bluuebunny/crossref_metadata_2025_split huggingface dataset:
Representación social de la memoria en una muestra universitaria de ingeniería de sistemas y antropología
Authors: Rodríguez de Ávila Ubaldo , Espitia Correa Joseph Luciano , Montenegro Arroyave Walberto Enrique , Ortiz Rúa Faissulys Milena , Suárez Colorado Yuly Paola 
Published: June 2016

Objetivo: A partir de las representaciones sociales (RS) se establecen las concepciones que determinarían la opinión, actitudes e intereses de los individuos. Materiales y métodos: El presente es un estudio cualitativo de tipo descriptivo y diseño transversal, que tuvo por objetivo identificar la RS de la memoria en estudiantes universitarios. La muestra estuvo conformada por 60 sujetos estudiantes de antropología e ingeniería de sistemas con edades entre 16 a 30 años (Media = 21,35 Desv. Tip = 3,3), quienes fueron evaluados por medio de una entrevista semiestructurada, en la que se indagó sobre la definición de la memoria y el universo semántico del constructo mediante la técnica de asociación libre. Resultados: La información obtenida fue manejada mediante las teorías de análisis del discurso y del contenido; los resultados arrojaron cuatro categorías relacionadas con la memoria: neuropsicológicas, culturales, experienciales y tecnológicas, las cuales fueron posteriormente contrastadas con las teorías científicas existentes.
Indoktrination oder Innovation?
Authors: Niethammer Verena 
Published: June 2016

Indoctrination or Innovation? Educational Film as a New Teaching Medium under National SocialismSeit 1934 wurden im Deutschen Reich von einer zentralen Stelle, der
Reichsstelle für den Unterrichtsfilm (RfdU) und seinem Nachfolger der Reichsanstalt
für Film und Bild in Wissenschaft und Unterricht (RWU), stumme, schwarz-weiße
Unterrichtsfilme als Lehrmedien für allgemeinbildende Schulen hergestellt. Von
der filmpädagogischen Diskussion begleitet, entwickelt die Filmgattung bereits
in ihrer Frühzeit spezifische Erzähl- und Darstellungsweisen, bei denen innovative
Filmtechniken und Verfahren zum Einsatz kommen. Aufgrund der Entstehungszeit
zwischen 1934 bis 1944 werden die RWU-Filme heute verdächtigt, primär der Indoktrination
der Schüler gedient zu haben. In diesem Beitrag wird anhand ausgewählter
Unterrichtsfilme und unter Berücksichtigung der RWU-Gesamtproduktion
dargelegt, dass – obwohl kaum direkte Spuren von nationalsozialistischer Ideologie
auszumachen sind – ein zweiter Blick auf den damaligen Film als Lehrmedium
nötig ist. Mit Hilfe filmanalytischer Verfahren werden hier wiederkehrende Themen
und visuellen Stereotype ausgemacht, welche die Einstellungen der Zielgruppe
prägen konnten.
RAF-Spielfilme im Geschichtsunterricht
Authors: Gerber Sophia E. 
Published: June 2016

RAF-Feature Films in History Lessons
1970 gründete eine kleine Gruppe radikaler Linker, die ursprünglich in
der frühen Studentenbewegung Westdeutschlands angesiedelt war (Andreas
Baader, Gudrun Ensslin, Horst Mahler und Ulrike Meinhof) die Rote Armee Fraktion,
RAF. Seit den frühen 1970er Jahren bis 1998 beging diese militante Gruppe zahlreiche
Terrorakte, besonders Ende 1977 als sie eine Nationalkrise auslöste, die als
der Deutsche Herbst bekannt geworden ist. Über einen Zeitraum von fast dreißig
Jahren ist sie verantwortlich zu machen für zahlreiche Verletzungen und vierunddreißig
Tode, zu denen auch viele sekundäre Ziele wie Chauffeure und Bodyguards
zählen. Obwohl die RAF erheblichen politischen Konflikt provozierte und Verbindungen
ins Ausland aufrechterhielt, wird der Linksterrorismus der RAF in der Regel
im Geschichtsunterricht behandelt. Dieser Artikel untersucht, wie das Thema über
Filme vermittelt werden kann zumal Filmregisseure seit den frühen 1970ern als
sorgfältige Beobachter politischer Ereignisse in Erscheinung treten.
PIVKA-II correlates with INR but not protein C or protein S concentrations in cord blood among newborns
Authors: Teruya M. , Soundar E. , Hui S.R. , Eldin K. , Adcock D. , Teruya J. 
Published: June 2016

