bluuebunny/crossref_metadata_2025_split huggingface dataset:
Engineering yellow fluorescent protein probe for visualization of parallel DNA G-quadruplex
Authors: Truong Tuom TT , Phan Trang PT , Le Linh TT , Nguyen Dung H , Nguyen Hoang D , Dang Dung Thanh 
Published: November 2018

Introduction: The formation of G-quadruplex plays a key role in many biological processes. Therefore, visualization of G-quadruplex is highly essential for design of G-quadruplex-targeted small molecules (drugs). Herein, we report on an engineered fluorescent protein probe which was able to distinguish G-quadruplex topologies.
Methods: The fluorescent protein probe was generated by genetically incorporating yellow fluorescent protein (YFP) to RNA helicase associated with AU-rich element (RHAU) peptide motif.
Results: This probe could selectively bind and visualize parallel G-quadruplex structure (T95-2T) at high affinity (Kd~130 nM). Visualization of the parallel G-quadruplex by RHAU-YFP could be easily observed in vitro by using normal Gel Doc or the naked eye.
Conclusion: The YFP probe could be encoded in cells to provide a powerful tool for detection of parallel G-quadruplexes both in vitro and in vivo.
Hubungan Antara Dukungan Keluarga Dengan Gangguan Citra Tubuh Pada Penderita Kusta
Authors: Yunalia Endang Mei 
Published: November 2018

Leprosy is cronic disease caused by Mycobacterium leprae. Leprosy is not only physical disease but it also influence patien’s mental, social and economic. The purpose of this research was to identify the correlation between family support with body image disturbance on leprosy patients. This research is analytic correlation research wich used a cross sectional design. Sampling technique used purposive sampling and the sample consisted of 78 respondent. The result of this research most a half from respondent who has minimal family support have a negative body image (34,6%). Based on Contingency Coefficient test can get P-value 0,04 0,05, with Coefficien Correlation 0,353, so H0 is refused and H1 accepted , it means that there is any correlation between family support with body image disturbance on leprosy patients. Based on the result of this research, its expected the family should be given a good support. Because with good family support patients can be motivated, so that patients receive the conditions that occur and not impaired body image.
Quelques aspects des conditions de circulation des eaux souterraines dans les "karsts" du gypse des Alpes internes
Authors: Couturier Bernard , Fourneaux Jean-Claude , Sommeria Laure 
Published: November 2018

Les affleurements de gypses sont nombreux dans les Alpes internes où ils jalonnent souvent les contacts entre unités structurales différentes et plus particulièrement les chevauchements. Une morphologie caractéristique avec dolines et zones d'effondrement souligne souvent leur présence même lorsqu'ils sont masqués par des dépôts morainiques ou des éboulis. Dans ces zones on peut aussi observer des pertes ce qui traduit l'existence de circulations souterraines. Dans certains cas il n'existe pas de résurgences à caractères karstiques que l'on puisse associer à ces pertes.
A partir de deux exemples de ce type où les gypses représentent la semelle d'un chevauchement, il est possible de voir que le contexte tectonique joue un grand rôle dans les conditions de circulation des eaux souterraines.
À La Norma, en Maurienne, les eaux infiltrées dans une vaste doline ressortent en différents points après un passage au sein d'une zone à perméabilité de pores. Aucune des sources n'a un débit important et variable qui soit caractéristique des exutoires karstiques. Sur le site du Clou, en haute Tarentaise, les eaux infiltrées dans plusieurs dolines se mélangent avec des eaux ayant une autre origine et subissent ensuite une grande dispersion. Deux traçages réalisés à différentes époques ont
montré que ces eaux ressortaient à plusieurs sources qui jalonnent un grand contact anormal.
Si la partie alimentation des réseaux est tout à fait analogue à celle des réseaux karstiques classiques que l'on rencontre en milieu calcaire, il n'en est pas de même au niveau des exutoires. Dans les deux exemples étudiés la structure des gypses induit une grande dispersion et la plupart des sources ne peuvent être assimilées à des résurgences. Ces karsts semblent se vidanger dans des nappes de fissures. Cela explique l'absence de véritables résurgences. Ces nappes de Assures jouent, par ailleurs, un rôle régulateur.
L'écoulement des eaux souterraines se fait comme s'il y avait passage continu d'un système karstique à un milieu fissuré sans chenaux et même par endroits à un milieu poreux. Cela se traduit sur les débits et sur la qualité des eaux par la disparition des traces de contamination.
Ce type de circulations semble lié aux zones où la tectonique ne permet pas le développement en profondeur des réseaux de chenaux. Il y a d'une part une sorte de compression qui empêche cette formation, mais aussi un écaillage qui entraîne une interpénétration des gypses et des cargneules avec les Schistes lustrés qui représentent dans les exemples étudiés la série chevauchante comme nous avons pu l'observer dans les galeries de reconnaissance sur le site du Clou.
The Binary Fraction of Stars in Dwarf Galaxies: The Cases of Draco and Ursa Minor
Authors: Spencer Meghin E. , Mateo Mario , Olszewski Edward W. , Walker Matthew G. , McConnachie Alan W. , Kirby Evan N. 
Published: November 2018

