bluuebunny/crossref_metadata_2025_split huggingface dataset:
Adaptation, linguistic and clinimetric validation of the Bangla version of Zarit Burden Interview
Authors: Rabin Farzana , Nahar Jhunu Shamsun , Mullick Mohammad S. I. , Ahmed Helal Uddin , Farzana Nafia 
Published: December 2016

The aim of this study was to develop a culturally adapted and validated Bangla version of Zarit Burden Interview (ZBI-B) questionnaire for use in Bangla speaking caregiver of patient with dementia. This study was conducted on 100 caregivers related to consecutively attending outpatients with a previously established primary diagnosis of dementia, according to DSM-IV criteria. Validity and reliability were evaluated by comparing with the caregiver burden inventory (CBI). An exploratory factor analysis with the principle component with varimax rotation was used to detect the factorial structure in observed measurements. To attain the best-fitting structure and the correct number of factors, the following criteria were used: Eigen values >1.0, factor loadings >0.30. The Cronbachs alpha value was 0.847 for test and 0.839 retest. The intra-class correlation for the test-retest reliability was 0.89. The ZBI score was highly correlated with the CBI score (Pearsons correlation coefficient, r=0.909, P=.001). From the exploratory factor analysis six factors comprising 20 items were extracted with Eigen values higher than 1.00 accounting for 69% of the total item variance. In conclusion, ZBI-B is valid, reliable and useful for use in clinical contexts and in future studies that could lead to a better understanding of caregiver burden in dementia.
Serum concentration of folate, vitamin B<sub>12</sub> and homocysteine in patients of cervical cancer
Authors: Ferdous Jannatul , Khatun Sabera , Biawas Subrata Kumar , Akter Latifa , Keya Kashfia Ahmed 
Published: December 2016

The aim of this study was to evaluate the risk of cervical cancer in relation to serum concentration of folate, vitamin B12 and homocysteine. Fifty patients with invasive cervical cancer and 50 VIA negative cases (control) with age range of 30-65 years were included. Majority of the patients had significantly low level of serum folate and B12 than those in the control group. In contrast, serum homocysteine level was significantly high in cases than those in the control group. The Pearson correlation coefficient test showed a significant negative relationship between serum folate, vitamin B12 and serum homocyteine. However, there was no significant association between stage of cervical cancer and level of serum homocysteine. In conclusion, a significantly low level of serum folate, vitamin B12 and high level of serum homocysteine were observed in patients with invasive cervical cancer.
Hot electrons in silicon oxide
Authors: Gritsenko V A 
Published: December 2016

Abstract
One particular application of amorphous silicon oxide (SiO2), a material crucial for silicon device technology and design, is as a flash memory tunnel dielectric. The breakdown field of SiO2 exceeds 107 V cm−1. Strong electric fields in SiO2 give rise to phenomena that do not occur in crystalline semiconductors. In relatively weak electric fields (104–106 V cm−1), the electron distribution function is determined by the scattering of electrons on longitudinal optical phonons. In high fields (in excess of 106 V cm−1), the distribution function is determined by electron–acoustic phonon scattering.
Le cycle peint du château de Cruet (Savoie, vers 1307) : une représentation du roman de Girart de Vienne ?
Authors: Le Deschault de Monredon Térence 
Published: December 2016

Der Bilderzyklus im Schloss von Cruet (im Departement Savoie, um 1307) : eine Illustration des Romans Girart de Vienne ?
Aufgrund ihrer Abmessungen und ihrer einzigartigen Ikonographie bilden die im Musée Savoisien von Chambéry deponierten mittelalterlichen Wandmalereien aus dem Schloss von Cruet (Savoie) einen außergewöhnlichen Bilderzyklus. Bisher nahm man an, die Anfang des 14. Jhds. realisierten Bilder seien auf eine literarische Quelle zurückzuführen, und zwar auf eine Mischung aus Berthe as grans pies von Adenet le Roi und L’istoire le roy Charlemaine von Girart von Amiens. Der vorliegende Beitrag sieht in dem langen Bilderfries aber eher eine Illustration des Romans Girart de Vienne. In der Tat sind mehrere Szenen eine getreueWiedergabe des Textes von Bertrand von Bar-sur-Aube. Zudem lässt sich dieWahl der Herren von Verdon, die denWandschmuck in Auftrag gegeben haben, mühelos erklären, da sich die geographischen und politischen Ereignisse des Romans in denen ihrer Herrschaft widerspiegeln.
L’abbaye de moniales cisterciennes de Clairefontaine (Luxembourg). Synthèse archéo-historique des quatre phases de construction, XIIIe-XVIIIe siècle
Authors: Herremans Davy , Coomans Thomas 
Published: December 2016