BACKGROUND: Protein induced by vitamin K absence (PIVKA)-II, inactive precursor of prothrombin, is elevated in vitamin K (VK) deficiency. Our aims were to find the prevalence of VK deficiency in neonates, assess the utility of international normalized ratio (INR) as a screening tool, and explore the relationship between PIVKA-II, activated partial thromboplastin time (aPTT) and VK dependent anticoagulants. METHODS: INR, aPTT, PIVKA-II, and proteins C and S activities were measured in neonatal cord blood prior to VK administration. RESULTS: We found 45% of neonates had subclinical VK deficiency based on PIVKA-II levels and 7% based on INR. Receiver operating characteristic (ROC) analysis assessed the utility of INR in detecting >4 ng/mL of PIVKA-II and ROC of the area under the curve was 0.70 (95% CI 0.46–0.92, p = 0.07). Proteins C and S activities were normal for age and did not correlate with PIVKA-II [(r = 0.40, p = 0.14) and (r = 0.29, p = 0.29), respectively]. There was no association between aPTT and PIVKA-II ( p = 0.83). CONCLUSION: PIVKA-II seems to be a sensitive indicator of mild VK deficiency. Further studies are needed to investigate the lack of relationship between PIVKA-II and functional protein C or S levels.
THE X-SHAPED BULGE OF THE MILKY WAY REVEALED BY WISE
Authors: Ness Melissa , Lang Dustin 
Published: June 2016

ABSTRACT
The Milky Way bulge has a boxy/peanut morphology and an X-shaped structure. This X-shape has been revealed by the “split in the red clump” from star counts along the line of sight toward the bulge, measured from photometric surveys. This boxy, X-shaped bulge morphology is not unique to the Milky Way and such bulges are observed in other barred spiral galaxies. N-body simulations show that boxy and X-shaped bulges are formed from the disk via dynamical instabilities. It has also been proposed that the Milky Way bulge is not X-shaped, but rather, the apparent split in the red clump stars is a consequence of different stellar populations, in an old classical spheroidal bulge. We present a Wide-Field Infrared Survey Explorer (WISE) image of the Milky Way bulge, produced by downsampling the publicly available “unWISE” coadds. The WISE image of the Milky Way bulge shows that the X-shaped nature of the Milky Way bulge is self-evident and irrefutable. The X-shape morphology of the bulge in itself and the fraction of bulge stars that comprise orbits within this structure has important implications for the formation history of the Milky Way, and, given the ubiquity of boxy X-shaped bulges, spiral galaxies in general.
BOLOMETRIC FLUX ESTIMATION FOR COOL EVOLVED STARS
Authors: Belle Gerard T. van , J. Creech-Eakman Michelle , E. Ruiz-Velasco Alma 
Published: June 2016