Abstract
Measuring the frequency of binary stars in dwarf spheroidal galaxies (dSphs) requires data taken over long time intervals. We combine radial velocity measurements from five literature sources taken over the course of ∼30 years to yield the largest multi-epoch kinematic sample for stars in the dSphs Draco and Ursa Minor. With this data set, we are able to implement an improved version of the Bayesian technique described in Spencer et al. to evaluate the binary fraction of red giant stars in these dwarf galaxies. Assuming Duquennoy & Mayor period and mass ratio distributions, the binary fractions in Draco and Ursa Minor are

and

, respectively. We find that a normal mass ratio distribution is preferred over a flat distribution, and that log-normal period distributions centered on long periods (

) are preferred over distributions centered on short ones. We reanalyzed the binary fractions in Leo II, Carina, Fornax, Sculptor, and Sextans, and find that there is <1% chance that binary fraction is a constant quantity across all seven dwarfs, unless the period distribution varies greatly. This indicates that the binary populations in Milky Way dSphs are not identical in regard to their binary fractions, period distributions, or both. We consider many different properties of the dwarfs (e.g., mass, radius, luminosity, etc.) and find that binary fraction might be larger in dwarfs that formed their stars quickly and/or have high velocity dispersions.
The California-Kepler Survey. VI. Kepler Multis and Singles Have Similar Planet and Stellar Properties Indicating a Common Origin∗
Authors: Weiss Lauren M. , Isaacson Howard T. , Marcy Geoffrey W. , Howard Andrew W. , Petigura Erik A. , Fulton Benjamin J. , Winn Joshua N. , Hirsch Lea , Sinukoff Evan , Rowe Jason F. ,   The California Kepler Survey
Published: November 2018

Abstract
The California-Kepler Survey (CKS) catalog contains precise stellar and planetary properties for the Kepler planet candidates, including systems with multiple detected transiting planets (“multis”) and systems with just one detected transiting planet (“singles”, although additional planets could exist). We compared the stellar and planetary properties of the multis and singles in a homogeneous subset of the full CKS-Gaia catalog. We found that sub-Neptune-sized singles and multis do not differ in their stellar properties or planet radii. In particular: (1.) The distributions of stellar properties

, [Fe/H], and

for the Kepler sub-Neptune-sized singles and multis are statistically indistinguishable. (2.) The radius distributions of the sub-Neptune-sized singles and multis with P > 3 days are indistinguishable, and both have a valley at ∼1.8

. However, there are significantly more detected short-period (P < 3 days), sub-Neptune-sized singles than multis. The similarity of the host-star properties, planet radii, and radius valley for singles and multis suggests a common origin. The similar radius valley, which is likely sculpted by photo-evaporation from the host star within the first 100 Myr, suggests that planets in both singles and multis spend much of the first 100 Myr near their present, close-in locations. One explanation that is consistent with the similar fundamental properties of singles and multis is that many of the singles are members of multi-planet systems that underwent planet–planet scattering.
Limits on Clouds and Hazes for the TRAPPIST-1 Planets
Authors: Moran Sarah E. , Hörst Sarah M. , Batalha Natasha E. , Lewis Nikole K. , Wakeford Hannah R. 
Published: November 2018

