bluuebunny/crossref_metadata_2025_split huggingface dataset:
Falls and fear of falling in vertigo and balance disorders: A controlled cross-sectional study
Authors: Schlick Cornelia , Schniepp Roman , Loidl Verena , Wuehr Max , Hesselbarth Kristin , Jahn Klaus 
Published: February 2016

BACKGROUND: Vertigo and dizziness are among the most prevalent symptoms in neurologic disorders. Although many of these patients suffer from postural instability and gait disturbances, there is only limited data on their risk of falling. METHODS: We conducted a controlled cross-sectional study at the tertiary care outpatient clinic of the German Center for Vertigo and Balance Disorders using a self-administered questionnaire to assess falls, fall-related injuries, and fear of falling. The recruitment period was 6 months. RESULTS: A total of 569 patients (mean age 59.6 ± 17.1 years, 55% females) and 100 healthy participants were included (response rate > 90%). Dizzy patients with central balance disorders (Parkinsonian, cerebellar, and brainstem oculomotor syndromes) had the highest fall rates (> 50% recurrent fallers, odds ratio > 10). The rate of recurrent fallers was 30% in bilateral vestibular failure and peripheral neuropathy (odds ratio > 5). Patients with functional dizziness (somatoform or phobic vertigo) were concerned about falling but did not fall more often than healthy controls (odds ratio 0.87). CONCLUSION: Falls are common in patients presenting to a dizziness unit. Those with central syndromes are at risk of recurrent and injurious falling. Fall rates and fear of falling should be assessed in balance disorders and used to guide the regimen of rehabilitation therapy. The identification of risk factors would help provide protective measures to these groups of patients.
Anticompensatory quick eye movements after head impulses: A peripheral vestibular sign in spontaneous nystagmus
Authors: Luis L. , Lehnen N. , Muñoz E. , de Carvalho M. , Schneider E. , Valls-Solé J. , Costa J. 
Published: February 2016

BACKGROUND: Differentiating central from peripheral origins of spontaneous nystagmus (SN) is challenging. Looking for a simple sign of peripheral disease with the video Head Impulsive Test we noticed anti-compensatory eye movements (AQEM) in patients with peripheral etiologies of spontaneous nystagmus (SN). Here we assess the diagnostic accuracy of AQEM in differentiating peripheral from central vestibular disorders. METHODS: We recorded the eye movements in response to horizontal head impulses in a group of 43 consecutive patients with acute vestibular syndrome (12 with central, 31 with peripheral disorders), 5 patients after acute vestibular neurectomy (positive controls) and 39 healthy subjects (negative controls). AQEM were defined as quick eye movements (peak velocity above 50°/s) in the direction of the head movement. RESULTS: All patients with peripheral disorders and positive controls had AQEM (latency 231 ± 53 ms, amplitude 3.4 ± 1.4°, velocity 166 ± 55°/s) when their head was moved to the opposite side of the lesion. Central patients did not have AQEM. AQEM occurrence rate was higher in peripheral patients with contralesional (74 ± 4%, mean ± SD) in comparison to ipsilesional (1 ± 4%) impulses (p< 0.001). Overall diagnostic accuracy for differentiating central from peripheral patients was 96% (95% CI for AUC ROC curve: 0.90 to 1.0) for VOR gain and 100% (95% CI: 1.0 to 1.0) for AQEM occurrence rate. CONCLUSIONS: These results suggest that AQEM are a sign of vestibular imbalance in a peripheral deficit. In addition to VOR gain they should be added to the evaluation of the head impulse test.
La juridiction privilégiée du magistrat face aux officiers de justice du Prince à Lille, XIVe-XVIIe siècle
Authors: Lorgnier Jacques 
Published: February 2016

