bluuebunny/crossref_metadata_2025_split huggingface dataset:
Risk of brain herniation after craniotomy with lumbar spinal drainage: a propensity score analysis
Authors: Motoyama Yasushi , Nakajima Tsukasa , Takamura Yoshiaki , Nakazawa Tsutomu , Wajima Daisuke , Takeshima Yasuhiro , Matsuda Ryosuke , Tamura Kentaro , Yamada Shuichi , Yokota Hiroshi , Nakagawa Ichiro , Nishimura Fumihiko , Park Young-Su , Nakamura Mitsutoshi , Nakase Hiroyuki 
Published: June 2018

OBJECTIVELumbar spinal drainage (LSD) during neurosurgery can have an important effect by facilitating a smooth procedure when needed. However, LSD is quite invasive, and the pathology of brain herniation associated with LSD has become known recently. The objective of this study was to determine the risk of postoperative brain herniation after craniotomy with LSD in neurosurgery overall.METHODSIncluded were 239 patients who underwent craniotomy with LSD for various types of neurological diseases between January 2007 and December 2016. The authors performed propensity score matching to establish a proper control group taken from among 1424 patients who underwent craniotomy and met the inclusion criteria during the same period. The incidences of postoperative brain herniation between the patients who underwent craniotomy with LSD (group A, n = 239) and the matched patients who underwent craniotomy without LSD (group B, n = 239) were compared.RESULTSBrain herniation was observed in 24 patients in group A and 8 patients in group B (OR 3.21, 95% CI 1.36–8.46, p = 0.005), but the rate of favorable outcomes was higher in group A (OR 1.79, 95% CI 1.18–2.76, p = 0.005). Of the 24 patients, 18 had uncal herniation, 5 had central herniation, and 1 had uncal and subfalcine herniation; 8 patients with other than subarachnoid hemorrhage were included. Significant differences in the rates of deep approach (OR 5.12, 95% CI 1.8–14.5, p = 0.002) and temporal craniotomy (OR 10.2, 95% CI 2.3–44.8, p = 0.002) were found between the 2 subgroups (those with and those without herniation) in group A. In 5 patients, brain herniation proceeded even after external decompression (ED). Cox regression analysis revealed that the risk of brain herniation related to LSD increased with ED (hazard ratio 3.326, 95% CI 1.491–7.422, p < 0.001). Among all 1424 patients, ED resulted in progression or deterioration of brain herniation more frequently in those who underwent LSD than it did in those who did not undergo LSD (OR 9.127, 95% CI 1.82–62.1, p = 0.004).CONCLUSIONSBrain herniation downward to the tentorial hiatus is more likely to occur after craniotomy with LSD than after craniotomy without LSD. Using a deep approach and craniotomy involving the temporal areas are risk factors for brain herniation related to LSD. Additional ED would aggravate brain herniation after LSD. The risk of brain herniation after placement of a lumbar spinal drain during neurosurgery must be considered even when LSD is essential.
Complications following pediatric cranioplasty after decompressive craniectomy: a multicenter retrospective study
Authors: Rocque Brandon G. , Agee Bonita S. , Thompson Eric M. , Piedra Mark , Baird Lissa C. , Selden Nathan R. , Greene Stephanie , Deibert Christopher P. , Hankinson Todd C. , Lew Sean M. , Iskandar Bermans J. , Bragg Taryn M. , Frim David , Grant Gerald , Gupta Nalin , Auguste Kurtis I. , Nikas Dimitrios C. , Vassilyadi Michael , Muh Carrie R. , Wetjen Nicholas M. , Lam Sandi K. 
Published: June 2018

