bluuebunny/crossref_metadata_2025_split huggingface dataset:
A Neuropsychological Profile for Agenesis of the Corpus Callosum? Cognitive, Academic, Executive, Social, and Behavioral Functioning in School-Age Children
Authors: Siffredi Vanessa , Anderson Vicki , McIlroy Alissandra , Wood Amanda G. , Leventer Richard J. , Spencer-Smith Megan M. 
Published: March 2018

AbstractObjectives:Agenesis of the corpus callosum (AgCC), characterized by developmental absence of the corpus callosum, is one of the most common congenital brain malformations. To date, there are limited data on the neuropsychological consequences of AgCC and factors that modulate different outcomes, especially in children. This study aimed to describe general intellectual, academic, executive, social and behavioral functioning in a cohort of school-aged children presenting for clinical services to a hospital and diagnosed with AgCC. The influences of age, social risk and neurological factors were examined.Methods:Twenty-eight school-aged children (8 to 17 years) diagnosed with AgCC completed tests of general intelligence (IQ) and academic functioning. Executive, social and behavioral functioning in daily life, and social risk, were estimated from parent and teacher rated questionnaires. MRI findings reviewed by a pediatric neurologist confirmed diagnosis and identified brain characteristics. Clinical details including the presence of epilepsy and diagnosed genetic condition were obtained from medical records.Results:In our cohort, ~50% of children experienced general intellectual, academic, executive, social and/or behavioral difficulties and ~20% were functioning at a level comparable to typically developing children. Social risk was important for understanding variability in neuropsychological outcomes. Brain anomalies and complete AgCC were associated with lower mathematics performance and poorer executive functioning.Conclusions: This is the first comprehensive report of general intellectual, academic, executive social and behavioral consequences of AgCC in school-aged children. The findings have important clinical implications, suggesting that support to families and targeted intervention could promote positive neuropsychological functioning in children with AgCC who come to clinical attention. (JINS, 2018,24, 445–455)
A cross-sectional survey of nutrition labelling use and its associated factors on parents of school students in Shanghai, China
Authors: Ma Jianhong , Zhu Zhenxin , Chen Xiao , Guo Yan , Zhang Huansheng , Zhang Yuyan , Zang Jiajie 
Published: March 2018

AbstractObjectiveTo understand parents’ knowledge and use of nutrition labelling and to explore its associated factors.DesignCross-sectional survey.SettingTwo schools providing a nine-year educational programme in Putuo District, Shanghai, China, were selected for the study. Information was included on demographic data and knowledge of the Chinese Food Pagoda.SubjectsStudents and their parents (n 1770) participated in a questionnaire survey.ResultsOf questionnaires, 1766 were completed (response rate 99·8 %). Utilization rate of nutrition labelling was 19·3 %. Among 624 parents knowing nutrition labelling, 22·1 % understood all the information included, 70·7 % understood it partially and 7·2 % could not understand it at all. Use of nutrition labelling by parents was related to the following factors (OR; 95 % CI): high educational level of parent (1·465; 1·165, 1·841), parent’s knowledge of the Chinese Food Pagoda (1·333; 1·053, 1·688), parent’s consumption of top three snacks which are unhealthy (1·065; 1·023, 1·109), parent’s assumption that nutrition labelling would affect their choice of food (1·522; 1·131, 2·048), student’s willingness to learn about labels (1·449; 1·093, 1·920) and student’s knowledge and use of labels (2·214; 1·951, 2·513).ConclusionsParents’ knowledge and use of nutrition labelling are still at a lower level, and some information included in the nutrition labels is not understood by parents. The forms of the existing nutrition labelling need to be continuously improved to facilitate their understanding and usefulness. It is necessary to establish nutrition projects focusing on education and use of nutrition labels which help parents and their children make the right choices in selecting foods.
Tc-trend and terrestrial planet formation: The case of Zeta Reticuli
Authors: Adibekyano V. , Delgado-Mena E. , Santos N. C. , Sousa S. G. , Figueira P. 
Published: March 2018