Jacques Lorgnier, De eigen rechtspraak van de magistraat tegenover de rechtsofficieren van de Prins, in Rijsel, xive-xvne eeuw.
De magistraat zorgde bij privilégie voor de rechtspraak van de burgers van Rijsel. Hij slaagde erin onafhankelijk te blijven door zich ertegen te verzetten dat er zonder hem recht gesproken werd in de schepenbank en voor wat de belastingen en de zone buiten de muren betrof, en door te weigeren zijn uits- praken voor te leggen aan andere lokale rechtbanken, vooral die van de sou- vereine gouverneur-baljuw van Rijsel.
Eeuwenlang erkende de Prins die rechtsmacht die hij verleend had als belo- ning voor de trouw van de Rijselse schepenen. Hij waakte op het opstellen van voor de stad gunstige voorzorgsmaatregelen en op de strikte scheiding met de buitengewone rechtsmacht van de baljuw. Zo werden de schepenen, vooral voor civiele zaken, het natuurlijk tribunaal van eerste instantie voor aile Rij- selenaren, eisers en verdedigers, tot in Parijs toe. Voor wat het strafrecht betreft werd de voorrang van de schepelijke rechtsmacht gedeeltelijk betwist tijdens de politieke en religieuze troebelen in de xvie eeuw, waarvoor men meer dan vroeger een beroep deed op uitzonderingsrechtbanken of op een gezagsni- veau dat dichter stond bij de vorst dan een Vlaamse schepenbank. Zaken als de politiemacht en de plakkaten over de openbare orde zijn daarvan een goed voorbeeld.
Men kan desondanks besluiten dat de officieren van de gemeentelijke recht- bank het haalden op die van de prins (kasteeldomein en baljuwschap), wegens de trouw van de stad en de hardnekkigheid waarmee de juristen het midde- leeuwse privilégie wisten aan te passen aan de evolutie van het recht. Toen zij opnieuw bij Frankrijk ingelijfd werden, bevonden zij zich in een uitzonderlijke toestand op rechterlijk gebied, overgeërfd uit de Spaanse rechtspraak, en die met koninklijk welnemen tijdelijk behouden bleef.
La musique dans la sociabilité urbaine au XVIIIe siècle : l'exemple de Lille
Authors: Duhamel Jean-Marie 
Published: February 2016

Malgré sa réputation, moquée par certains lettrés tel l'abbé Expilly, de cité profondément marchande, uniquement préoccupée de négoce et de profits, la ville de Lille n'a pas complètement ignoré les charmes des Lumières. Si une Académie n'a jamais pu s'installer, le xvme siècle a vu néanmoins la mise en place non seulement d'un opéra régulier mais encore de successives sociétés de concerts semi-privées. Ainsi, en 1767, l'opéra emploie une centaine de personnes tandis qu'à la veille de la Révolution, «le Concert de MM. les Abonnés» accueille plus de 600 souscripteurs.
Au-delà d'une activité artistique au cœur des préoccupations du siècle, s'interroger sur ces structures musicales permet d'approcher quelques-unes des pratiques culturelles et des rituels de sociabilité des élites lilloises.
THE INNER DEBRIS STRUCTURE IN THE FOMALHAUT PLANETARY SYSTEM*
Authors: Su Kate Y. L. , Rieke George H. , Defrére Denis , Wang Kuo-Song , Lai Shih-Ping , Wilner David J. , Lieshout Rik van , Lee Chin-Fei 
Published: February 2016

