bluuebunny/crossref_metadata_2025_split huggingface dataset:
A longitudinal analysis of maternal depressive symptoms and children's food consumption and weight outcomes
Authors: Morrissey Taryn W , Dagher Rada K 
Published: January 2014

AbstractObjectiveMaternal depressive symptoms negatively impact mothers’ parenting practices and children's development, but the evidence linking these symptoms to children's obesity is mixed.DesignWe use a large sample to examine contemporaneous and lagged associations between maternal depressive symptoms and children's BMI, obesity and food consumption, controlling for background characteristics.SettingData from the Early Childhood Longitudinal Study-Birth Cohort (ECLS-B), a longitudinal study of children from infancy through kindergarten in the USA, were collected at four waves from 2001 to 2007, when children were 9 months, 2 years, 4 years and 5½years of age, through surveys, child assessments and observations.SubjectsA sub-sample of children from the ECLS-B is used (n6500).ResultsBetween 17 % and 19 % of mothers reported experiencing depressive symptoms; 17 % to 20 % of children were obese. Maternal depressive symptoms were associated with a small decrease in the likelihood her child was obese (0·8 percentage points) and with lower consumption of healthy foods. The duration of maternal depressive symptoms was associated with higher BMI (0·02sd) among children whose parents lacked college degrees.ConclusionsResults indicate that mothers’ depressive symptoms have small associations with children's food consumption and obesity. Among children whose parents lack college degrees, persistent maternal depressive symptoms are associated with slightly higher child BMI. Findings highlight the need to control for depression in analyses of children's weight. Interventions that consider maternal depression early may be useful in promoting healthy weight outcomes and eating habits among children.
Nineteenth-Century Gagaku Songs as a Subject of Musical Analysis: An Early Example of Musical Creativity in Modern Japan
Authors: Gottschewski Hermann 
Published: January 2014

Nineteenth-century gagaku (Japanese traditional court music) songs, composed mainly between 1877 and 1884, are almost forgotten today; but they deserve special attention for their function in the development of modern composition in Japan. More than 100 compositions by 28 composers, belonging to two collections, can be counted as gagaku songs in the narrowest sense. Most of them are accompanied by an individually composed ostinato pattern played on the wagon, a six-stringed zither. The songs are strongly shaped by Restoration thought, one of the characteristic aspects of the early modernization period in Japan, although the genre originated in response to the need for music for a modern Western method of education.An analysis of the two collections, of intertextually related pieces and of different versions of single songs shows that the collective process of genre development and the individual process of song composition were closely intertwined. The aim of my analysis was to uncover the problems faced by composers when they composed a single song. Particular solutions were often required to fulfil all the demands of the strict stylistic framework of the genre, while meeting the conditions of a specific poem. While similarity to an already existing song was not avoided when a new song was composed, the effort to create a difference can also be observed clearly in some cases. My analysis gives special attention to heterophonic techniques that characterize the relation between voice and accompaniment. Their use is constitutive for the musical form, and their analysis sheds light on the aesthetic significance of each song. An analytical approach to the gagaku song repertoire provides us with a fascinating insight into how musical creativity was performed under the circumstances of a quickly changing cultural environment in the early modernization period of Japan.
The Milky Way thin disk structure as revealed by stars and young open clusters
Authors: Carraro Giovanni 
Published: January 2014

AbstractIn this contribution I shall focus on the structure of the Galactic thin disk. The evolution of the thin disk and its chemical properties have been discussed in detail by T. Bensby's contribution in conjunction with the properties of the Galactic thick disk, and by L.Olivia in conjunction with the properties of the Galactic bulge. I will review and discuss the status of our understanding of three major topics, which have been the subject of intense research nowadays, after long years of silence: (1) the spiral structure of the Milky Way, (2) the size of the Galactic disk, and (3) the nature of the Local arm (Orion spur), where the Sun is immersed. The provisional conclusions of this discussion are that: (1) we still have quite a poor knowledge of the Milky Way spiral structure, and the main disagreements among various tracers are still to be settled; (2) the Galactic disk does clearly not have an obvious luminous cut-off at about 14 kpc from the Galactic center, and next generation Galactic models need to be updated in this respect, and (3) the Local arm is most probably an inter-arm structure, similar to what we see in several external spirals, like M 74. Finally, the impact of Gaia and LAMOST in this field will be briefly discussed as well.
Variable Stars and Galactic Structure
Authors: Feast Michael , Whitelock Patricia A. 
Published: January 2014