AbstractSome studies suggested that the chemical abundance trend with the condensation temperature, Tc, is a signature of rocky planet formation. Very recently, a strong Tc trend was reported in ζ2 Ret relative to its companion (ζ1 Ret) and was explained by the presence of a debris disk around ζ2 Ret. We re-evaluated the presence and variability of the Tc trend in this system with a goal to understand the impact of the presence of the debris disk on a star. Our results confirm the reported abundance difference between ζ2 Ret and ζ1 Ret and its dependence on the Tc. However, we also found that the Tc trends depend on the individual spectrum used. We conclude that for the ζ Reticuli system, for example, nonphysical factors can be at the root of the Tc trends for the case of individual spectra. For more details see Adibekyan et al. (2016b).
The white dwarf mass-radius relation with Gaia, Hubble and FUSE
Authors: Joyce Simon R. G. , Barstow Martin A. , Casewell Sarah L. , Holberg Jay B. , Bond Howard E. 
Published: March 2018

AbstractWhite dwarfs are becoming useful tools for many areas of astronomy. They can be used as accurate chronometers over Gyr timescales. They are also clues to the history of star formation in our galaxy. Many of these studies require accurate estimates of the mass of the white dwarf. The theoretical mass-radius relation is often invoked to provide these mass estimates. While the theoretical mass-radius relation is well developed, observational tests of this relation show a much larger scatter in the results than expected. High precision observational tests to confirm this relation are required. Gaia is providing distance measurements which will remove one of the main source of uncertainty affecting most previous observations. We combine Gaia distances with spectra from the Hubble and FUSE satelites to make precise tests of the white dwarf mass-radius relation.
Observational Facilities of Sternberg Astronomical Institute for Ground-Based Photometric Study of Newly Identified GAIA Objects, — CV-candidates.
Authors: Voloshina Irina , Sementsov Valerian 
Published: March 2018

AbstractThe extended observational program for study of cataclysmic variables is realized in Sternberg Astronomical Institute during the last years. A few telescopes of Crimean Observational Station equipped with a different devices, — UBV photometer and two CCD camera, are used for observations. Among the close binary systems (CBS), cataclysmic variables are the most interesting objects because of the outburst activity and variety of their observational features. They could serve a good laboratory for study of physical processes in CBS. GAIA provides astronomers with a new ample opportunity for investigation of cataclysmic variables. Though the relative faintness of detected objects it is still possible to carry out a high accuracy ground-based observations with our equipment. Obtained ground-based data permit us to confirm classification of detected CV-candidates, to determine the physical characteristics with a sample of new cods and improve the current understanding of their nature.
Stellar Parameters, Chemical composition and Models of chemical evolution
Authors: Mishenina T. , Pignatari M. , Côté B. , Thielemann F.-K. , Soubiran C. , Basak N. , Gorbaneva T. , Korotin S. A. , Kovtyukh V. V. , Wehmeyer B. , Bisterzo S. , Travaglio C. , Gibson B. K. , Jordan C. , Paul A. , Ritter C. , Herwig F. 
Published: March 2018

AbstractWe present an in-depth study of metal-poor stars, based high resolution spectra combined with newly released astrometric data from Gaia, with special attention to observational uncertainties. The results are compared to those of other studies, including Gaia benchmark stars. Chemical evolution models are discussed, highlighting few puzzles that are still affecting our understanding of stellar nucleosynthesis and of the evolution of our Galaxy.
Massive companions of binary systems
Authors: Jableka D. , Zola S. , Zakrzewski B. , Kreiner J. M. , Ogloza W. 
Published: March 2018

AbstractWe examined the O-C diagrams of eclipsing binary systems and selected these exhibiting cyclic shape, either sinusoidal or quasi sinusoidal. Assuming these variations being due to the Light Time Travel effect (LTE), we estimated the parameters of companions with the Monte Carlo method. As a result, we identified nearly two dozen of eclipsing systems that might have companions with a minimum mass larger than that of a neutron star. Their masses fall into the range between 1.7 and 34 solar masses. This sample of triples with high mass companions can be confirmed with the help of observations gathered by Gaia: parallaxes and astrometric measurements.
The LQAC-4, last update of the Large Quasar Astrometric Catalogue
Authors: Souchay J. , Andrei A. H. , Barache C. , Taris F. , Gattano C. , Coelho B. 
Published: March 2018

AbstractThanks to their point-like structure and to their lack of significant proper motion, quasars represent the ideal objects for modeling quasi-inertial directions in space. For that reason the present primary conventional reference frame, the ICRF-2, is constructed from the set of the celestial coordinates of a sample of extragalactic objects, whose the very large majority are quasars. Thus any newly discovered quasar must be considered as a potential future ideal astrometric marker. Therefore compiling all the recorded quasars at a given epoch looks as a useful task. This constitutes the aim of the LQAC (Large Quasar Astrometric Catalogue). We present here the contents of the future release of this catalogue quoted as the LQAC-4, insisting on the related strategy of compilation. Preliminary results concerning the cross-identification with the Gaia DR1 catalogue are emphasized
Searching for planets around eclipsing binary stars using timing method: NSVS 14256825
Authors: Nasiroglu Ilham , Goździewski Krzysztof , Słowikowska Aga , Krzeszowski Krzysztof , Żejmo Michal , Zola Staszek , Er Huseyin 
Published: March 2018