Abstract
The TRAPPIST-1 planetary system is an excellent candidate for study of the evolution and habitability of M-dwarf-hosted planets. Transmission spectroscopy observations performed on the system with the Hubble Space Telescope (HST) suggest that the innermost five planets do not possess clear hydrogen atmospheres. Here we reassess these conclusions with recently updated mass constraints. Additionally, we expand the analysis to include limits on metallicity, cloud top pressure, and the strength of haze scattering. We connect recent laboratory results of particle size and production rate for exoplanet hazes to a one-dimensional atmospheric model for TRAPPIST-1 transmission spectra. In this way, we obtain a physically based estimate of haze scattering cross sections. We find haze scattering cross sections on the order of 10−26–10−19 cm2 are needed in modeled hydrogen-rich atmospheres for TRAPPIST-1 d, e, and f to match the HST data. For TRAPPIST-1 g, we cannot rule out a clear hydrogen-rich atmosphere. We model the effects an opaque cloud deck and substantial heavy element content have on the transmission spectra using the updated mass estimates. We determine that hydrogen-rich atmospheres with high-altitude clouds, at pressures of 12 mbar and lower, are consistent with the HST observations for TRAPPIST-1 d and e. For TRAPPIST-1 f and g, we cannot rule out clear hydrogen-rich cases to high confidence. We demonstrate that metallicities of at least 60× solar with tropospheric (0.1 bar) clouds are in agreement with observations. Additionally, we provide estimates of the precision necessary for future observations to disentangle degeneracies in cloud top pressure and metallicity. For TRAPPIST-1 e and f, for example, 20 ppm precision is needed to distinguish between a clear atmosphere and one with a thick cloud layer at 0.1 bar across a wide range (1× to 1000× solar) of metallicity. Our results suggest secondary, volatile-rich atmospheres for the outer TRAPPIST-1 planets d, e, and f.
Tracing Outflowing Metals in Simulations of Dwarf and Spiral Galaxies
Authors: Christensen Charlotte R. , Davé Romeel , Brooks Alyson , Quinn Thomas , Shen Sijing 
Published: November 2018

Abstract
We analyze the metal accumulation in dwarf and spiral galaxies by following the history of metal enrichment and outflows in a suite of 20 high-resolution simulated galaxies. These simulations agree with the observed stellar and gas-phase mass–metallicity relation, an agreement that relies on large fractions of the produced metals escaping into the circumgalactic media. For instance, in galaxies with M
vir ∼ 109.5–1010

, we find that about ∼85% of the available metals are outside of the galactic disk at z = 0, although the fraction decreases to a little less than half in Milky-Way-mass galaxies. In many cases, these metals are spread far beyond the virial radius. We analyze the metal deficit within the ISM and stars in the context of previous work tracking the inflow and outflow of baryons. Outflows are prevalent across the entire mass range, as is reaccretion. We find that between 40% and 80% of all metals removed from the galactic disk are later reaccreted. The outflows themselves are metal-enriched relative to the ISM by a factor of 0.2 dex because of the correspondence between sites of metal enrichment and outflows. As a result, the metal mass loading factor scales as

, a somewhat shallower scaling than the total mass loading factor. We analyze the simulated galaxies within the context of analytic chemical evolution models by determining their net metal expulsion efficiencies, which encapsulate the rates of metal loss and reaccretion. We discuss these results in light of the inflow and outflow properties necessary for reproducing the mass–metallicity relation.
Resolving Star Formation on Subkiloparsec Scales in the High-redshift Galaxy SDP.11 Using Gravitational Lensing*
Authors: Lamarche C. , Verma A. , Vishwas A. , Stacey G. J. , Brisbin D. , Ferkinhoff C. , Nikola T. , Higdon S. J. U. , Higdon J. , Tecza M. 
Published: November 2018

Abstract
We investigate the properties of the interstellar medium, star formation, and the current-day stellar population in the strongly lensed star-forming galaxy H-ATLAS J091043.1-000321 (SDP.11), at z = 1.7830, using new Herschel and Atacama Large Millimeter/submillimeter Array (ALMA) observations of far-infrared fine-structure lines of carbon, oxygen, and nitrogen. We report detections of the [O iii] 52 μm, [N iii] 57 μm, and [O i] 63 μm lines from Herschel/PACS, and present high-resolution imaging of the [C ii] 158 μm line, and underlying continuum, using ALMA. We resolve the [C ii] line emission into two spatially offset Einstein rings, tracing the red and blue velocity components of the line, in the ALMA/Band 9 observations at 0.″2 resolution. The values seen in the [C ii]/far-infrared (FIR) ratio map, as low as ∼0.02% at the peak of the dust continuum, are similar to those of local ULIRGs, suggesting an intense starburst in this source. This is consistent with the high intrinsic FIR luminosity (∼3 × 1012
L
⊙), ∼16 Myr gas depletion timescale, and ≲8 Myr timescale since the last starburst episode, estimated from the hardness of the UV radiation field. By applying gravitational lensing models to the visibilities in the uv-plane, we find that the lensing magnification factor varies by a factor of two across SDP.11, affecting the observed line profiles. After correcting for the effects of differential lensing, a symmetric line profile is recovered, suggesting that the starburst present here may not be the result of a major merger, as is the case for local ULIRGs, but instead could be powered by star formation activity spread across a 3–5 kpc rotating disk.
OGLE-2017-BLG-0039: Microlensing Event with Light from a Lens Identified from Mass Measurement
Authors: Han C. , Jung Y. K. , Udalski A. , Bond I. , Bozza V. , Albrow M. D. , Chung S.-J. , Gould A. , Hwang K.-H. , Kim D. , Lee C.-U. , Kim H.-W. , Ryu Y.-H. , Shin I.-G. , Yee J. C. , Shvartzvald Y. , Cha S.-M. , Kim S.-L. , Kim D.-J. , Lee D.-J. , Lee Y. , Park B.-G. , Pogge R. W. ,   (The KMTNet Collaboration), Szymański M. K. , Mróz P. , Skowron J. , Poleski R. , Soszyński I. , Kozłowski S. , Pietrukowicz P. , Ulaczyk K. , Pawlak M. ,   (The OGLE Collaboration), Abe F. , Barry R. , Bennett D. P. , Bhattacharya A. , Donachie M. , Evans P. , Fukui A. , Hirao Y. , Itow Y. , Kawasaki K. , Koshimoto N. , Li M. C. A. , Ling C. H. , Matsubara Y. , Miyazaki S. , Munakata H. , Muraki Y. , Nagakane M. , Ohnishi K. , Ranc C. , Rattenbury N. , Saito T. , Sharan A. , Sullivan D. J. , Sumi T. , Suzuki D. , Tristram P. J. , Yamada T. , Yonehara A. ,   (The MOA Collaboration)
Published: November 2018