AbstractVariable stars have a unique part to play in Galactic astronomy. Among the most important of these variables are the Cepheids (types I and II), the RR Lyraes and the Miras (O- and C-rich). The current status of the basic calibration of these stars in their roles as distance, structure and population indicators is outlined and some examples of recent applications of these stars to Galactic and extragalactic problems are reviewed. The expected impact of Gaia on this type of work is discussed and the need for complementary ground based observations, particularly large scale near-infrared photometry, is stressed.
Peculiar Metal Poor Stars as Guides to Key Processes in the Early Halo
Authors: Andersen Johannes , Nordström Birgitta 
Published: January 2014

AbstractLarge photometric or spectroscopic surveys are used to sort stars into populations and define the main trends that characterise them, as diagnostics of their origin. Stars falling off the trends defined by the ‘normal’ stars are called ‘peculiar’ and typically eliminated in discussions of Galactic structure and evolution. In our programme on extremely metal-poor halo giants, we have recently focused on the small subgroup that is strongly enhanced in r-process elements, asking whether the chemical peculiarity is intrinsic to these stars or due to local surface pollution caused by mass transfer from a binary companion. Precise radial-velocity monitoring over several years turns out to disprove the binary hypothesis and has led to new insight in the processes of chemical enrichment in the early Galactic halo. An ongoing analogous programme on carbon-enhanced metal-poor giants is briefly described at the end.
The evolution of C and O abundances in stellar populations
Authors: Nissen Poul E. , Schuster William J. 
Published: January 2014

AbstractCarbon and oxygen abundances in F and G main-sequence stars ranging in metallicity from [Fe/H] = −1.6 to +0.5 are determined from a non-LTE analysis of C i and O i atomic lines in high-resolution spectra. Both C and O are good tracers of stellar populations; distinct trends of [C/Fe] and [O/Fe] as a function of [Fe/H] are found for high- and low-alpha halo stars and for thick- and thin-disk stars. These trends and that of [C/O] provide new information on the nucleosynthesis sites of carbon and the time-scale for the chemical enrichment of the various Galactic components.
Two distinct halo populations in the solar neighborhood: evidence from stellar abundance of beryllium
Authors: Tan Kefeng , Zhao Gang 
Published: January 2014

AbstractIt is now generally believed that the Galaxy was formed through hierarchical merging, which means that different components of the Galaxy may have experienced different chemical evolution histories. Since alpha elements are mainly produced by core collapse supernovae, they are closely associated with the star formation history of the Galaxy. In this regard, Galactic components with different alpha elemental abundance patterns may show different behaviors in beryllium abundances since the production of beryllium is correlated with the cosmic rays and thus the supernovae. A recent study by Nissen & Schuster (2010) has revealed the existence of two distinct halo populations in the solar neighborhood based on the alpha elemental abundances and kinematics of 94 dwarf stars. We determined beryllium abundances for some of these stars and find systematic differences in beryllium abundances between these two halo populations. Our results consolidate the conclusion of two distinct halo populations in the solar neighborhood. Our results also show that beryllium abundance is a very good indicator of star formation rate, and could be used to trace the substructures of the Galactic halo.
Star formation in galaxies: the role of spiral arms
Authors: Dobbs Clare L. 
Published: January 2014