ABSTRACT
Fomalhaut plays an important role in the study of debris disks and small bodies in other planetary systems. The proximity and luminosity of the star make key features of its debris, like the water ice line, accessible. Here we present ALMA cycle 1, 870 μm (345 GHz) observations targeted at the inner part of the Fomalhaut system with a synthesized beam of 0.″45 × 0.″37 (∼3 AU linear resolution at the distance of Fomalhaut) and an rms of 26 μJy beam−1. The high angular resolution and sensitivity of the ALMA data enable us to place strong constraints on the nature of the warm excess revealed by Spitzer and Herschel observations. We detect a point source at the star position with a total flux consistent with thermal emission from the stellar photosphere. No structures that are brighter than 3σ are detected in the central 15 AU × 15 AU region. Modeling the spectral energy distribution using parameters expected for a dust-producing planetesimal belt indicates a radial location in the range of ∼8–15 AU. This is consistent with the location where ice sublimates in Fomalhaut, i.e., an asteroid-belt analog. The 3σ upper limit for such a belt is <1.3 mJy at 870 μm. We also interpret the 2 and 8–13 μm interferometric measurements to reveal the structure in the inner 10 AU region as dust naturally connected to this proposed asteroid belt by Poynting–Robertson drag, dust sublimation, and magnetically trapped nanograins.
THE SINFONI BLACK HOLE SURVEY: THE BLACK HOLE FUNDAMENTAL PLANE REVISITED AND THE PATHS OF (CO)EVOLUTION OF SUPERMASSIVE BLACK HOLES AND BULGES
Authors: Saglia R. P. , Opitsch M. , Erwin P. , Thomas J. , Beifiori A. , Fabricius M. , Mazzalay X. , Nowak N. , Rusli S. P. , Bender R. 
Published: February 2016

ABSTRACT
We investigate the correlations between the black hole (BH) mass M
BH, the velocity dispersion σ, the bulge mass M
Bu, the bulge average spherical density

, and its spherical half-mass radius r
h, constructing a database of 97 galaxies (31 core ellipticals, 17 power-law ellipticals, 30 classical bulges, and 19 pseudobulges) by joining 72 galaxies from the literature to 25 galaxies observed during our recent SINFONI BH survey. For the first time we discuss the full error covariance matrix. We analyze the well-known M
BH–σ and M
BH–M
Bu relations and establish the existence of statistically significant correlations between M
Bu and r
h and anticorrelations between M
Bu and

. We establish five significant bivariate correlations (M
BH–σ–ρ
h, M
BH–σ–r
h, M
BH–M
Bu–σ, M
BH–M
Bu–ρ
h, M
BH–M
Bu–r
h) that predict M
BH of 77 core and power-law ellipticals and classical bulges with measured and intrinsic scatter as small as

dex and

dex, respectively, or 0.26 dex when the subsample of 45 galaxies defined by Kormendy & Ho is considered. In contrast, pseudobulges have systematically lower M
BH but approach the predictions of all of the above relations at spherical densities

or scale lengths

. These findings fit in a scenario of coevolution of BH and classical-bulge masses, where core ellipticals are the product of dry mergers of power-law bulges and power-law ellipticals and bulges the result of (early) gas-rich mergers and of disk galaxies. In contrast, the (secular) growth of BHs is decoupled from the growth of their pseudobulge hosts, except when (gas) densities are high enough to trigger the feedback mechanism responsible for the existence of the correlations between M
BH and galaxy structural parameters.
EVOLUTION OF THE X-RAY PROFILE OF THE CRAB PULSAR
Authors: Ge M. Y. , Yan L. L. , Lu F. J. , Zheng S. J. , Yuan J. P. , Tong H. , Zhang S. N. , Lu Y. 
Published: February 2016

ABSTRACT
Using the archival data from the Rossi X-ray Timing Explorer, we study the evolution of the Crab pulsar’s X-ray profile in a time span of 11 years. The X-ray profiles, as characterized by a few parameters, changed slightly, but with high statistical significance in these years: the separation of the two peaks increased with a rate of 0.°88 ± 0.°20 per century, the flux ratio of the second pulse to the first pulse decreased by

per century, and the pulse widths of the two pulses represented by their full widths at half maxima decreased by

and

per century, respectively. The evolutionary trends of the X-ray profile are similar to that observed in radio, but with quantitative differences. Finally, we briefly discuss the constraints of these X-ray properties on the geometry of the emission region of this pulsar.
ON THE INTERACTIVE-BEATING-MODES MODEL: GENERATION OF ASYMMETRIC MULTIPLET STRUCTURES AND EXPLANATION OF THE BLAZHKO EFFECT
Authors: Bryant Paul H. 
Published: February 2016

