bluuebunny/crossref_metadata_2025_split huggingface dataset:
Short- and long-term effects of selective dorsal rhizotomy on gross motor function in ambulatory children with spastic diplegia
Authors: van Schie Petra E. M. , Schothorst Maaike , Dallmeijer Annet J. , Vermeulen R. Jeroen , van Ouwerkerk Willem J. R. , Strijers Rob L. M. , Becher Jules G. 
Published: December 2016

Object
The primary aim of this prospective cohort study was to evaluate the short-term (1 year) and long-term (mean 6 years) effects of selective dorsal rhizotomy (SDR) on gross motor function and spasticity in ambulatory children with spastic diplegia. Secondary aims were to investigate side effects, additional treatment during follow-up (botulinum toxin type A injections or orthopedic surgery), and parental satisfaction.

Methods
Thirty-three children who had undergone SDR at a mean age of 6 years and 7 months (± 2 years) were included. There were 7 children at Gross Motor Function Classification System (GMFCS) Level I, 7 at Level II, and 19 at Level III. Gross motor function was assessed with the Gross Motor Function Measure–66 (GMFM-66). Spasticity was measured according to a modified Tardieu scale. Side effects, additional treatment, and parental satisfaction were recorded using a parental questionnaire and medical records.

Results
At 1-year follow-up, mean GMFM-66 scores improved significantly by 4.3 ± 4.1 points. Children at GMFCS Levels I and II showed significantly more improvement (7.2 points) on the GMFM-66 compared with children at GMFCS Level III (2.9 points). On long-term follow-up (mean 6 years ± 22 months), mean GMFM-66 scores improved significantly by 6.5 ± 5.9 points, without a difference between children at GMFCS Levels I and II and Level III. No relapse of spasticity was noted. Ten children (30%) needed orthopedic surgery and 13 children (39%) received botulinum toxin type A treatment after SDR. Twenty (91%) of the 22 parents who answered the questionnaire at long-term follow-up believed that their child's functioning had improved after SDR.

Conclusions
Selective dorsal rhizotomy resulted in short- and long-term improvements in gross motor function, without relapse of spasticity. However, the majority of the children still needed additional surgery or botulinum toxin A treatment.
Rapid online language mapping with electrocorticography
Authors: Miller Kai J. , Abel Taylor J. , Hebb Adam O. , Ojemann Jeffrey G. 
Published: December 2016

Object
Emerging research in evoked broadband electrocorticographic (ECoG) measurement from the cortical surface suggests that it might cleanly delineate the functional organization of cortex. The authors sought to demonstrate whether this could be done in a same-session, online manner to identify receptive and expressive language areas.

Methods
The authors assessed the efficacy of simple integration of “χ-band” (76–200 Hz) change in the ECoG signal by implementing a simple band-pass filter to estimate broadband spectral change. Following a brief (less than 10-second) period to characterize baseline activity, χ-band activity was integrated while 7 epileptic patients with implanted ECoG electrodes performed a verb-generation task.

Results
While the patients were performing verb-generation or noun-reading tasks, cortical activation was consistently identified in primary mouth motor area, superior temporal gyrus, and Broca and Wernicke association areas. Maps were robust after a mean time of 47seconds (using an “activation overlap” measure). Correlation with electrocortical stimulation was not complete and was stronger for noun reading than verb generation.

Conclusions
Broadband ECoG changes can be captured online to identify eloquent cortex. This demonstrates the existence of a powerful new tool for functional mapping in the operative and chronic implant setting.
Level I to III craniofacial approaches based on Barrow classification for treatment of skull base meningiomas: surgical technique, microsurgical anatomy, and case illustrations
Authors: Avcı Emel , Aktüre Erinç , Seçkin Hakan , Uluç Kutluay , Bauer Andrew M. , Izci Yusuf , Morcos Jacques J. , Başkaya Mustafa K. 
Published: December 2016

Object
Although craniofacial approaches to the midline skull base have been defined and surgical results have been published, clear descriptions of these complex approaches in a step-wise manner are lacking. The objective of this study is to demonstrate the surgical technique of craniofacial approaches based on Barrow classification (Levels I–III) and to study the microsurgical anatomy pertinent to these complex craniofacial approaches.