ABSTRACT
Estimation of bolometric fluxes

is an essential component of stellar effective temperature determination with optical and near-infrared interferometry. Reliable estimation of

simply from broadband K-band photometry data is a useful tool in those cases were contemporaneous and/or wide-range photometry is unavailable for a detailed spectral energy distribution (SED) fit, as was demonstrated in Dyck et al. Recalibrating the intrinsic

versus observed

relationship of that study with modern SED fitting routines, which incorporate the significantly non-blackbody, empirical spectral templates of the INGS spectral library (an update of the library in Pickles) and estimation of reddening, serves to greatly improve the accuracy and observational utility of this relationship. We find that

values predicted are roughly 11% less than the corresponding values predicted in Dyck et al., indicating the effects of SED absorption features across bolometric flux curves.
RAPID EVOLUTION OF GSC 03144-595, A NEW TRIPLE-MODE RADIALLY PULSATING HIGH-AMPLITUDE δ SCUTI
Authors: Mow Benjamin , Reinhart Erik , Nhim Samantha , Watkins Richard 
Published: June 2016

ABSTRACT
We present the results of a multi-year study of the high-amplitude δ Scuti (HADS) star GSC 03144-595. The star was observed between June and September in 2011 and 2014 for 13 nights and 28 nights, respectively. Based on our results, we argue that GSC 03144-595 is a new triple-mode radially pulsating HADS, only the fifth discovered and only the second that has a fundamental frequency in the traditional δ Scuti regime. While the frequencies and amplitudes of the fundamental and first harmonic were found to be unchanged between 2011 and 2014, we found that the amplitude of the second harmonic increased by 44%, a form of evolution not previously seen. This finding suggests that the second harmonic may be transient, thus explaining the scarcity of triple-mode HADS stars.
TIME-DEPENDENT ELECTRON ACCELERATION IN BLAZAR TRANSIENTS: X-RAY TIME LAGS AND SPECTRAL FORMATION
Authors: Lewis Tiffany R. , Becker Peter A. , Finke Justin D. 
Published: June 2016

ABSTRACT
Electromagnetic radiation from blazar jets often displays strong variability, extending from radio to γ-ray frequencies. In a few cases, this variability has been characterized using Fourier time lags, such as those detected in the X-rays from Mrk 421 using BeppoSAX. The lack of a theoretical framework to interpret the data has motivated us to develop a new model for the formation of the X-ray spectrum and the time lags in blazar jets based on a transport equation including terms describing stochastic Fermi acceleration, synchrotron losses, shock acceleration, adiabatic expansion, and spatial diffusion. We derive the exact solution for the Fourier transform of the electron distribution and use it to compute the Fourier transform of the synchrotron radiation spectrum and the associated X-ray time lags. The same theoretical framework is also used to compute the peak flare X-ray spectrum, assuming that a steady-state electron distribution is achieved during the peak of the flare. The model parameters are constrained by comparing the theoretical predictions with the observational data for Mrk 421. The resulting integrated model yields, for the first time, a complete first-principles physical explanation for both the formation of the observed time lags and the shape of the peak flare X-ray spectrum. It also yields direct estimates of the strength of the shock and the stochastic magnetohydrodynamical wave acceleration components in the Mrk 421 jet.
ON THE LIMITS OF MEASURING THE BULGE AND DISK PROPERTIES OF LOCAL AND HIGH-REDSHIFT MASSIVE GALAXIES
Authors: Davari Roozbeh , Ho Luis C. , Peng Chien Y. 
Published: June 2016

ABSTRACT
A considerable fraction of the massive quiescent galaxies at z ≈ 2, which are known to be much more compact than galaxies of comparable mass today, appear to have a disk. How well can we measure the bulge and disk properties of these systems? We simulate two-component model galaxies in order to systematically quantify the effects of non-homology in structures and the methods employed. We employ empirical scaling relations to produce realistic-looking local galaxies with a uniform and wide range of bulge-to-total ratios (B/T), and then rescale them to mimic the signal-to-noise ratios and sizes of observed galaxies at z ≈ 2. This provides the most complete set of simulations to date for which we can examine the robustness of two-component decomposition of compact disk galaxies at different B/T. We confirm that the size of these massive, compact galaxies can be measured robustly using a single Sérsic fit. We can measure B/T accurately without imposing any constraints on the light profile shape of the bulge, but, due to the small angular sizes of bulges at high redshift, their detailed properties can only be recovered for galaxies with B/T ≳ 0.2. The disk component, by contrast, can be measured with little difficulty.
DETECTION AND CHARACTERIZATION OF EXOPLANETS USING PROJECTIONS ON KARHUNEN–LOEVE EIGENIMAGES: FORWARD MODELING
Authors: Pueyo Laurent 
Published: June 2016