ABSTRACT
This paper considers a nonlinear coupling between a radial and a nonradial mode of nearly the same frequency. The results may be of general interest, but in particular have application to the “beating-modes model” of the Blazhko effect which was recently shown to accurately reproduce the light curve of RR Lyr. For weak coupling, the two modes do not phase-lock and they retain separate frequencies, but the coupling nevertheless has important consequences. Upon increasing the coupling strength from zero, an additional side-peak emerges in the spectrum forming an asymmetric triplet centered on the fundamental. As the coupling is further increased, the amplitude of this side-peak increases and the three peaks are also pulled toward each other, decreasing the Blazhko frequency. Beyond a critical coupling strength, phase-locking occurs between the modes. With appropriate choice of coupling strength, this “interactive beating-modes model” can match the side-peak amplitude ratio of any star. The effects of nonlinear damping are also explored and found to generate additional side-peaks of odd order. Consistent with this, the odd side-peaks are found to be favored in V808 Cyg. It is also shown that the Blazhko effect generates a fluctuating “environment” that can have a modulatory effect on other excited modes of the star. An example is found in V808 Cyg where the modulation is at double the Blazhko frequency. An explanation is found for this mysterious doubling, providing additional evidence in favor of the model.
ANALYSIS OF FLOWS INSIDE QUIESCENT PROMINENCES AS CAPTURED BY HINODE/SOLAR OPTICAL TELESCOPE
Authors: Freed M. S. , McKenzie D. E. , Longcope D. W. , Wilburn M. 
Published: February 2016

ABSTRACT
Developing an understanding of how magnetic fields can become entangled in a prominence is important for predicting a possible eruption. This work investigates the kinetic energy and vorticity associated with plasma motion residing inside quiescent prominences (QPs). These plasma flow characteristics can be utilized to improve our understanding of how the prominence maintains a stable magnetic field configuration. Three different contrast-enhanced solar prominence observations from Hinode/Solar Optical Telescope were used to construct velocity maps—in the plane of the sky—via a Fourier local correlation tracking program. The resulting velocities were then used to perform the first-ever analysis of the two-dimensional kinetic energy and enstrophy spectra of a prominence. Enstrophy is introduced here as a means of quantifying the vorticity that has been observed in many QPs. The kinetic energy power spectral density (PSD) produced indices ranging from −1.00 to −1.60. There was a consistent anisotropy in the kinetic energy spectrum of all three prominences examined. Examination of the intensity PSD reveals that a different scaling relationship exists between the observed prominence structure and velocity maps. All of the prominences exhibited an inertial range of at least

. Quasi-periodic oscillations were also detected in the centroid of the velocity distributions for one prominence. Additionally, a lower limit was placed on the kinetic energy density (ϵ ∼ 0.22–7.04

) and enstrophy density (ω ∼ 1.43–13.69

) associated with each prominence.
THE SIZES OF GLOBULAR CLUSTERS AS TRACERS OF GALACTIC HALO POTENTIALS
Authors: Zonoozi A. H. , Rabiee M. , Haghi H. , Küpper A. H. W. 
Published: February 2016

ABSTRACT
We present N-body simulations of globular clusters, exploring the effect of different galactic potentials on cluster sizes, r

h
. For various galactocentric distances, R

G
, we assess how cluster sizes change when we vary the virial mass and concentration of the host galaxy’s dark-matter halo. We show that sizes of GCs are determined by the local galactic mass density rather than the virial mass of the host galaxy. We find that clusters evolving in the inner halos of less concentrated galaxies are significantly more extended than those evolving in more concentrated ones, while the sizes of those orbiting in the outer halo are almost independent of concentration. Adding a baryonic component to our galaxy models does not change these results much, since its effect is only significant in the very inner halo. Our simulations suggest that there is a relation between r

h
and R

G
, which systematically depends on the physical parameters of the halo. Hence, observing such relations in individual galaxies can put a new observational constraint on dark-matter halo characteristics. However, by varying the halo mass in a wide range of