OBJECTIVEIn children, the repair of skull defects arising from decompressive craniectomy presents a unique set of challenges. Single-center studies have identified different risk factors for the common complications of cranioplasty resorption and infection. The goal of the present study was to determine the risk factors for bone resorption and infection after pediatric cranioplasty.METHODSThe authors conducted a multicenter retrospective case study that included all patients who underwent cranioplasty to correct a skull defect arising from a decompressive craniectomy at 13 centers between 2000 and 2011 and were less than 19 years old at the time of cranioplasty. Prior systematic review of the literature along with expert opinion guided the selection of variables to be collected. These included: indication for craniectomy; history of abusive head trauma; method of bone storage; method of bone fixation; use of drains; size of bone graft; presence of other implants, including ventriculoperitoneal (VP) shunt; presence of fluid collections; age at craniectomy; and time between craniectomy and cranioplasty.RESULTSA total of 359 patients met the inclusion criteria. The patients’ mean age was 8.4 years, and 51.5% were female. Thirty-eight cases (10.5%) were complicated by infection. In multivariate analysis, presence of a cranial implant (primarily VP shunt) (OR 2.41, 95% CI 1.17–4.98), presence of gastrostomy (OR 2.44, 95% CI 1.03–5.79), and ventilator dependence (OR 8.45, 95% CI 1.10–65.08) were significant risk factors for cranioplasty infection. No other variable was associated with infection.Of the 240 patients who underwent a cranioplasty with bone graft, 21.7% showed bone resorption significant enough to warrant repeat surgical intervention. The most important predictor of cranioplasty bone resorption was age at the time of cranioplasty. For every month of increased age the risk of bone flap resorption decreased by 1% (OR 0.99, 95% CI 0.98–0.99, p < 0.001). Other risk factors for resorption in multivariate models were the use of external ventricular drains and lumbar shunts.CONCLUSIONSThis is the largest study of pediatric cranioplasty outcomes performed to date. Analysis included variables found to be significant in previous retrospective reports. Presence of a cranial implant such as VP shunt is the most significant risk factor for cranioplasty infection, whereas younger age at cranioplasty is the dominant risk factor for bone resorption.
Mediterranean Diet, Its Components, and Amyloid Imaging Biomarkers
Authors: Vassilaki Maria , Aakre Jeremiah A. , Syrjanen Jeremy A. , Mielke Michelle M. , Geda Yonas E. , Kremers Walter K. , Machulda Mary M. , Alhurani Rabe E. , Staubo Sara C. , Knopman David S. , Petersen Ronald C. , Lowe Val J. , Jack Clifford R. , Roberts Rosebud O. 
Published: June 2018

Background: There is accumulating evidence suggesting that diet may play a role in preventing or delaying cognitive decline and dementia, but the underlying biological mechanisms are not well understood. Objectives: To examine the cross-sectional associations of the Mediterranean diet (MeDi) and its components with 11C-PiB-PET scan measures of amyloid-β (Aβ) deposition. Methods: The study consisted of 278 Mayo Clinic Study of Aging participants 70+ years old, who were cognitively unimpaired (CU) at the time of completion of the Food Frequency Questionnaire (FFQ) and when they underwent PET imaging. Adherence to the MeDi was assessed by computing the MeDi score for each participant. All scans were performed after the FFQ completion; median [IQR] time between FFQ and Aβ PET was 3.5 (1.4) years. Z-scores were created for component, macro- and micronutrients measured. Linear and logistic regression models were adjusted for age, sex, education, apolipoprotein E (APOE) ɛ4 allele carrier status, time interval between the FFQ completion and PET scan, and total energy intake. Results: Participants’ median age at FFQ was 77.7 years (55.8% men; 26.6% with an APOE ɛ4 allele). Higher MeDi score (linear regression slope (beta):–0.035, p = 0.012; per standard deviation increase), vegetable intake (beta:–0.043, p = 0.002), intake of vitamin A (beta:–0.041, p = 0.003) or β-carotene (beta: –0.039, p = 0.005) from food sources and moderate alcohol consumption (beta: –0.074, p = 0.03) were associated with lower 11C-PiB standardized uptake value ratio. Conclusion: Findings are consistent with previous studies suggesting that higher adherence to a MeDi pattern and higher vegetable consumption are associated with better neuroimaging biomarker profile. Prospective studies are needed to validate current findings.
Improvement in upper-limb UPDRS motor scores following fast-paced arm exercise: A pilot study
Authors: Levy-Tzedek Shelly , Arbelle Dan , Forman Dan , Zlotnik Yair 
Published: June 2018

Background: The symptoms of patients with Parkinson’s disease (PD) have been shown to improve when they perform fast-paced rhythmic cycling movements with their lower limbs. Objective: Our goal in this pilot experiment was to test the feasibility and the benefits of a short exercise program involving fast-paced rhythmic movements of the upper limb for patients with PD. Methods: We used an experimental procedure that elicits large, fast-paced movements by the participants without the direct instructions to do so by the experimenter. Ten participants with PD (71.0±6.5 years old) performed a 50-min fast-paced rhythmic exercise of the upper limb after withdrawal from PD medication for at least 12 hours. Results: Participants improved their kinematic performance, in terms of accuracy and combined speed and amplitude ( p < 0.02), as well as their upper-limb MDS-UPDRS motor scores ( p = 0.023). Conclusions: The results demonstrate the feasibility of using the described apparatus to perform an exercise session of approximately 50 min with both arms, and give a preliminary indication of the potential benefit of such an exercise program.
Kinematic and kinetic benefits of implantable peroneal nerve stimulation in people with post-stroke drop foot using an ankle-foot orthosis
Authors: Berenpas Frank , Schiemanck Sven , Beelen Anita , Nollet Frans , Weerdesteyn Vivian , Geurts Alexander 
Published: June 2018