ABSTRACT
A new class of high-contrast image analysis algorithms that empirically fit and subtract systematic noise has lead to recent discoveries of faint exoplanet/substellar companions and scattered light images of circumstellar disks. These methods are extremely efficient at enhancing the detectability of a faint astrophysical signal, but they generally create systematic biases in their observed properties. This paper provides a general solution for this outstanding problem. We present an analytical derivation of a linear expansion that captures the impact of astrophysical over-subtraction or self-subtraction in current image analysis techniques. We examine the general case for which the reference images of the astrophysical scene move azimuthally and/or radially across the field of view as a result of the observation strategy. Our new method is based on perturbing the covariance matrix underlying any least-squares speckles problem, and propagating this perturbation through the data analysis algorithm. Most of the work in this paper is presented in the Principal Component Analysis framework, but it can be easily generalized to methods relying on the linear combination of images (instead of eigenmodes). Based on this linear expansion, which is obtained in the most general case, we then demonstrate practical applications of this new algorithm. We first consider the spectral extraction of faint point sources in IFS data and illustrate, using public Gemini Planet Imager commissioning data, that our novel perturbation-based Forward Modeling, which we named Karhunen Loeve Image Processing (KLIP-FM), can indeed alleviate algorithmic biases. We then apply KLIP-FM to the detection of point sources and show how it decreases the rate of false negatives while keeping the rate of false positives unchanged when compared to classical KLIP. This can potentially have important consequences on the design of follow-up strategies of ongoing direct imaging surveys.
THE KINETIC SUNYAEV–ZEL’DOVICH EFFECT FROM REIONIZATION: SIMULATED FULL-SKY MAPS AT ARCMINUTE RESOLUTION
Authors: Alvarez Marcelo A. 
Published: June 2016

ABSTRACT
The kinetic Sunyaev–Zel’dovich (kSZ) effect results from Thomson scattering by coherent flows in the reionized intergalactic medium. We present new results based on ray-tracing an 8 Gpc/h realization of reionization with resolution elements 2 Mpc/h (subtending

′ at z = 6) on a side to create a full-sky kSZ map. The realization includes, self-consistently, the effects of reionization on scales corresponding to multipoles

. We separate the kSZ map into Doppler (

), Ostriker–Vishniac (

), patchy (

), and third-order (

) components, and compute explicitly all the auto- and cross-correlations (e.g.,

,

, etc.) that contribute to the total power. We find a complex and nonmonotonic dependence on the duration of reionization at

and evidence for a non-negligible (10%–30%) contribution from connected four-point correlations,

, usually neglected in analytical models. We also investigate the cross-correlation of linear matter and large-scale kSZ temperature fluctuations, focusing on (1) cross-power spectra with biased tracers of the matter density and (2) cold spots from infall onto large, rare H ii regions centered on peaks in the matter distribution at redshifts

that are a generic non-Gaussian feature of patchy reionization. Finally, we show that the reionization history can be reconstructed at 5σ–10σ significance by correlating full-sky 21 cm maps stacked in bins with

with existing cosmic microwave background (CMB) temperature maps at

, raising the prospects for probing reionization by correlating CMB and LSS measurements. The resulting kSZ maps have been made publicly available at www.cita.utoronto.ca/~malvarez/research/ksz-data/.
FORMATION OF MASSIVE PRIMORDIAL STARS: INTERMITTENT UV FEEDBACK WITH EPISODIC MASS ACCRETION
Authors: Hosokawa Takashi , Hirano Shingo , Kuiper Rolf , Yorke Harold W. , Omukai Kazuyuki , Yoshida Naoki 
Published: June 2016