, we find that the r

h
− R

G
relationship will be nearly independent of halo mass, if one assumes M
vir and c
vir as two correlated parameters, as is suggested by cosmological simulations.
IN-SYNC. IV. THE YOUNG STELLAR POPULATION IN THE ORION A MOLECULAR CLOUD
Authors: Rio Nicola Da , Tan Jonathan C. , Covey Kevin R. , Cottaar Michiel , Foster Jonathan B. , Cullen Nicholas C. , Tobin John J. , Kim Jinyoung S. , Meyer Michael R. , Nidever David L. , Stassun Keivan G. , Chojnowski S. Drew , Flaherty Kevin M. , Majewski Steve , Skrutskie Michael F. , Zasowski Gail , Pan Kaike 
Published: February 2016

ABSTRACT
We present the results of the Sloan Digital Sky Survey APOGEE INfrared Spectroscopy of Young Nebulous Clusters program (IN-SYNC) survey of the Orion A molecular cloud. This survey obtained high-resolution near-infrared spectroscopy of about 2700 young pre-main-sequence stars on a

field of view. We have measured accurate stellar parameters (

,

,

) and extinctions and placed the sources in the Hertzsprung–Russel diagram (HRD). We have also extracted radial velocities for the kinematic characterization of the population. We compare our measurements with literature results to assess the performance and accuracy of the survey. Source extinction shows evidence for dust grains that are larger than those in the diffuse interstellar medium: we estimate an average R

V
= 5.5 in the region. Importantly, we find a clear correlation between HRD inferred ages and spectroscopic surface-gravity-inferred ages and between extinction and disk presence; this strongly suggests a real spread of ages larger than a few Myr. Focusing on the young population around NGC 1980/ι Ori, which has previously been suggested to be a separate, foreground, older cluster, we confirm its older (∼5 Myr) age and low A

V
, but considering that its radial velocity distribution is indistinguishable from Orion A’s population, we suggest that NGC 1980 is part of Orion A’s star formation activity. Based on their stellar parameters and kinematic properties, we identify 383 new candidate members of Orion A, most of which are diskless sources in areas of the region poorly studied by previous works.
PLASMA EMISSION BY COUNTER-STREAMING ELECTRON BEAMS
Authors: Ziebell L. F. , Petruzzellis L. T. , Yoon P. H. , Gaelzer R. , Pavan J. 
Published: February 2016

ABSTRACT
The radiation emission mechanism responsible for both type-II and type-III solar radio bursts is commonly accepted as plasma emission. Recently Ganse et al. suggested that type-II radio bursts may be enhanced when the electron foreshock geometry of a coronal mass ejection contains a double hump structure. They reasoned that the counter-streaming electron beams that exist between the double shocks may enhance the nonlinear coalescence interaction, thereby giving rise to more efficient generation of radiation. Ganse et al. employed a particle-in-cell simulation to study such a scenario. The present paper revisits the same problem with EM weak turbulence theory, and show that the fundamental (F) emission is not greatly affected by the presence of counter-streaming beams, but the harmonic (H) emission becomes somewhat more effective when the two beams are present. The present finding is thus complementary to the work by Ganse et al.
WHAT SHAPES THE FAR-INFRARED SPECTRAL ENERGY DISTRIBUTIONS OF GALAXIES?
Authors: Safarzadeh Mohammadtaher , Hayward Christopher C. , Ferguson Henry C. , Somerville Rachel S. 
Published: February 2016