Synthese der Bauforschungsergebnisse der in vier Etappen (13. – 18. Jhd.) immer wieder neu errichteten Zisterzienserinnenabtei von Clairefontaine (Belgien, Provinz Luxemburg).
In der nahe Arlon (Belgien, Provinz Luxemburg) gelegenen Zisterzienserinnenabtei von Clairefontaine wurden zehn Jahre lang archäologische Grabungen durchgeführt. Der Artikel verknüpft archäologische Befunde mit historischen Quellen und gelangt so zu einer Bauanalyse der Klosteranlage, die viermal wiederaufgebaut worden war : Clairefontaine I (um 1247), Clairefontaine II (erste Hälfte des 14. Jhds.), Clairefontaine III (erste Hälfte des 16. Jhds.), Clairefontaine IV (Ende des 17. bis Anfang des 18. Jhds.), schließlich die völlige Zerstörung und Auflösung durch die Franzosen (1796). Eine Stratigraphie dieser Art ist für eine Frauenklosterkirche eher selten ; sie ist jedoch außergewöhnlich für Klostergebäude, die einen Kreuzgang umschließen, denn in nur wenigen Frauenabteien wurden so umfangreiche Grabungen beschlossen wie in Clairefontaine. Jede Veränderung wurde mit dem entsprechenden historischen Umfeld in Verbindung gebracht und auf die in Luxemburg herrschenden Fürsten bezogen : die Gräfin Ermesinde, Heinrich der Blonde, Johann der Blinde, Christoph von Baden, Peter Ernst vonMansfeld, sowie die Erzherzöge Albert und Isabella. Sie alle waren bedeutende Auftraggeber und mächtige Schutzherren der von einer kleinen Gemeinschaft adeliger Zisterzienserinnen bewohnten Abtei.
IMAGING ANALYSIS OF THE HARD X-RAY TELESCOPE ProtoEXIST2 AND NEW TECHNIQUES FOR HIGH-RESOLUTION CODED-APERTURE TELESCOPES
Authors: Hong Jaesub , Allen Branden , Grindlay Jonathan , Barthelmy Scott 
Published: December 2016

ABSTRACT
Wide-field (≳100 deg

) hard X-ray coded-aperture telescopes with high angular resolution (≲2′) will enable a wide range of time domain astrophysics. For instance, transient sources such as gamma-ray bursts can be precisely localized without the assistance of secondary focusing X-ray telescopes to enable rapid followup studies. On the other hand, high angular resolution in coded-aperture imaging introduces a new challenge in handling the systematic uncertainty: the average photon count per pixel is often too small to establish a proper background pattern or model the systematic uncertainty in a timescale where the model remains invariant. We introduce two new techniques to improve detection sensitivity, which are designed for, but not limited to, a high-resolution coded-aperture system: a self-background modeling scheme which utilizes continuous scan or dithering operations, and a Poisson-statistics based probabilistic approach to evaluate the significance of source detection without subtraction in handling the background. We illustrate these new imaging analysis techniques in high resolution coded-aperture telescope using the data acquired by the wide-field hard X-ray telescope ProtoEXIST2 during a high-altitude balloon flight in fall 2012. We review the imaging sensitivity of ProtoEXIST2 during the flight, and demonstrate the performance of the new techniques using our balloon flight data in comparison with a simulated ideal Poisson background.
THE MAGNETIC FIELD OF L1544. I. NEAR-INFRARED POLARIMETRY AND THE NON-UNIFORM ENVELOPE
Authors: Clemens Dan P. , Tassis K. , Goldsmith Paul F. 
Published: December 2016

ABSTRACT
The magnetic field (B-field) of the starless dark cloud L1544 has been studied using near-infrared (NIR) background starlight polarimetry (BSP) and archival data in order to characterize the properties of the plane-of-sky B-field. NIR linear polarization measurements of over 1700 stars were obtained in the H band and 201 of these were also measured in the K band. The NIR BSP properties are correlated with reddening, as traced using the Rayleigh–Jeans color excess (H–M) method, and with thermal dust emission from the L1544 cloud and envelope seen in Herschel maps. The NIR polarization position angles change at the location of the cloud and exhibit their lowest dispersion there, offering strong evidence that NIR polarization traces the plane-of-sky B-field of L1544. In this paper, the uniformity of the plane-of-sky B-field in the envelope region of L1544 is quantitatively assessed. This allows evaluation of the approach of assuming uniform field geometry when measuring relative mass-to-flux ratios in the cloud envelope and core based on averaging of the radio Zeeman observations in the envelope, as done by Crutcher et al. In L1544, the NIR BSP shows the envelope B-field to be significantly non-uniform and likely not suitable for averaging Zeeman properties without treating intrinsic variations. Deeper analyses of the NIR BSP and related data sets, including estimates of the B-field strength and testing how it varies with position and gas density, are the subjects of later papers in this series.
ON THE FINE STRUCTURE SPLITTING OF THE 3p43d 4D5/2 AND 3p43d 4D7/2 LEVELS OF Fe x
Authors: Judge Philip G. , Hutton Roger , Li Wenxian , Brage Tomas 
Published: December 2016