Background: Contralesional ‘drop foot’ after stroke is usually treated with an ankle-foot orthosis (AFO). However, AFOs may hamper ankle motion during stance. Peroneal functional electrical stimulation (FES) is an alternative treatment that provides active dorsiflexion and allows normal ankle motion. Despite this theoretical advantage of FES, the kinematic and kinetic differences between AFO and FES have been scarcely investigated. Objective: To test whether walking with implanted FES leads to improvements in stance stability, propulsion, and swing initiation compared to AFO. Methods: A 4-channel peroneal nerve stimulator (ActiGait ®) was implanted in 22 chronic patients after stroke. Instrumented gait analyses were performed during comfortable walking up to 26 weeks ( n = 10) or 52 weeks ( n = 12) after FES-system activation. Kinematics of knee and ankle (stance and swing phase) and kinetics (stance phase) of gait were determined, besides spatiotemporal parameters. Finally, we determined whether differences between devices regarding late stance kine(ma)tics correlated with those regarding the swing phase. Results: In mid-stance, knee stability improved as the peak knee extension velocity was lower with FES (β = 18.1°/s, p = 0.007), while peak ankle plantarflexion velocity (β = –29.2°/s, p = 0.006) and peak ankle plantarflexion power (β = –0.2 W/kg, p = 0.018) were higher with FES compared to AFO. With FES, the ground reaction force (GRF) vector at peak ankle power (i.e., ‘propulsion’) was oriented more anteriorly (β = –1.1°, p = 0.001). Similarly, the horizontal GRF (β = –0.8% body mass, p = 0.003) and gait speed (β = 0.03 m/s, p = 0.015) were higher. An increase in peak ankle plantarflexion velocity and a more forward oriented GRF angle during late stance were moderately associated with an increase in hip flexion velocity during initial swing (rs = 0.502, p = 0.029 and rs = 0.504, p = 0.028, respectively). Conclusions: This study substantiates the evidence that implantable peroneal FES as a treatment for post-stroke drop foot may be superior over AFO in terms of knee stability, ankle plantarflexion power, and propulsion.
Unconfirmed Near-Earth Objects
Authors: Vereš Peter , Payne Matthew J. , Holman Matthew J. , Farnocchia Davide , Williams Gareth V. , Keys Sonia , Boardman Ian 
Published: June 2018

Abstract
We studied the Near-Earth Asteroid (NEA) candidates posted on the Minor Planet Center’s Near-Earth Object Confirmation Page (NEOCP) between years 2013 and 2016. Out of more than 17000 NEA candidates, while the majority became either new discoveries or were associated with previously known objects, about 11% were unable to be followed-up or confirmed. We further demonstrate that of the unconfirmed candidates, 926 ± 50 are likely to be NEAs, representing 18% of discovered NEAs in that period. Only 11% (∼93) of the unconfirmed NEA candidates were large (having absolute magnitude H < 22). To identify the reasons why these NEAs were not recovered, we analyzed those from the most prolific asteroid surveys: Pan-STARRS, the Catalina Sky Survey, the Dark Energy Survey, and the Space Surveillance Telescope. We examined the influence of plane-of-sky positions and rates of motion, brightnesses, submission delays, and computed absolute magnitudes, as well as correlations with the phase of the moon and seasonal effects. We find that delayed submission of newly discovered NEA candidate to the NEOCP drove a large fraction of the unconfirmed NEA candidates. A high rate of motion was another significant contributing factor. We suggest that prompt submission of suspected NEA discoveries and rapid response to fast-moving targets and targets with fast growing ephemeris uncertainty would allow better coordination among dedicated follow-up observers, decrease the number of unconfirmed NEA candidates, and increase the discovery rate of NEAs.
Ultra-dense Broad-line Region Scale Outflow in Highly Reddened Quasar SDSS J145057.28+530007.6
Authors: Zhang Shaohua , Zhou Hongyan , Shi Xiheng , Pan Xiang , Ji Tuo , Jiang Peng 
Published: June 2018