Methods
Ten adult cadaveric heads perfused with colored silicone and 24 dry human skulls were used to study the microsurgical anatomy and to demonstrate craniofacial approaches in a step-wise manner. In addition to cadaveric studies, case illustrations of anterior skull base meningiomas were presented to demonstrate the clinical application of the first 3 (Levels I–III) approaches.

Results
Cadaveric head dissection was performed in 10 heads using craniofacial approaches. Ethmoid and sphenoid sinuses, cribriform plate, orbit, planum sphenoidale, clivus, sellar, and parasellar regions were shown at Levels I, II, and III. In 24 human dry skulls (48 sides), a supraorbital notch (85.4%) was observed more frequently than the supraorbital foramen (14.6%). The mean distance between the supraorbital foramen notch to the midline was 21.9 mm on the right side and 21.8 mm on the left. By accepting the middle point of the nasofrontal suture as a landmark, the mean distances to the anterior ethmoidal foramen from the middle point of this suture were 32 mm on the right side and 34 mm on the left. The mean distance between the anterior and posterior ethmoidal foramina was 12.3 mm on both sides; the mean distance between the posterior ethmoidal foramen and distal opening of the optic canal was 7.1 mm on the right side and 7.3 mm on the left.

Conclusions
Barrow classification is a simple and stepwise system to better understand the surgical anatomy and refine the techniques in performing these complex craniofacial approaches. On the other hand, thorough anatomical knowledge of the midline skull base and variations of the neurovascular structures is crucial to perform successful craniofacial approaches.
Surgical nuances for removal of tuberculum sellae meningiomas with optic canal involvement using the endoscopic endonasal extended transsphenoidal transplanum transtuberculum approach
Authors: Liu James K. , Christiano Lana D. , Patel Smruti K. , Tubbs R. Shane , Eloy Jean Anderson 
Published: December 2016

Tuberculum sellae meningiomas frequently extend into the optic canals. Radical tumor resection including the involved dural attachment, underlying hyperostotic bone, and intracanalicular tumor in the optic canal offers the best chance of a Simpson Grade I resection to minimize recurrence. Decompression of the optic canal with removal of the intracanalicular tumor also improves visual outcome since this portion of the tumor is usually the cause of asymmetrical visual loss.
The purely endoscopic endonasal extended transsphenoidal approach offers a direct midline trajectory and immediate access to tuberculum sellae meningiomas without brain retraction and manipulation of neurovascular structures. Although the endoscopic approach has been previously criticized for its inability to remove tumor within the optic canals, complete Simpson Grade I tumor removal including intracanalicular tumor, dural attachment, and involved hyperostotic bone can be achieved in properly selected patients. Excellent visualization of the suprasellar region and the inferomedial aspects of both optic canals allows for extracapsular, extraarachnoid dissection of the tumor from the critical structures using bimanual microsurgical dissection.
In this report, the authors describe the operative nuances for removal of tuberculum sellae meningiomas with optic canal involvement using a purely endoscopic endonasal extended transsphenoidal (transplanum transtuberculum) approach. They specifically highlight the technique for endonasal bilateral optic nerve decompression and removal of intracanalicular tumor to improve postoperative visual function, as demonstrated in 2 illustrative cases. Special attention is also given to cranial base reconstruction to prevent CSF leakage using the vascularized pedicled nasoseptal flap.
Hemodynamic and autonomic responses after a single session of resistance exercise following anodal motor cortex tDCS
Authors: Germano-Soares Antonio H. , Montenegro Rafael A. , Cavalcante Bruno R. , Domingues Wagner J.R. , de Lima Paulo F.M. , Menêses Annelise L. , Almeida Tarciso R.M. , Okano Alexandre H. , Ritti-Dias Raphael M. 
Published: December 2016