Abstract
We present an analysis of the caustic-crossing binary microlensing event OGLE-2017-BLG-0039. Thanks to the very long duration of the event, with a time scale t
E ∼ 130 days, the microlens parallax is measured precisely despite its low value of

. Analysis of the well-resolved caustic crossings during the source star’s entrance and exit of the caustic yields an angular Einstein radius of

mas. The measured

and

indicate that the lens is a binary composed of two stars with masses

and ∼0.15 M
⊙, and is located at a distance of ∼6 kpc. From the color and brightness of the lens estimated from its determined mass and distance, it is expected that ∼2/3 of the I-band blended flux comes from the lens. Therefore, the event is a rare case of a bright lens event for which high-resolution follow-up observations can confirm its nature.
SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IIn
Authors: Chen T.-W. , Inserra C. , Fraser M. , Moriya T. J. , Schady P. , Schweyer T. , Filippenko A. V. , Perley D. A. , Ruiter A. J. , Seitenzahl I. , Sollerman J. , Taddia F. , Anderson J. P. , Foley R. J. , Jerkstrand A. , Ngeow C.-C. , Pan Y.-C. , Pastorello A. , Points S. , Smartt S. J. , Smith K. W. , Taubenberger S. , Wiseman P. , Young D. R. , Benetti S. , Berton M. , Bufano F. , Clark P. , Valle M. Della , Galbany L. , Gal-Yam A. , Gromadzki M. , Gutiérrez C. P. , Heinze A. , Kankare E. , Kilpatrick C. D. , Kuncarayakti H. , Leloudas G. , Lin Z.-Y. , Maguire K. , Mazzali P. , McBrien O. , Prentice S. J. , Rau A. , Rest A. , Siebert M. R. , Stalder B. , Tonry J. L. , Yu P.-C. 
Published: November 2018

Abstract
We present observations of supernova (SN) 2017ens, discovered by the ATLAS survey and identified as a hot blue object through the GREAT program. The redshift z = 0.1086 implies a peak brightness of M

g
= −21.1 mag, placing the object within the regime of superluminous supernovae. We observe a dramatic spectral evolution, from initially being blue and featureless, to later developing features similar to those of the broadlined Type Ic SN 1998bw, and finally showing ∼2000 km s−1 wide Hα and Hβ emission. Relatively narrow Balmer emission (reminiscent of a SN IIn) is present at all times. We also detect coronal lines, indicative of a dense circumstellar medium. We constrain the progenitor wind velocity to ∼50–60 km s−1 based on P-Cygni profiles, which is far slower than those present in Wolf–Rayet stars. This may suggest that the progenitor passed through a luminous blue variable phase, or that the wind is instead from a binary companion red supergiant star. At late times we see the ∼2000 km s−1 wide Hα emission persisting at high luminosity (∼3 × 1040 erg s−1) for at least 100 day, perhaps indicative of additional mass loss at high velocities that could have been ejected by a pulsational pair instability.
Le travail, peut-il encore être la santé ?
Authors: Di Liberatore Dominique 
Published: November 2018