AbstractStudying star formation in spiral arms tells us not only about the evolution of star formation, and molecular clouds, but can also tell us about the nature of spiral structure in galaxies. I will address both these topics using the results of recent simulations and observations. Galactic scale simulations are beginning to examine in detail the evolution of Giant Molecular Clouds (GMC) as they form in spiral arms, and then disperse by stellar feedback or shear. The overall timescale for this process appears comparable to the crossing time of the GMCs, a few Myrs for 105 M⊙ clouds, 20 Myr or so for more massive GMCs. Both simulations and observations show that the massive clouds are found in the spiral arms, likely as a result of cloud-cloud collisions. Simulations including stars should also tell us about the stellar age distribution in GMCs, and across spiral arms. More generally, recent work on spiral galaxies suggests that the dynamics of gas flows in spiral arms are different in longlived and transient spiral arms, resulting in different age patterns in the stars. Such results could be used to help establish the main driver of spiral structure in the Milky Way (Toomre instabilities, the bar, or nearby companion galaxies) in conjunction with future surveys.
The GALAH survey
Authors: Anguiano B. , Freeman K. , Bland-Hawthorn J. , De Silva G. , Asplund M. , Carollo D. , D'Orazi V. , Keller S. , Martell S. , Sharma S. , Sneden C. , de Boer L. Wylie , Zucker D. , Zwitter T. ,   the GALAH survey team
Published: January 2014

AbstractHERMES is a new high-resolution multi-object spectrograph on the Anglo Australian Telescope. The primary science driver for HERMES is the GALAH survey, GALactic Archaeology with HERMES. We are planning a spectroscopic survey of about a million stars, aimed at using chemical tagging techniques to reconstruct the star-forming aggregates that built up the disk, the bulge and halo of the Galaxy. This project will benefit greatly from the stellar distances and transverse motions from the Gaia mission.
Fundamental stellar properties from asteroseismology
Authors: Aguirre Víctor Silva , Casagrande Luca , Miglio Andrea 
Published: January 2014

AbstractAccurate characterization of stellar populations is of prime importance to correctly understand the formation and evolution process of our Galaxy. The field of asteroseismology has been particularly successful in such an endeavor providing fundamental parameters for large samples of stars in different evolutionary phases. We present our results on determinations of masses, radii, and distances of stars in the CoRoT and Kepler fields, showing that we can map and date different regions of the galactic disk and distinguish gradients in the distribution of stellar properties at different heights. We further review how asteroseismic determinations can produce a unique set of constraints, including ages, outside the solar neighborhood for galactic chemical evolution models.
Stellar population analysis of galaxies in SDSS and LAMOST Pilot Survey
Authors: Chen Xiaoyan , Luo Ali , Yang Haifeng 
Published: January 2014

AbstractThe Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST, i.e. Guoshoujing Telescope) has finished its pilot survey (from October 2011 to June 2012). With about 3000 galaxy spectra collected during the pilot survey, we are planning to analyze the stellar populations of these galaxies in two different ways respectively. One is Lick indices (such as Hβ, Mgb, 〈Fe〉 etc., Worthey et al. 1994), which are not sensitive to the flux calibration, and another one is the full optical spectra fitting (Chen et al. 2009, 2010). Then we can evaluate the affects of flux calibration errors on stellar population analysis by comparing the results of the two methods′. Here we briefly show the early experiments aiming to test the consistency and/or difference between the two methods.
The Light Side and The Dark Side of the Milky Way Halo
Authors: Kafle Prajwal R. , Sharma Sanjib , Lewis Geraint F. , Bland-Hawthorn Joss 
Published: January 2014