BACKGROUND: Transcranial direct current stimulation (tDCS) seems to modulate cardiac autonomic function and blood pressure (BP) at rest and during exercise. Therefore, it is possible that anodal tDCS could influence post-exercise hypotension. OBJECTIVE: To investigate whether anodal tDCS applied over the motor cortex would affect cardiac autonomic modulation and BP after resistance exercise. METHODS: Twelve apparently healthy young men performed two experimental sessions: anodal tDCS or sham condition followed by resistance exercise. Blood pressure (BP), heart rate (HR), rate-pressure product (RPP), and HR variability (HRV) were obtained before and during post-exercise recovery (at 20 and 60 minutes). RESULTS: Compared to pre-exercise, systolic BP decreased at 20 and at 60 minutes of post-exercise recovery only in anodal tDCS condition(p = 0.03), with no statistical differences in sham condition (p > 0.05). Diastolic and mean BP reduced after both anodal tDCS and sham conditions with no differences between them (P> 0.05). In comparison with anodal tDCS, there were slower HR recovery (tDCS vs. sham: -2 ± 14 vs. 14 ± 8 bpm) and higher RPP (tDCS vs. sham: -1083 ± 1846 vs. 1672 ± 1275 mmHg × bpm) after exercise following sham condition (P< 0.01). No differences were found in any of the HRV analyzed parameters (P> 0.05). CONCLUSION: A single session of primary motor cortex tDCS is capable of decreasing the systolic BP and HR responses, as well as the cardiac work after a resistance exercise session in young normotensive subjects regardless of any changes in cardiac autonomic modulation.
Gastrocnemius muscle activation during plantar flexion with different feet positioning in physically active young men
Authors: Marcori Alexandre J. , Moura Túlio B.M.A. , Okazaki Victor H.A. 
Published: December 2016

BACKGROUND: Varying exercise parameters, such as angles of movement, can cause different activation patterns within muscle compartments. Therefore, it is expected that feet positioning variations could influence gastrocnemius activity. OBJECTIVE: Compare gastrocnemius activation during plantar flexion with feet pointing forwards (FO), inwards (IN) and outwards (OU). METHODS: Sixteen physically active men (21 ± 2 years; 1.75 ± 0.06 meters and 74.8 ± 7.2 kg), performed 3 sets of 10 repetitions in each of the following experimental conditions: plantar flexion with feet pointing FO, IN and OU. The root mean square (RMS) of the muscular activation of both gastrocnemius heads was analyzed in each set by electromyography. RESULTS: For the medial head of the gastrocnemius, the OU condition presented greater RMS values when compared to the IN (z = 3.41; p < 0.001) and FO (z = 2.37; p≤ 0.017) conditions. For the lateral head, however, the IN condition demonstrated greatest RMS when compared with OU (z = 3.20; p = 0.001) and FO (z = 3.25; p = 0.001) conditions. CONCLUSIONS: These results suggest that it is possible to create greater activation sites in the gastrocnemius. Trainers and practitioners could use this to prescribe exercise more efficiently, possibly correcting asymmetries in athletes, especially bodybuilders.
PROBING WHIM AROUND GALAXY CLUSTERS WITH FAST RADIO BURSTS AND THE SUNYAEV–ZEL’DOVICH EFFECT
Authors: Fujita Yutaka , Akahori Takuya , Umetsu Keiichi , Sarazin Craig L. , Wong Ka-Wah 
Published: December 2016

ABSTRACT
We propose a new method to probe the warm hot intergalactic medium (WHIM) beyond the virial radius (R
200) of a cluster of galaxies, where X-ray observations are not easily achievable. In this method, we use dispersion measures (DMs) of fast radio bursts (FRBs) that appear behind the cluster and the Sunyaev–Zel’dovich (SZ) effect toward the cluster. The DMs reflect the density of the intracluster medium including the WHIM. If we observe a sufficient number of FRBs in the direction of the cluster, we can derive the density profile from the DMs. Similarly, we can derive the pressure profile from the SZ effect. By combining the density and the pressure profiles, the temperature profile can be obtained. Based on mock observations of nearby clusters, we find that the density of the WHIM will be determined even at

from the cluster center when FRB observations with the Square Kilometre Array become available. The temperature can be derived out to

, and the radius is limited by the current sensitivity of SZ observations.
GIANT CORONAL LOOPS DOMINATE THE QUIESCENT X-RAY EMISSION IN RAPIDLY ROTATING M STARS
Authors: Cohen O. , Yadav R. , Garraffo C. , Saar S. H. , Wolk S. J. , Kashyap V. L. , Drake J. J. , Pillitteri I. 
Published: December 2016