Abstract
We report the discovery of highly reddening and hydrogen Balmer and metastable helium broad absorption lines in the quasar SDSS J145057.28+530007.6, based on the optical and near-infrared spectra taken from the SDSS-III/BOSS and the TripleSpec observations. The nuclear continuum, Balmer decrement, and absorption-line depth analyses suggest that (1) the accretion disk is completely obscured and the covering factor of the broad-line region (BLR) is only 0.39 ± 0.03, (2) the power-law continuum is reddened by the SMC extinction law of E(B – V) =0.72 ± 0.01 mag and the dusty materials are mainly associated with Ca ii H and K rather than the Balmer and He i* absorption-line system, (3) the unsaturated Balmer (Hβ, Hγ, and Hδ) and He i* λ3889 absorption lines have the same two-Gaussian profiles as the shifts of −931 ± 33 and −499 ± 39 km s−1 and the widths of 121 ± 28 and 196 ± 37 km s−1, respectively. Constrained mutually by the Balmer, He i* absorption lines and undetected Fe ii* λ5169 in the photoionization simulations, the physical properties of the outflow gases are derived as follows: ionization parameter 10−1.4 ≲ U ≲ 10−0.8, density 108.2±0.4 ≲ n
H ≲ 109.0±0.4 cm−3, and column density 1022.0±0.2 ≲ N
H ≲ 1022.2–22.3 cm−2. We propose that the ultra-dense outflow gases appear in the vicinity of the surface of the BLR or are located at most 3.12 pc away from the engine. That probably implies that the outflow originates from the BLR, and this kind of ultra-dense BLR scale outflow gases can effectively test the physical properties of the outer gases of the BLR.
Constraints for the Progenitor Masses of Historic Core-collapse Supernovae
Authors: Williams Benjamin F. , Hillis Tristan J. , Murphy Jeremiah W. , Gilbert Karoline , Dalcanton Julianne J. , Dolphin Andrew E. 
Published: June 2018

Abstract
We age-date the stellar populations associated with 12 historic nearby core-collapse supernovae (CCSNe) and two supernova impostors; from these ages, we infer their initial masses and associated uncertainties. To do this, we have obtained new Hubble Space Telescope imaging covering these CCSNe. Using these images, we measure resolved stellar photometry for the stars surrounding the locations of the SNe. We then fit the color–magnitude distributions of this photometry with stellar evolution models to determine the ages of any young existing populations present. From these age distributions, we infer the most likely progenitor masses for all of the SNe in our sample. We find ages between 4 and 50 Myr, corresponding to masses from 7.5 to 59 solar masses. There were no SNe that lacked a local young population. Our sample contains four SNe Ib/c; their masses have a wide range of values, suggesting that the progenitors of stripped-envelope SNe are binary systems. Both impostors have masses constrained to be ≲7.5 solar masses. In cases with precursor imaging measurements, we find that age-dating and precursor imaging give consistent progenitor masses. This consistency implies that, although the uncertainties for each technique are significantly different, the results of both are reliable to the measured uncertainties. We combine these new measurements with those from our previous work and find that the distribution of 25 core-collapse SNe progenitor masses is consistent with a standard Salpeter power-law mass function, no upper mass cutoff, and an assumed minimum mass for core-collapse of 7.5 M
⊙. The distribution is consistent with a minimum mass <9.5 M
⊙.
The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. XV. The Dynamical Clock: Reading Cluster Dynamical Evolution from the Segregation Level of Blue Straggler Stars
Authors: Ferraro F. R. , Lanzoni B. , Raso S. , Nardiello D. , Dalessandro E. , Vesperini E. , Piotto G. , Pallanca C. , Beccari G. , Bellini A. , Libralato M. , Anderson J. , Aparicio A. , Bedin L. R. , Cassisi S. , Milone A. P. , Ortolani S. , Renzini A. , Salaris M. , van der Marel R. P. 
Published: June 2018

Abstract
The parameter A
+, defined as the area enclosed between the cumulative radial distribution of blue straggler stars (BSSs) and that of a reference population, is a powerful indicator of the level of BSS central segregation. As part of the Hubble Space Telescope UV Legacy Survey of Galactic globular clusters (GCs), here we present the BSS population and the determination of A
+ in 27 GCs observed out to about one half-mass radius. In combination with 21 additional clusters discussed in a previous paper, this provides us with a global sample of 48 systems (corresponding to ∼32% of the Milky Way GC population), for which we find a strong correlation between A
+ and the ratio of cluster age to the current central relaxation time. Tight relations have also been found with the core radius and the central luminosity density, which are expected to change with the long-term cluster dynamical evolution. An interesting relation is emerging between A
+ and the ratio of the BSS velocity dispersion relative to that of main sequence turn-off stars, which measures the degree of energy equipartition experienced by BSSs in the cluster. These results provide further confirmation that BSSs are invaluable probes of GC internal dynamics and that A
+ is a powerful dynamical clock.
Density Fluctuations in a Polar Coronal Hole
Authors: Hahn Michael , D’Huys Elke , Savin Daniel Wolf 
Published: June 2018