AbstractWe present our recent measurement of the kinematics of the Milky Way stellar halo (Light Side) and the derived mass of the dark matter halo (Dark Side) using the Jeans analysis. A tangential dip in the velocity anisotropy profile at r ~ 17 kpc (Kafle et al. 2012), and a distinct difference of ~65 kms−1 in the mean azimuthal velocity and the r.m.s dispersion of the most metal-rich and the metal-poor Blue Horizontal Branch stars we find (Kafle et al. 2013) are reported. The implications of this on the current controversial issue of an existence of the two-components in the halo are also discussed.Aided with the kinematic measurements of the light side, we demonstrate how we infer the dynamical property of the dark side. Considering a realistic three component galaxy model (Hernquist bulge, Miyamoto-Nagai disk and NFW halo), we estimate the virial mass of the Galaxy to be Mvir = 1.2+0.5−0.4 × 1012M⊙ (Kafle et al. 2012). We also show that the rotation curve of the Galaxy has undulations similar to what have also been seen in the studies of the HI gas (Sofue et al. 2009).
Offsetting the bright sources for LAMOST
Authors: Lei Ya-Juan , Zhang Hao-Tong , Dong Yi-Qiao , Yuan Hai-Long 
Published: January 2014

AbstractFor optical fiber spectrum of LAMOST, the requirement for magnitude difference between neighbor fibers is less than 5 magnitudes to avoid faint sources being contaminated by their bright neighbors. However, sometime, neither bright nor faint sources are dense enough to fill a whole plate (4000 fibers). To make full use of all the fibers, they have better be put into the same plate. To resolve crosstalk, we propose that photons fed into a fiber can be degraded by offsetting the fiber from disc center of the bright star. Thus the bright and faint sources can be observed in the same plate without crosstalk contamination. We test the feasibility of the program with the test observation of LAMOST, and the results show that our program is consistent with the expectation.
The Galactic rotation curve from red clump stars
Authors: Liu Chao , van de Ven Glenn , Fang Min , Wu Yue , Carrell Kenneth , Xue Xiangxiang 
Published: January 2014

AbstractWe use line-of-sight velocities of more than 4000 red clump stars observed from MMT/Hectospec to derive the Galactic rotation curve between 8 and 13 kpc in Galactocentric radius to better than 10 km s−1. A three-component (bulge+disk+halo) with an additional massive ring of 1.66×1010 M⊙ at about 11.6 kpc provides an excellent fit with the observation.
Data reduction and calibration for LAMOST survey
Authors: Luo Ali , Zhang Jiannan , Chen Jianjun , Song Yihan , Wu Yue , Bai Zhongrui , Wang Fengfei , Du Bing , Zhang Haotong 
Published: January 2014

AbstractThere are three data pipelines for LAMOST survey. The raw data is reduced to one dimension spectra by the data reduction pipeline(2D pipeline), the extracted spectra are classified and measured by the spectral analysis pipeline(1D pipeline), while stellar parameters are measured by LASP pipeline.(a) The data reduction pipeline. The main tasks of the data reduction pipeline include bias calibration, flat field, spectra extraction, sky subtraction, wavelength calibration, exposure merging and wavelength band connection.(b) The spectra analysis pipeline. This pipeline is designed to classify and identify objects from the extracted spectra and to measure their redshift (or radial velocity). The PCAZ (Glazebrooket al. 1998) method is applied to do the classification and redshift measurement.(c) Stellar parameters LASP. Stellar parameters pipeline (LASP) is to estimate stellar atmospheric parameters, e.g. effective temperature Teff, surface gravity log g, and metallicity [Fe/H], for F, G and K type stars. To effectively determine those fundamental stellar measurements, three steps with different methods are employed. The first step utilizes the line indices to approximately define the effective temperature range of the analyzed star. Secondly, a set of the initial approximate values of the three parameters are given based on template fitting method. Finally, we exploit ULySS (Kolevaet al. 2009) to give the final values of parameters through minimizing the χ2value between the observed spectrum and a multidimensional grid of model spectra which is generated by an interpolating of ELODIE library. There are two other classification for A type star and M type star. For A type star, standard MK system is employed (Grayet al. 2009) to give each object temperature class and luminosity type. For M type star, they are classified into subclasses by an improved Hammer method, and metallicity of each objects is also given.During the pilot survey, algorithms were improved and the pipelines were tested. The products of LAMOST survey will include extracted and calibrated spectra in FITS format, a catalog of FGK stars with stellar parameters, a catalog of M dwarf with subclass and metallicity, and a catalog of A type star with MK classification. A part of the pilot survey data, including about 319 000 high quality spectra with SNR > 10, a catalog of stellar parameters of FGK stars and another catalog of a subclass of M type stars have been released to the public in August 2012 (Luoet al. 2012). The general survey started from October 2012, and completed the first year survey. The formal data release one (DR1) is being prepared, which will include both pilot survey and first year general survey, and planed to be released under the LAMOST data policy.
Traces of the formation history of the Milky Way
Authors: Nordström B. , Stonkutė E. , Ženovienė R. , Tautvaišienė G. 
Published: January 2014