AbstractWe present four new mid eclipse times and an updated O-C diagram of the short period eclipsing binary NSVS14256825. The new data follow the (O-C) trend and its model proposed in Nasiroglu et al. (2017). The (O-C) diagram shows quasi-periodic variations that can be explained with the presence of a brown-dwarf in a quasi-circular circumbinary orbit.
CNO distributions in the Solar neighborhood with Gaia data
Authors: Mikolaitis Šarūnas , Tautvaišienė Gražina , Ženovienė Renata , Drazdauskas Arnas , Pakštienė Erika , Janulis Rimvydas , Bagdonas Vilius , Klebonas Lukas 
Published: March 2018

AbstractA spread of lifebuilding elements, such as carbon, nitrogen, and oxygen in the Galactic discs is yet not well investigated. In this study, we use spectra from the UVES spectrograph (Gaia-ESO survey ) and the VUES spectograph (SPFOT-PLATO survey) and determine the carbon, nitrogen, and oxygen abundances in FGK stars using the same technique. For some of our target stars the Gaia space observatory has already presented accurate distances, thus we overview the first results of radial and vertical CNO abundance distributions in the Galactic thin and thick disc populations.
What we learn from TGAS about the moving groups of the Solar neighbourhood
Authors: Goldman B. , Schilbach E. , Röser S. , Schöfer P. , Derekas A. , Moor A. , Brandner W. , Henning T. 
Published: March 2018

AbstractWe use the TGAS proper motions and parallaxes as well as published and new radial velocities to study the dynamics of nearby moving groups. In particular we try to determine their age using backtracing of the individual members to a common origin. We find that the current data, probably the radial velocities, do not allow to reach a successful conclusion.
Understanding Li enhancement in K giants and role of accurate parallaxes
Authors: singh Raghubar , Reddy B. E. 
Published: March 2018

AbstractOur recent studies based on a large sample of K giants with Hipparcos parallaxes and spectroscopic analysis resulted more than a dozen new Li-rich K giants including few super Li-rich ones. Most of the Li-rich K giants including the new ones appear to occur at the luminosity bump in the HR diagram. However, one can’t rule out the possibility of overlap with the clump region where core He-burning K giants reside post He-flash at the tip of RGB. It is important to distinguish field K giants of clump from the bump region in the HR diagram to understand clues for Li production in K giants. In this poster, we explore whether GAIA parallaxes improve to disentangle clump from bump region, more precisely.
Follow-up studies of Gaia transients at the Terskol Observatory
Authors: Godunova Vira , Reshetnyk Volodymyr , Simon Andrii , Velichko Sergii , Sergeev Oleksandr , Taradii Volodymyr 
Published: March 2018

AbstractSince 2015, scientific activities at the Terskol Observatory have been aimed at optical follow-up of stellar objects and asteroids detected within the framework of the Gaia mission. Two years of successful research have yielded new data and findings in this field. Photometric observations of Gaia transients allowed us to reveal physical characteristics of a good few of them. Moreover, we detected positions of dozens of asteroids which were reported by the GBOT group. In this paper, some results obtained from observations of transients Gaia16bkf, Gaia16bkn, Gaia17asz and newly detected asteroids are presented.
On-sky verification of the 6-h periodic basic angle variations of the Gaia satellite
Authors: Liao Shilong , Lattanzi Mario G. , Vecchiato Alberto , Qi Zhaoxiang , Crosta Mariateresa , Tang Zhenghong 
Published: March 2018

AbstractA Basic Angle (BA) of 106.5° separates the view directions of Gaia's two fields of view (FoV). A precise determination of the BA variations (BAV) is essential to guarantee a correct reconstruction of the global astrometric sphere, as residual systematic errors would result in, e.g., a bias in the parallaxes of the final Gaia catalog. The Basic Angle Monitoring (BAM) device, which provides a reliable and accurate estimation of BAV, shows that there exists a ~1 mas amplitude, 6-h period BA oscillation. It's essential to verify to what extent this signal is caused by real BAV, or is at least in part an effect of the BAM device itself. Here, we propose an astrometric on-sky approach to re-determine the 6-h periodic BAV. The results of this experiment, which treated a full day (17 Oct 2016) of Gaia astrometric data, recover a value for the 6-h oscillation of 1.856±0.857 mas. This is consistent, within the errors, with the BAM finding for that day.
Dynamical effects of the spiral arms on the velocity distribution of disc stars
Authors: Hattori Kohei , Gouda Naoteru , Yano Taihei , Sakai Nobuyuki , Tagawa Hiromichi 
Published: March 2018