ABSTRACT
We study UV spectra obtained with the SO82-B slit spectrograph on board SKYLAB to estimate the fine structure (FS) splitting of the Cl-like

and

levels of Fe x. The splitting is of interest because the Zeeman effect mixes these levels, producing a “magnetically induced transition” (MIT) from

to

for modest magnetic field strengths characteristic of the active solar corona. We estimate the splitting using the Ritz combination formula applied to two lines in the UV region of the spectrum close to 1603.2 Å, which decay from the level

to these two lower levels. The MIT and accompanying spin-forbidden transition lie near 257 Å. By careful inspection of a deep exposure obtained with the S082B instrument, we derive a splitting of

cm−1. The upper limit arises because of a degeneracy between the effects of non-thermal line broadening and FS splitting for small values of the latter parameter. Although the data were recorded on photographic film, we solved for optimal values of line width and splitting of 8.3 ± 0.9 and 3.6 ± 2.7 cm−1.
THE AGORA HIGH-RESOLUTION GALAXY SIMULATIONS COMPARISON PROJECT. II. ISOLATED DISK TEST
Authors: Kim Ji-hoon , Agertz Oscar , Teyssier Romain , Butler Michael J. , Ceverino Daniel , Choi Jun-Hwan , Feldmann Robert , Keller Ben W. , Lupi Alessandro , Quinn Thomas , Revaz Yves , Wallace Spencer , Gnedin Nickolay Y. , Leitner Samuel N. , Shen Sijing , Smith Britton D. , Thompson Robert , Turk Matthew J. , Abel Tom , Arraki Kenza S. , Benincasa Samantha M. , Chakrabarti Sukanya , DeGraf Colin , Dekel Avishai , Goldbaum Nathan J. , Hopkins Philip F. , Hummels Cameron B. , Klypin Anatoly , Li Hui , Madau Piero , Mandelker Nir , Mayer Lucio , Nagamine Kentaro , Nickerson Sarah , O’Shea Brian W. , Primack Joel R. , Roca-Fàbrega Santi , Semenov Vadim , Shimizu Ikkoh , Simpson Christine M. , Todoroki Keita , Wadsley James W. , Wise John H. ,   (for the AGORA Collaboration)
Published: December 2016

ABSTRACT
Using an isolated Milky Way-mass galaxy simulation, we compare results from nine state-of-the-art gravito-hydrodynamics codes widely used in the numerical community. We utilize the infrastructure we have built for the AGORA High-resolution Galaxy Simulations Comparison Project. This includes the common disk initial conditions, common physics models (e.g., radiative cooling and UV background by the standardized package Grackle) and common analysis toolkit yt, all of which are publicly available. Subgrid physics models such as Jeans pressure floor, star formation, supernova feedback energy, and metal production are carefully constrained across code platforms. With numerical accuracy that resolves the disk scale height, we find that the codes overall agree well with one another in many dimensions including: gas and stellar surface densities, rotation curves, velocity dispersions, density and temperature distribution functions, disk vertical heights, stellar clumps, star formation rates, and Kennicutt–Schmidt relations. Quantities such as velocity dispersions are very robust (agreement within a few tens of percent at all radii) while measures like newly formed stellar clump mass functions show more significant variation (difference by up to a factor of ∼3). Systematic differences exist, for example, between mesh-based and particle-based codes in the low-density region, and between more diffusive and less diffusive schemes in the high-density tail of the density distribution. Yet intrinsic code differences are generally small compared to the variations in numerical implementations of the common subgrid physics such as supernova feedback. Our experiment reassures that, if adequately designed in accordance with our proposed common parameters, results of a modern high-resolution galaxy formation simulation are more sensitive to input physics than to intrinsic differences in numerical schemes.
DENSE CORE PROPERTIES IN THE INFRARED DARK CLOUD G14.225-0.506 REVEALED BY ALMA
Authors: Ohashi Satoshi , Sanhueza Patricio , Chen Huei-Ru Vivien , Zhang Qizhou , Busquet Gemma , Nakamura Fumitaka , Palau Aina , Tatematsu Ken’ichi 
Published: December 2016

