), type of MH closure, and multifocal electroretinogram (mfERG) were evaluated at presentation, 1 week, 1 month, and 3 months postoperatively.

RESULTS:

Mean postoperative BCVA was 0.86 ± 0.19 in group 1 and 0.67 ± 0.3 in group 2 at 3 months postoperatively (
P
= .001). Type 1 closure was observed in 34.04% of patients in group 1 and in 62.79% of patients in group 2 (
P
= .02). mfERG showed improvement in both groups.

CONCLUSION:
IFT provides superior outcomes compared to SIP and, hence, could be considered as the surgical modality of choice in large MH.

[
Ophthalmic Surg Lasers Imaging Retina
. 2018;49:236–240.]
The hedonic valuation of South African wine brands
Authors: Priilaid D. , Van Rensburg P. 
Published: April 2018

Working with a set of 35 South African wine brands identified in Priilaid and Van Rensburg (2010a), this study presents two brand valuation techniques that combine non-ordinal wine valuation models with conventional methods of valuation. The first price-premium approach defines brand equity value as the difference between a wine’s price and a valuation of its intrinsic worth. The second quality premium approach defines brand equity value as the difference between a wine’s intrinsic value and, instead of price, the value of its perceived quality when sampled sighted. With a set of assumptions regarding consistency in future wine quality, hectorage, price premiums, and sales volumes, brand valuations for each method are calculated as the net present value of the brand premiums paid per unit over the total cases sold. The consequent computations reveal how the price-premium method realises a mean valuation three times greater than the average derived from the alternate quality premium method. This difference is attributed to extreme valuations noted at either end of the price-premium sample, and suggests that this method is perhaps less conservative than perceived quality premium-based valuations. Additionally, the specification of perpetuity is observed to be too extreme. Alternate time scenarios are considered, with a period of ten years posited as perhaps more appropriate to such computations.
Does service innovation matter? An empirical study on market orientation and supply chain performance
Authors: Cheng T-Y. D.J. , Chen C-H. V. 
Published: April 2018

The objective of this study was to explore how firm service innovation mediates market orientation and business performance. This paper begins with a literature review indicating the themes from which we developed our conceptual framework. Structural equation modeling based on a cross-section (n = 260) of 5 years of supply chain business data (2009–2013) in Greater China was conducted. We concluded that firm market orientation and service innovation exert significantly positive effects on business performance. In addition, the results supported our model that market orientation is mediated by the effect of service innovation on business performance. Market orientation and service innovation had a stronger combined effect on business performance than market orientation alone did. This paper provides implications for how firms can be more effectively synergized amid challenges and gain a competitive advantage in the global supply chain.