ABSTRACT
We present coupled stellar evolution (SE) and 3D radiation-hydrodynamic (RHD) simulations of the evolution of primordial protostars, their immediate environment, and the dynamic accretion history under the influence of stellar ionizing and dissociating UV feedback. Our coupled SE RHD calculations result in a wide diversity of final stellar masses covering 10

≲ M
* ≲ 103

. The formation of very massive (≳250

) stars is possible under weak UV feedback, whereas ordinary massive (a few ×10

) stars form when UV feedback can efficiently halt the accretion. This may explain the peculiar abundance pattern of a Galactic metal-poor star recently reported by Aoki et al., possibly the observational signature of very massive precursor primordial stars. Weak UV feedback occurs in cases of variable accretion, in particular when repeated short accretion bursts temporarily exceed 0.01

, causing the protostar to inflate. In the bloated state, the protostar has low surface temperature and UV feedback is suppressed until the star eventually contracts, on a thermal adjustment timescale, to create an H ii region. If the delay time between successive accretion bursts is sufficiently short, the protostar remains bloated for extended periods, initiating at most only short periods of UV feedback. Disk fragmentation does not necessarily reduce the final stellar mass. Quite the contrary, we find that disk fragmentation enhances episodic accretion as many fragments migrate inward and are accreted onto the star, thus allowing continued stellar mass growth under conditions of intermittent UV feedback. This trend becomes more prominent as we improve the resolution of our simulations. We argue that simulations with significantly higher resolution than reported previously are needed to derive accurate gas mass accretion rates onto primordial protostars.
THE ENERGY BUDGET OF GRBs BASED ON A LARGE SAMPLE OF PROMPT AND AFTERGLOW OBSERVATIONS
Authors: Wygoda N. , Guetta D. , Mandich M. A. , Waxman E. 
Published: June 2016

ABSTRACT
We compare the isotropic equivalent 15–2000 keV γ-ray energy, E

γ
, emitted by a sample of 91 swift Gamma-Ray Bursts with known redshifts, with the isotropic equivalent fireball energy, E
fb, as estimated within the fireball model framework from X-ray afterglow observations of these bursts. The uncertainty in E

γ
, which spans the range of ∼1051 to ∼1053.5 erg, is ≈25% on average, due mainly to the extrapolation from the BAT detector band to the 15–2000 keV band. The uncertainty in E
fb is approximately a factor of 2, due mainly to the X-ray measurements’ scatter. We find E

γ
and E
fb to be tightly correlated. The average(std) of

are −0.34(0.60), and the upper limit on the intrinsic spread of η

γ
is approximately 0.5 (

is the fraction of energy carried by electrons and

is inferred from the X-ray flux at x hours).

and

are similar, with an average(std) of

of 0.04(0.28). The small variance of η

γ
implies that burst-to-burst variations in

and in the efficiency of fireball energy conversion to γ-rays are small, and suggests that both are of order unity. The small variance of η

γ
and the similarity of

and

further imply that deviations from a simple fireball model description, if present, are small. This puts stringent constraints on models incorporating such modifications (due e.g., to radiative losses, energy injection, off-axis viewing).
C IV BROAD ABSORPTION LINE ACCELERATION IN SLOAN DIGITAL SKY SURVEY QUASARS
Authors: Grier C. J. , Brandt W. N. , Hall P. B. , Trump J. R. , Filiz Ak N. , Anderson S. F. , Green Paul J. , Schneider D. P. , Sun M. , Vivek M. , Beatty T. G. , Brownstein Joel R. , Roman-Lopes Alexandre 
Published: June 2016