ABSTRACT
We have performed a dense core survey toward the Infrared Dark Cloud G14.225-0.506 at 3 mm continuum emission with the Atacama Large Millimeter/Submillimeter Array (ALMA). This survey covers the two hub-filament systems with an angular resolution of

(∼0.03 pc). We identified 48 dense cores. 20 out of the 48 cores are protostellar due to their association with young stellar objects (YSOs) and/or X-ray point-sources, while the other 28 cores are likely prestellar and unrelated with known IR or X-ray emission. Using APEX 870 μm continuum emission, we also identified the 18 clumps hosting these cores. Through virial analysis using the ALMA N2H+ and VLA/Effelsberg NH3 molecular line data, we found a decreasing trend in the virial parameter with decreasing scales from filaments to clumps, and then to cores. The virial parameters of 0.1–1.3 in cores indicate that cores are likely undergoing dynamical collapse. The cumulative core mass function for the prestellar core candidates has a power law index of

, with masses ranging from 1.5 to 22

. We find no massive prestellar or protostellar cores. Previous studies suggest that massive O-type stars have not been produced yet in this region. Therefore, high-mass stars should be formed in the prestellar cores by accreting a significant amount of gas from the surrounding medium. Another possibility is that low-mass YSOs become massive by accreting from their parent cores that are fed by filaments. These two possibilities might be consistent with the scenario of global hierarchical collapse.
A RECONNECTION-DRIVEN MODEL OF THE HARD X-RAY LOOP-TOP SOURCE FROM FLARE 2004 FEBRUARY 26
Authors: Longcope Dana , Qiu Jiong , Brewer Jasmine 
Published: December 2016

ABSTRACT
A compact X-class flare on 2004 February 26 showed a concentrated source of hard X-rays at the tops of the flare’s loops. This was analyzed in previous work and interpreted as plasma heated and compressed by slow magnetosonic shocks (SMSs) generated during post-reconnection retraction of the flux. That work used analytic expressions from a thin flux tube (TFT) model, which neglected many potentially important factors such as thermal conduction and chromospheric evaporation. Here we use a numerical solution of the TFT equations to produce a more comprehensive and accurate model of the same flare, including those effects previously omitted. These simulations corroborate the prior hypothesis that slow-mode shocks persist well after the retraction has ended, thus producing a compact, loop-top source instead of an elongated jet, as steady reconnection models predict. Thermal conduction leads to densities higher than analytic estimates had predicted, and evaporation enhances the density still higher, but at lower temperatures. X-ray light curves and spectra are synthesized by convolving the results from a single TFT simulation with the rate at which flux is reconnected, as measured through motion of flare ribbons, for example. These agree well with light curves observed by RHESSI and GOES and spectra from RHESSI. An image created from a superposition of TFT model runs resembles one produced from RHESSI observations. This suggests that the HXR loop-top source, at least the one observed in this flare, could be the result of SMSs produced in fast reconnection models like Petschek’s.
DOES THE MILKY WAY OBEY SPIRAL GALAXY SCALING RELATIONS?
Authors: Licquia Timothy C. , Newman Jeffrey A. , Bershady Matthew A. 
Published: December 2016

ABSTRACT
It is crucial to understand how the Milky Way (MW), the galaxy we can study in the most intimate detail, fits in among other galaxies. Key considerations include the Tully–Fisher relation (TFR)—i.e., the tight correlation between luminosity (L) and rotational velocity (V
rot)—and the three-dimensional luminosity–velocity–radius (LVR) scaling relation. Several past studies have characterized the MW as a 1–1.5σ outlier to the TFR. This study re-examines such comparisons using new estimates of MW properties that are robust to many of the systematic uncertainties that have been a problem in the past and are based on assumptions consistent with those used for other spiral galaxies. Comparing to scaling relations derived from modern extragalactic data, we find that our Galaxy’s properties are in excellent agreement with TFRs defined using any Sloan Digital Sky Survey-filter absolute magnitude, stellar mass, or baryonic mass as the L proxy. We next utilize disk scale length (R
d) measurements to extend this investigation to the LVR relation. Here we find that our Galaxy lies farther from the relation than ∼90% of other spiral galaxies, yielding ∼9.5σ evidence that it is unusually compact for its L and V
rot (based on MW errors alone), a result that holds for all of the L proxies considered. The expected R
d for the MW from the LVR relation is ∼5 kpc, nearly twice as large as the observed value, with error estimates placing the two in tension at the ∼1.4σ level. The compact scale length of the Galactic disk could be related to other ways in which the MW has been found to be anomalous.
THE GALEX TIME DOMAIN SURVEY. II. WAVELENGTH-DEPENDENT VARIABILITY OF ACTIVE GALACTIC NUCLEI IN THE PAN-STARRS1 MEDIUM DEEP SURVEY
Authors: Hung T. , Gezari S. , Jones D. O. , Kirshner R. P. , Chornock R. , Berger E. , Rest A. , Huber M. , Narayan G. , Scolnic D. , Waters C. , Wainscoat R. , Martin D. C. , Forster K. , Neill J. D. 
Published: December 2016