AbstractNearby disc stars in Gaia DR1 (TGAS) and RAVE DR5 show a bimodal velocity distribution in the metal-rich region (characterized by the Hercules stream) and mono-modal velocity distribution in the metal-poor region. We investigate the origin of this [Fe/H] dependence of the local velocity distribution by using 2D test particle simulations. We found that this [Fe/H] dependence can be well reproduced if we assume fast rotating bar models with Ωbar ≃ 52 km s−1 kpc−1. A possible explanation for this result is that the metal-rich, relatively young stars are more likely to be affected by bar's outer Lindblad resonance due to their relatively cold kinematics. We also found that slowly rotating bar models with Ωbar ≃ 39 km s−1 kpc−1 can not reproduce the observed data. Interestingly, when we additionally consider spiral arms, some models can reproduce the observed velocity distribution even when the bar is slowly rotating.
Open Cluster Dynamics via Fundamental Plane
Authors: Lin Chien-Cheng , Pang Xiao-Ying 
Published: March 2018

AbstractOpen clusters (OCs) are important objects for stellar dynamics studies. The short survival timescale of OCs makes them closely related to the formation of Galactic field stars. We motivate to investigate the dynamical evolution of OCs on the aspect of internal effect and the external influence. Firstly, we make use of the known OC catalog to obtain OCs masses, effective radii. Additionally, we estimate OCs kinematics properties by OC members cross-matched with radial velocity and metallicity from SDSSIV/APOGEE2. We then establish the fundamental plane of OCs based on the radial velocity dispersion, the effective radius, and average surface brightness. The deviation of the fundamental plane from the Virial Plane, so called the tilt, and the r.m.s. dispersion of OCs around the average plane are used to indicate the dynamical status of OCs. Parameters of the fitted plane will vary with cluster age and distance.
Stellar parameters with FASMA: a new spectral synthesis package
Authors: Tsantaki M. , Andreasen D. T. , Teixeira G. D. C. , Sousa S. G. , Santos N. C. , Delgado-Mena E. , Bruzual G. 
Published: March 2018

AbstractCurrent Galactic surveys, including the Gaia mission, rely on the efficiency of the spectral analysis techniques to provide precise and accurate spectral information (i.e. effective temperature, surface gravity, metallicity, and chemical abundances) in the shortest computational time. In this work, we present a new package to preform complete spectral analyses based on the spectral synthesis technique (Tsantaki et al. 2017, submitted). We focus on deriving atmospheric parameters for FGK-type stars using both high and medium resolution (GIRAFFE) spectra. This method is implemented on the Gaia-ESO benchmark stars to confirm its validity, achieving similar accuracy for the two resolution setups.
Precise CCD positions of Triton in 2014-2016 from the Gaia DR1
Authors: Wang N. , Peng Q. Y. , Peng H. W. , Zhang Q. F. 
Published: March 2018

Abstract755 CCD observations during the years 2014-2016 have been reduced to derive the precise positions of Triton, the first satellite of Neptune. The observations were made by the 1 m telescope at Yunnan Observatory over 15 nights during the years 2014-2016. The theoretical position of Triton was retrieved from the Jet Propulsion Laboratory Horizons system. Our results show that when the newest Gaia catalogue (Gaia DR1) is referred to the mean O-Cs (observed minus computed) residuals are about 0.042 and -0.006 arcsec, the dispersions are 0.012 and 0.012 arcsec in right ascension and declination, respectively. The dispersions are improved very significantly when the Gaia DR1 is referred to. However, the agreement in right ascension is not so good as that in declination, the reason might come from the uncertainty of planet ephemeris. More observations are needed to confirm this.
Shape and spin of asteroid 967 Helionape
Authors: Apostolovska G. , Kostov A. , Donchev Z. , Bebekovska E. Vchkova , Kuzmanovska O. 
Published: March 2018