ABSTRACT
We present results from the largest systematic investigation of broad absorption line (BAL) acceleration to date. We use spectra of 140 quasars from three Sloan Digital Sky Survey programs to search for global velocity offsets in BALs over timescales of ≈2.5–5.5 years in the quasar rest frame. We carefully select acceleration candidates by requiring monolithic velocity shifts over the entire BAL trough, avoiding BALs with velocity shifts that might be caused by profile variability. The C iv BALs of two quasars show velocity shifts consistent with the expected signatures of BAL acceleration, and the BAL of one quasar shows a velocity-shift signature of deceleration. In our two acceleration candidates, we see evidence that the magnitude of the acceleration is not constant over time; the magnitudes of the change in acceleration for both acceleration candidates are difficult to produce with a standard disk-wind model or via geometric projection effects. We measure upper limits to acceleration and deceleration for 76 additional BAL troughs and find that the majority of BALs are stable to within about 3% of their mean velocities. The lack of widespread acceleration/deceleration could indicate that the gas producing most BALs is located at large radii from the central black hole and/or is not currently strongly interacting with ambient material within the host galaxy along our line of sight.
ALMA SCIENCE VERIFICATION DATA: MILLIMETER CONTINUUM POLARIMETRY OF THE BRIGHT RADIO QUASAR 3C 286
Authors: Nagai H. , Nakanishi K. , Paladino R. , Hull C. L. H. , Cortes P. , Moellenbrock G. , Fomalont E. , Asada K. , Hada K. 
Published: June 2016

ABSTRACT
We present full-polarization observations of the compact, steep-spectrum radio quasar 3C 286 made with the Atacama Large Millimeter and Submillimeter Array (ALMA) at 1.3 mm. These are the first full-polarization ALMA observations, which were obtained in the framework of Science Verification. A bright core and a south–west component are detected in the total intensity image, similar to previous centimeter images. Polarized emission is also detected toward both components. The fractional polarization of the core is about 17%; this is higher than the fractional polarization at centimeter wavelengths, suggesting that the magnetic field is even more ordered in the millimeter radio core than it is further downstream in the jet. The observed polarization position angle (or electric vector position angle (EVPA)) in the core is ∼39◦, which confirms the trend that the EVPA slowly increases from centimeter to millimeter wavelengths. With the aid of multi-frequency VLBI observations, we argue that this EVPA change is associated with the frequency-dependent core position. We also report a serendipitous detection of a sub-mJy source in the field of view, which is likely to be a submillimeter galaxy.
THE HE II PROXIMITY EFFECT AND THE LIFETIME OF QUASARS
Authors: Khrykin I. S. , Hennawi J. F. , McQuinn M. , Worseck G. 
Published: June 2016

ABSTRACT
The lifetime of quasars is fundamental for understanding the growth of supermassive black holes, and is an important ingredient in models of the reionization of the intergalactic medium (IGM). However, despite various attempts to determine quasar lifetimes, current estimates from a variety of methods are uncertain by orders of magnitude. This work combines cosmological hydrodynamical simulations and 1D radiative transfer to investigate the structure and evolution of the He ii Lyα proximity zones around quasars at z ≃ 3–4. We show that the time evolution in the proximity zone can be described by a simple analytical model for the approach of the He ii fraction

to ionization equilibrium, and use this picture to illustrate how the transmission profile depends on the quasar lifetime, quasar UV luminosity, and the ionization state of Helium in the ambient IGM (i.e., the average He ii fraction, or equivalently the metagalactic He ii ionizing background). A significant degeneracy exists between the lifetime and the average He ii fraction, however the latter can be determined from measurements of the He ii Lyα optical depth far from quasars, allowing the lifetime to be measured. We advocate stacking existing He ii quasar spectra at z ∼ 3, and show that the shape of this average proximity zone profile is sensitive to lifetimes as long as ∼30 Myr. At higher redshift z ∼ 4 where the He ii fraction is poorly constrained, degeneracies will make it challenging to determine these parameters independently. Our analytical model for He ii proximity zones should also provide a useful description of the properties of H i proximity zones around quasars at z ≃ 6–7.