ABSTRACT
We analyze the wavelength-dependent variability of a sample of spectroscopically confirmed active galactic nuclei selected from near-UV (NUV) variable sources in the GALEX Time Domain Survey that have a large amplitude of optical variability (difference-flux S/N > 3) in the Pan-STARRS1 Medium Deep Survey (PS1 MDS). By matching GALEX and PS1 epochs in five bands (NUV, g

P1, r

P1, i

P1, z

P1) in time, and taking their flux difference, we create co-temporal difference-flux spectral energy distributions (

) using two chosen epochs for each of the 23 objects in our sample, on timescales of about a year. We confirm the “bluer-when-brighter” trend reported in previous studies, and measure a median spectral index of the

of

= 2.1 that is consistent with an accretion disk spectrum. We further fit the

of each source with a standard accretion disk model in which the accretion rate changes from one epoch to the other. In our sample, 17 out of 23 (∼74%) sources are described well by this variable accretion-rate disk model, with a median average characteristic disk temperature

of

K that is consistent with the temperatures expected, given the distribution of accretion rates and black hole masses inferred for the sample. Our analysis also shows that the variable accretion rate model is a better fit to the

than a simple power law.
OBSERVATIONAL EVIDENCE OF DYNAMIC STAR FORMATION RATE IN MILKY WAY GIANT MOLECULAR CLOUDS
Authors: Lee Eve J. , Miville-Deschênes Marc-Antoine , Murray Norman W. 
Published: December 2016

ABSTRACT
Star formation on galactic scales is known to be a slow process, but whether it is slow on smaller scales is uncertain. We cross-correlate 5469 giant molecular clouds (GMCs) from a new all-sky catalog with 256 star-forming complexes (SFCs) to build a sample of 191 SFC-GMC complexes—collections of multiple clouds each matched to 191 SFCs. The total mass in stars harbored by these clouds is inferred from WMAP free–free fluxes. We measure the GMC mass, the virial parameter, the star formation efficiency ϵ and the star formation rate per freefall time ϵ
ff. Both ϵ and ϵ
ff range over 3–4 orders of magnitude. We find that 68.3% of the clouds fall within

and

about the median. Compared to these observed scatters, a simple model with a time-independent ϵ
ff that depends on the host GMC properties predicts

. Allowing for a time-variable ϵ
ff, we can recover the large dispersion in the rate of star formation. This strongly suggests that star formation in the Milky Way is a dynamic process on GMC scales. We also show that the surface star formation rate profile of the Milky Way correlates well with the molecular gas surface density profile.
FROM MIRRORS TO WINDOWS: LYMAN-ALPHA RADIATIVE TRANSFER IN A VERY CLUMPY MEDIUM
Authors: Gronke Max , Dijkstra Mark , McCourt Michael , Oh S. Peng 
Published: December 2016

ABSTRACT
Lyman-alpha (Lyα) is the strongest emission line in the universe and is frequently used to detect and study the most distant galaxies. Because Lyα is a resonant line, photons typically scatter prior to escaping; this scattering process complicates the interpretation of Lyα spectra, but also encodes a wealth of information about the structure and kinematics of neutral gas in the Galaxy. Modeling the Lyα line therefore allows us to study tiny-scale features of the gas. Curiously, observed Lyα spectra can be modeled successfully with very simple, homogeneous geometries (such as an expanding, spherical shell), whereas more realistic, multiphase geometries often fail to reproduce the observed spectra. This seems paradoxical since the gas in galaxies is known to be multiphase. In this Letter, we show that spectra emerging from clumpy geometries with a large number (

for a clump column density of

) of clouds along the line of sight converge to the predictions from simplified, homogeneous models. We suggest that this resolves the apparent discrepancy and may provide a way to study the gas structure in galaxies on scales far smaller than can be probed in either cosmological simulations or direct (i.e., spatially resolved) observations.