AbstractKnowledge of the spin and shape parameters of the asteroids is very important for understanding of the conditions during the creation of our planetary system and formation of asteroid populations. The main belt asteroid and Flora family member 967 Helionape was observed during five apparitions. The observations were made at the Bulgarian National Astronomical Observatory (BNAO) Rozhen, since March 2006 to March 2016. Lihtcurve inversion method (Kaasalainen et al. (2001)), applied on 12 relative lightcurves obtained at various geometric conditions of the asteroid, reveals the spin vector, the sense of rotation and the preliminary shape model of the asteroid. Our aim is to contribute in increasing the set of asteroids with known spin and shape parameters. This could be done with dense lightcurves, obtained during small number of apparitions, in combination with sparse data produced by photometric asteroid surveys such as the Gaia satellite (Hanush (2011)).
The kinematics of the white dwarf population from the SDSS DR12
Authors: Anguiano B. , Rebassa-Mansergas A. , García-Berro E. , Torres S. , Freeman K. , Zwitter T. 
Published: March 2018

AbstractWe use the Sloan Digital Sky Survey Data Release 12, which is the largest available white dwarf catalog to date, to study the evolution of the kinematical properties of the population of white dwarfs in the Galactic disc. We derive masses, ages, photometric distances and radial velocities for all white dwarfs with hydrogen-rich atmospheres. For those stars for which proper motions from the USNO-B1 catalog are available the true three-dimensional components of the stellar space velocity are obtained. This subset of the original sample comprises 20,247 objects, making it the largest sample of white dwarfs with measured three-dimensional velocities. Furthermore, the volume probed by our sample is large, allowing us to obtain relevant kinematical information. In particular, our sample extends from a Galactocentric radial distance RG = 7.8 kpc to 9.3 kpc, and vertical distances from the Galactic plane ranging from Z = −0.5 kpc to 0.5 kpc. We examine the mean components of the stellar three-dimensional velocities, as well as their dispersions with respect to the Galactocentric and vertical distances. We confirm the existence of a mean Galactocentric radial velocity gradient, ∂〈VR〉/∂RG = −3 ± 5 km s−1 kpc−1. We also confirm North-South differences in 〈Vz〉. Specifically, we find that white dwarfs with Z > 0 (in the North Galactic hemisphere) have 〈Vz〉 < 0, while the reverse is true for white dwarfs with Z < 0. The age-velocity dispersion relation derived from the present sample indicates that the Galactic population of white dwarfs may have experienced an additional source of heating, which adds to the secular evolution of the Galactic disc.
Momelotinib therapy for myelofibrosis: a 7-year follow-up
Authors: Tefferi Ayalew , Barraco Daniela , Lasho Terra L. , Shah Sahrish , Begna Kebede H. , Al-Kali Aref , Hogan William J. , Litzow Mark R. , Hanson Curtis A. , Ketterling Rhett P. , Gangat Naseema , Pardanani Animesh 
Published: March 2018

AbstractOne-hundred Mayo Clinic patients with high/intermediate-risk myelofibrosis (MF) received momelotinib (MMB; JAK1/2 inhibitor) between 2009 and 2010, as part of a phase 1/2 trial (NCT00935987); 73% harbored JAK2 mutations, 16% CALR, 7% MPL, 44% ASXL1, and 18% SRSF2. As of July 2017, MMB was discontinued in 91% of the patients, after a median treatment duration of 1.4 years. Grade 3/4 toxicity included thrombocytopenia (34%) and liver/pancreatic test abnormalities (<10%); grade 1/2 peripheral neuropathy occurred in 47%. Clinical improvement (CI) occurred in 57% of patients, including 44% anemia and 43% spleen response. CI was more likely to occur in ASXL1-unmutated patients (66% vs 44%) and in those with <2% circulating blasts (66% vs 42%). Response was more durable in the presence of CALR type 1/like and absence of very high-risk karyotype. In multivariable analysis, absence of CALR type 1/like (HR 3.0; 95% CI 1.2–7.6) and presence of ASXL1 (HR 1.9; 95% CI 1.1–3.2) or SRSF2 (HR 2.4, 95% CI 1.3–4.5) mutations adversely affected survival. SRSF2 mutations (HR 4.7, 95% CI 1.3–16.9), very high-risk karyotype (HR 7.9, 95% CI 1.9–32.1), and circulating blasts ≥2% (HR 3.9, 95% CI 1.4–11.0) predicted leukemic transformation. Post-MMB survival (median 3.2 years) was not significantly different than that of a risk-matched MF cohort not receiving MMB.