Le travail tel qu’il faut le considérer aujourd’hui, avec son organisation, sa répartition des tâches et des fonctions, avec sa gestion et sa communication, avec toutes les avancées sociales que ce soit la législation, la sécurité, les assurances, avec aussi toutes les diverses instances, internes ou externes à l’entreprise, ce travail donc, offre-t-il encore aux personnes un lieu de sublimation, de transfert ou de répétition de leurs problématiques personnelles ? Et jusqu’à quel point ne les crée-t-il pas ou ne les aggrave-t-il pas ?
L’opéra italien à la cour de France : réception et adaptation d’un objet étranger (1645-1662)
Authors: Nestola Barbara 
Published: November 2018

Si les circonstances de la réception de l’opéra italien en France au xviie siècle sont aujourd’hui connues, il reste tout de même encore des questions ouvertes concernant les modalités effectives de l’acclimatation de ce répertoire à la cour. Malgré les efforts de Mazarin pour italianiser le milieu musical français, les opéras italiens donnés entre 1645 et 1662 ont été soumis à des réadaptations orientées vers une francisation, de nature artistique ou politique, au moment d’être présentés au public de la cour. Ce processus s’est déroulé par phases et en suivant plusieurs étapes : dans les années 1645-1647, il concerne principalement le texte et la musique des opéras, tandis que dans la période suivante, 1654-1662, les remaniements interviennent d’une manière plus envahissante par l’insertion d’éléments issus de genres musicaux français, tel le ballet de cour. Parallèlement, avec l’entrée du roi dans l’âge adulte, l’ingérence d’éléments politiques se fait tangible, notamment après la disparition de Mazarin. Le propos de cette étude est d’explorer ce croisement d’influences et de montrer comment l’objet « opéra italien » a progressivement été dévêtu de ses connotations artistiques saillantes pour répondre aux enjeux de nature artistique et politique propres au contexte de la cour dans la période charnière de la passation du pouvoir entre Mazarin et Louis XIV.
Reconstituer Marly
Authors: Queval Hélène 
Published: November 2018

De formation académique, gravitant autour d’Eugène Viollet-le-Duc et participant à de nombreuses éditions d’ouvrages d’architecture, ainsi qu’annuellement au Salon des artistes français, le dessinateur et graveur d’architecture Auguste-Alexandre Guillaumot (1815-1892) resta associé au domaine de Marly, qu’il arpenta à maintes reprises pendant trente ans à la recherche de points de vue à croquer et qu’il chercha à faire revivre dans sa monographie. Par une consultation assidue des dessins et estampes témoignant de l’apparence du château de Marly et conservés à la Bibliothèque nationale de France et aux Archives nationales, ainsi que par l’étude des vestiges exhumés lors des premières fouilles sur le site réalisées à son instigation, Guillaumot s’attela à la difficile tâche d’évoquer un monument disparu quasi intégralement depuis un demi-siècle. Il mit en œuvre une réflexion intellectuelle et artistique originale, mêlant archéologie de papier et archéologie de terrain. Ses croquis, conservés en grand nombre au Musée-Promenade de Marly-le-Roi / Louveciennes, témoignent des sources iconographiques consultées et des étapes artistiques entre le matériau archivistique et les gravures finales.
Impact of demographic variables on emotional intelligence levels amongst a sample of early career academics at a South African higher education institution
Authors: Marembo Matthew , Chinyamurindi Willie T. 
Published: November 2018

Orientation: Emotional intelligence (EI) is highlighted by the literature as an important attribute that enables an individual to cope with changes and pressures in the work environment and subsequently yields consistent performance. However, some scholars debate the role of demographic diversities and their impact on levels of EI amongst individuals.Research purpose: This study examined the influence of demographic variables on EI levels amongst early career academics (ECAs).Motivation for the study: The study interrogates demographic variables and EI, two issues important in the 21st-century workforce setting. The relationship between the two may be of value to the debate surrounding the success of early career professionals in the higher education sector. The success of ECAs should be of importance to institutions of higher learning.Research approach/design and method: A quantitative approach was followed in conducting the study. Data were collected from a sample of 220 ECAs in a selected university in South Africa. A self-administered questionnaire was sent to the participants using SurveyMonkey online data collection tool. EI was measured using the Schutte Emotional Intelligence Scale.Main findings: Significant EI level differences were observed based on the participants’ ethnic background. However, no significant differences in EI levels could be found based on the respondents’ gender, age and work experience.Practical/managerial implications: The findings may be relevant to career management and human resources forecasting.Contribution/value-add: The study adds to the literature on EI and career success of early career professionals.