ABSTRACT
To explore the connection between the global physical properties of galaxies and their far-infrared (FIR) spectral energy distributions (SEDs), we study the variation in the FIR SEDs of a set of 51 hydrodynamically simulated galaxies, both mergers and isolated systems representative of low- and high-redshift galaxies, that are generated by performing dust radiative transfer in post-processing. We study the FIR SEDs using principal component (PC) analysis, and find that 97% of the variance in the sample can be explained by two PCs. The first PC characterizes the wavelength of the peak of the FIR SED, and the second encodes the breadth of the SED. We find that the coefficients of both PCs can be predicted well using a double power law in terms of the IR luminosity and dust mass, which suggests that these two physical properties are the primary determinants of galaxies’ FIR SED shapes. Incorporating galaxy sizes does not significantly improve our ability to predict the FIR SEDs. Our results suggest that the observed redshift evolution in the effective dust temperature at a fixed IR luminosity is not driven by geometry: the SEDs of

ultraluminous IR galaxies (ULIRGs) are cooler than those of local ULIRGs, not because the high-redshift galaxies are more extended, but rather because they have higher dust masses at fixed IR luminosity. Finally, based on our simulations, we introduce a two-parameter set of SED templates that depend on both IR luminosity and dust mass.
THE FUNDAMENTAL PLANE OF THE BROAD-LINE REGION IN ACTIVE GALACTIC NUCLEI
Authors: Du Pu , Wang Jian-Min , Hu Chen , Ho Luis C. , Li Yan-Rong , Bai Jin-Ming 
Published: February 2016

ABSTRACT
Broad emission lines in active galactic nuclei (AGNs) mainly arise from gas photoionized by continuum radiation from an accretion disk around a central black hole. The shape of the broad-line profile, described by

, the ratio of full width at half maximum to the dispersion of broad Hβ, reflects the dynamics of the broad-line region (BLR) and correlates with the dimensionless accretion rate (

) or Eddington ratio (

/

). At the same time,

and

/

correlate with

, the ratio of optical Fe ii to Hβ line flux emission. Assembling all AGNs with reverberation mapping measurements of broad Hβ, both from the literature and from new observations reported here, we find a strong bivariate correlation of the form

where α = (2.47, 0.31), β = −(1.59, 0.82), and γ = (1.34, 0.80). We refer to this as the fundamental plane of the BLR. We apply the plane to a sample of z < 0.8 quasars to demonstrate the prevalence of super-Eddington accreting AGNs are quite common at low redshifts.
THE PDS 66 CIRCUMSTELLAR DISK AS SEEN IN POLARIZED LIGHT WITH THE GEMINI PLANET IMAGER
Authors: Wolff Schuyler G. , Perrin Marshall , Millar-Blanchaer Maxwell A. , Nielsen Eric L. , Wang Jason , Cardwell Andrew , Chilcote Jeffrey , Dong Ruobing , Draper Zachary H. , Duchêne Gaspard , Fitzgerald Michael P. , Goodsell Stephen J. , Grady Carol A. , Graham James R. , Greenbaum Alexandra Z. , Hartung Markus , Hibon Pascale , Hines Dean C. , Hung Li-Wei , Kalas Paul , Macintosh Bruce , Marchis Franck , Marois Christian , Pueyo Laurent , Rantakyrö Fredrik T. , Schneider Glenn , Sivaramakrishnan Anand , Wiktorowicz Sloane J. 
Published: February 2016

ABSTRACT
We present H- and K-band imaging polarimetry for the PDS 66 circumstellar disk obtained during the commissioning of the Gemini Planet Imager (GPI). Polarization images reveal a clear detection of the disk in to the 0.″12 inner working angle (IWA) in the H band, almost three times closer to the star than the previous Hubble Space Telescope (HST) observations with NICMOS and STIS (0.″35 effective IWA). The centro-symmetric polarization vectors confirm that the bright inner disk detection is due to circumstellar scattered light. A more diffuse disk extends to a bright outer ring centered at 80 AU. We discuss several physical mechanisms capable of producing the observed ring + gap structure. GPI data confirm enhanced scattering on the east side of the disk that is inferred to be nearer to us. We also detect a lateral asymmetry in the south possibly due to shadowing from material within the IWA. This likely corresponds to a temporally variable azimuthal asymmetry observed in HST/STIS coronagraphic imaging.