Abstract
We have measured the root-mean-square (rms) amplitude of intensity fluctuations, ΔI, in plume and interplume regions of a polar coronal hole. These intensity fluctuations correspond to density fluctuations. Using data from the Sun Watcher using the Active Pixel System detector and Image Processing on the Project for Onboard Autonomy
(Proba2), our results extend up to a height of about 1.35 R
⊙. One advantage of the rms analysis is that it does not rely on a detailed evaluation of the power spectrum, which is limited by noise levels to low heights in the corona. The rms approach can be performed up to larger heights where the noise level is greater, provided that the noise itself can be quantified. At low heights, both the absolute ΔI, and the amplitude relative to the mean intensity, ΔI/I, decrease with height. However, starting at about 1.2 R
⊙, ΔI/I increases, reaching 20%–40% by 1.35 R
⊙. This corresponds to density fluctuations of Δn
e/n
e ≈ 10%–20%. The increasing relative amplitude implies that the density fluctuations are generated in the corona itself. One possibility is that the density fluctuations are generated by an instability of Alfvén waves. This generation mechanism is consistent with some theoretical models and with observations of Alfvén wave amplitudes in coronal holes. Although we find that the energy of the observed density fluctuations is small, these fluctuations are likely to play an important indirect role in coronal heating by promoting the reflection of Alfvén waves and driving turbulence.
Probing Self-interacting Dark Matter with Disk Galaxies in Cluster Environments
Authors: Secco Lucas F. , Farah Amanda , Jain Bhuvnesh , Adhikari Susmita , Banerjee Arka , Dalal Neal 
Published: June 2018

Abstract
Self-interacting dark matter (SIDM) has long been proposed as a solution to small-scale problems posed by standard cold dark matter. We use numerical simulations to study the effect of dark matter interactions on the morphology of disk galaxies falling into galaxy clusters. The effective drag force on dark matter leads to offsets of the stellar disk with respect to the surrounding halo, causing distortions in the disk. For anisotropic scattering cross sections of 0.5 and

, we show that potentially observable warps, asymmetries, and thickening of the disk occur in simulations. We discuss observational tests of SIDM with galaxy surveys and more realistic simulations needed to obtain detailed predictions.
ELUCID. V. Lighting Dark Matter Halos with Galaxies
Authors: Yang Xiaohu , Zhang Youcai , Wang Huiyuan , Liu Chengze , Lu Tianhuan , Li Shijie , Shi Feng , Jing Y. P. , Mo H. J. , Bosch Frank C. van den , Kang Xi , Cui Weiguang , Guo Hong , Li Guoliang , Lim S. H. , Lu Yi , Luo Wentao , Wei Chengliang , Yang Lei 
Published: June 2018

Abstract
In a recent study, using the distribution of galaxies in the north galactic pole of the SDSS DR7 region enclosed in a 500

box, we carried out our ELUCID simulation (ELUCID III). Here, we light the dark matter halos and subhalos in the reconstructed region in the simulation with galaxies in the SDSS observations using a novel neighborhood abundance matching method. Before we make use of the galaxy–subhalo connections established in the ELUCID simulation to evaluate galaxy formation models, we set out to explore the reliability of such a link. For this purpose, we focus on the following few aspects of galaxies: (1) the central–subhalo luminosity and mass relations, (2) the satellite fraction of galaxies, (3) the conditional luminosity function (CLF) and conditional stellar mass function (CSMF) of galaxies, and (4) the cross-correlation functions between galaxies and dark matter particles, most of which are measured separately for all, red, and blue galaxy populations. We find that our neighborhood abundance matching method accurately reproduces the central–subhalo relations, satellite fraction, and the CLFs, CSMFs, and biases of galaxies. These features ensure that galaxy–subhalo connections thus established will be very useful in constraining galaxy formation processes. We provide some suggestions for the three levels of using the galaxy–subhalo pairs for galaxy formation constraints. The galaxy–subhalo links and the subhalo merger trees in the SDSS DR7 region extracted from our ELUCID simulation are available upon request.