ABSTRACT
Observations indicate that magnetic fields in rapidly rotating stars are very strong, on both small and large scales. What is the nature of the resulting corona? Here we seek to shed some light on this question. We use the results of an anelastic dynamo simulation of a rapidly rotating fully convective M star to drive a physics-based model for the stellar corona. We find that due to the several kilo Gauss large-scale magnetic fields at high latitudes, the corona, and its X-ray emission are dominated by star-size large hot loops, while the smaller, underlying colder loops are not visible much in the X-ray. Based on this result, we propose that, in rapidly rotating stars, emission from such coronal structures dominates the quiescent, cooler but saturated X-ray emission.
THE BURRELL SCHMIDT DEEP VIRGO SURVEY: TIDAL DEBRIS, GALAXY HALOS, AND DIFFUSE INTRACLUSTER LIGHT IN THE VIRGO CLUSTER
Authors: Mihos J. Christopher , Harding Paul , Feldmeier John J. , Rudick Craig , Janowiecki Steven , Morrison Heather , Slater Colin , Watkins Aaron 
Published: December 2016

ABSTRACT
We present the results of a deep imaging survey of the Virgo cluster of galaxies, concentrated around the cores of Virgo subclusters A and B. The goal of this survey was to detect and study very low surface brightness features present in Virgo, including discrete tidal features, the faint halos of luminous galaxies, and the diffuse intracluster light (ICL). Our observations span roughly 16 degrees2 in two filters, reaching a 3σ limiting depth of

= 29.5 and

= 28.5 mag arcsec−2. At these depths, our limiting systematic uncertainties are astrophysical: variations in faint background sources as well as scattered light from galactic dust. We show that this dust-scattered light is well traced by deep far-infrared imaging, making it possible to separate it from true diffuse light in Virgo. We use our imaging to trace and measure the color of the diffuse tidal streams and ICL in the Virgo core near M87, in fields adjacent to the core including the M86/M84 region, and to the south of the core around M49 and subcluster B, along with the more distant W

cloud around NGC 4365. Overall, the bulk of the projected ICL is found in the Virgo core and within the W

cloud; we find little evidence for an extensive ICL component in the field around M49. The bulk of the ICL we detect is fairly red in color (B − V = 0.7–0.9), indicative of old, evolved stellar populations. Based on the luminosity of the observed ICL features in the cluster, we estimate a total Virgo ICL fraction of 7%–15%. This value is somewhat smaller than that expected for massive, evolved clusters, suggesting that Virgo is still in the process of growing its extended ICL component. We also trace the shape of M87's extremely boxy outer halo out to ∼150 kpc, and show that the current tidal stripping rate from low luminosity galaxies is insufficient to have built M87's outer halo over a Hubble time. We identify a number of previously unknown low surface brightness structures around galaxies projected close to M86 and M84. The extensive diffuse light seen in the infalling W

cloud around NGC 4365 is likely to be subsumed in the general Virgo ICL component once the group enters the cluster, illustrating the importance of group infall in generating ICL. Finally, we also identify another large and extremely low surface brightness ultradiffuse galaxy, likely in the process of being shredded by the cluster tidal field. With the survey complete, the full imaging data set is now available for public release.
MOSFIRE SPECTROSCOPY OF QUIESCENT GALAXIES AT 1.5 < z < 2.5. I. EVOLUTION OF STRUCTURAL AND DYNAMICAL PROPERTIES
Authors: Belli Sirio , Newman Andrew B. , Ellis Richard S. 
Published: December 2016

ABSTRACT
We present deep near-infrared spectra for a sample of 24 quiescent galaxies in the redshift range

obtained with the MOSFIRE spectrograph at the W. M. Keck Observatory. In conjunction with a similar data set we obtained in the range

with the LRIS spectrograph, we analyze the kinematic and structural properties for 80 quiescent galaxies, the largest homogeneously selected sample to date spanning 3 Gyr of early cosmic history. Analysis of our Keck spectra together with measurements derived from associated Hubble Space Telescope images reveals increasingly larger stellar velocity dispersions and smaller sizes to redshifts beyond

. By classifying our sample according to Sérsic indices, we find that among disk-like systems the flatter ones show a higher dynamical to stellar mass ratio compared to their rounder counterparts, which we interpret as evidence for a significant contribution of rotational motion. For this subset of disk-like systems, we estimate that

, the ratio of the circular velocity to the intrinsic velocity dispersion, is a factor of two larger than for present-day disky quiescent galaxies. We use the velocity dispersion measurements also to explore the redshift evolution of the dynamical to stellar mass ratio, and to measure for the first time the physical size growth rate of individual systems over two distinct redshift ranges, finding a faster evolution at earlier times. We discuss the physical origin of this time-dependent growth in size in the context of the associated reduction of the systematic rotation.
THE ACCRETION RATE DEPENDENCE OF BURST OSCILLATION AMPLITUDE
Authors: Ootes Laura S. , Watts Anna L. , Galloway Duncan K. , Wijnands Rudy 
Published: December 2016

ABSTRACT
Neutron stars in low-mass X-ray binaries exhibit oscillations during thermonuclear bursts, attributed to asymmetric brightness patterns on the burning surfaces. All models that have been proposed to explain the origin of these asymmetries (spreading hotspots, surface waves, and cooling wakes) depend on the accretion rate. By analysis of archival RXTE data of six oscillation sources, we investigate the accretion rate dependence of the amplitude of burst oscillations. This more than doubles the size of the sample analyzed previously by Muno et al., who found indications for a relationship between accretion rate and oscillation amplitudes. We find that burst oscillation signals can be detected at all observed accretion rates. Moreover, oscillations at low accretion rates are found to have relatively small amplitudes (

) while oscillations detected in bursts observed at high accretion rates cover a broad spread in amplitudes (

). In this paper we present the results of our analysis and discuss these in the light of current burst oscillation models. Additionally, we investigate the bursts of two sources without previously detected oscillations. Despite the fact that these sources have been observed at accretion rates where burst oscillations might be expected, we find their behavior not to be anomalous compared to oscillation sources.
FOLLOWING THE COSMIC EVOLUTION OF PRISTINE GAS. I. IMPLICATIONS FOR MILKY WAY HALO STARS
Authors: Sarmento Richard , Scannapieco Evan , Pan Liubin 
Published: December 2016

ABSTRACT
We make use of a new subgrid model of turbulent mixing to accurately follow the cosmological evolution of the first stars, the mixing of their supernova (SN) ejecta, and the impact on the chemical composition of the Galactic Halo. Using the cosmological adaptive mesh refinement code ramses, we implement a model for the pollution of pristine gas as described in Pan et al. Tracking the metallicity of Pop III stars with metallicities below a critical value allows us to account for the fraction of

stars formed even in regions in which the gas’s average metallicity is well above

We demonstrate that such partially mixed regions account for 0.5 to 0.7 of all Pop III stars formed up to z = 5. Additionally, we track the creation and transport of “primordial metals” (PM) generated by Pop III SNe. These neutron-capture deficient metals are taken up by second-generation stars and likely lead to unique abundance signatures characteristic of carbon-enhanced, metal-poor (CEMP-no) stars. As an illustrative example, we associate primordial metals with abundance ratios used by Keller et al. to explain the source of metals in the star SMSS J031300.36-670839.3, finding good agreement with the observed [Fe/H], [C/H], [O/H], and [Mg/Ca] ratios in CEMP-no Milky Way halo stars. Similar future simulations will aid in further constraining the properties of Pop III stars using CEMP observations, as well as improve predictions of the spatial distribution of Pop III stars, as will be explored by the next generation of ground- and space-based telescopes.
ZEEMAN DOPPLER MAPS: ALWAYS UNIQUE, NEVER SPURIOUS?
Authors: Stift Martin J. , Leone Francesco 
Published: December 2016

ABSTRACT
Numerical models of atomic diffusion in magnetic atmospheres of ApBp stars predict abundance structures that differ from the empirical maps derived with (Zeeman) Doppler mapping (ZDM). An in-depth analysis of this apparent disagreement investigates the detectability by means of ZDM of a variety of abundance structures, including (warped) rings predicted by theory, but also complex spot-like structures. Even when spectra of high signal-to-noise ratio are available, it can prove difficult or altogether impossible to correctly recover shapes, positions, and abundances of a mere handful of spots, notwithstanding the use of all four Stokes parameters and an exactly known field geometry; the recovery of (warped) rings can be equally challenging. Inversions of complex abundance maps that are based on just one or two spectral lines usually permit multiple solutions. It turns out that it can by no means be guaranteed that any of the regularization functions in general use for ZDM (maximum entropy or Tikhonov) will lead to a true abundance map instead of some spurious one. Attention is drawn to the need for a study that would elucidate the relation between the stratified, field-dependent abundance structures predicted by diffusion theory on the one hand, and empirical maps obtained by means of “canonical” ZDM, i.e., with mean atmospheres and unstratified abundances, on the other hand. Finally, we point out difficulties arising from the three-dimensional nature of the atomic diffusion process in magnetic ApBp star atmospheres.