AbstractChemical and kinematical information is needed in order to understand and trace the formation history of our Galaxy. In the homogeneous large sample of F and G stars in the survey by Nordström et al. (2004), groups of stars with orbital parameters different from field stars were found by Helmi et al. (2006). Simulations of disrupted satellites showed that the groups had similar properties as infalling dwarf satellites would have after several Gyr. From high resolution spectra, we analyse elemental abundances of stars in 3 such groups with conserved kinematic properties. Here we present first results of s- and r- process element abundances in two such groups and compare with average field stars.
Comparison of Determined Stellar Parameters between LAMOST and SEGUE Spectra
Authors: Wu Yue , Luo Ali , Du Bing , Guo Yanxin 
Published: January 2014

AbstractWe positionally cross-matched the stellar observations between LAMOST pilot survey and SDSS/SEGUE database, picked out more than 4000 targets observed by both projects, mostly are late A and FGK type stars. For the two dataset, we adopted ULySS program (Koleva et al. 2009, Wu et al. 2011a) to determine the stellar atmospheric parameters (Teff, log g, [Fe/H], Radial Velocity) with the ELODIE library as a reference (Wu et al. 2011b). For the individual parameter, we made two kinds of comparison, first for the SDSS spectra, second for the LAMOST spectra, tested the differences between the SSPP (SDSS/SEGUE stellar parameter pipeline) measurements and the ULySS derived results. Since the LAMOST pilot survey observations SNR (Signal to Noise Ratio) are low, for the latter comparison we excluded those stars with g band SNR < 10, then the sample volumn reduced to around 1300. Fig.1 displays the details of the second kind comparison for each parameter. All the comparisons demonstrate acceptable and reasonable agreement between each other for medium-resolution survey spectra. Our preliminary examination on the precision of the stellar parameters that could be derived from the LAMOST pilot survey observations exhibits the equivalent capability of LAMOST to study our Milky Way as for the SDSS/SEGUE. The LAMOST telescope executed its formal survey from Sep. 28th 2012, it will yield more better quality stellar spectroscopic data spanning in deeper and broader sky coverage (this work was supported by the Natural Science Foundation of China under No. 11103031).
Development of target allocation methods for LAMOST focal plate
Authors: Yuan Hailong , Zhang Haotong , Zhang Yanxia , Lei Yajuan , Dong Yiqiao 
Published: January 2014

AbstractWe first introduce the primary target allocation requirements and restrictions for the parallel control multiple fiber system, which is used in the LAMOST spectroscopic survey. The fiber positioner anti-collision model is imported. Then several target allocation methods and features are discussed in detail, including a network flow algorithm, high priority for fiber unit holding less target number, target allocation algorithm for groups, target allocation method for add-ons and target reallocation. Their virtues and weaknesses are analyzed for various kinds of scientific research situations. Furthermore an optimization concept using the Simulate Anneal Arithmetic (SAA) is developed to improve the fiber utilizing efficiency.
Detecting and Characterizing Exoplanets with Direct Imaging: Past, Present, and Future
Authors: Biller Beth 
Published: January 2014

AbstractThe last decade has yielded the first images of exoplanets, considerably advancing our understanding of the properties of young giant planets. In this talk I will discuss current results from ongoing direct imaging efforts as well as future prospects for detection and characterization of exoplanets via high contrast imaging. Direct detection, and direct spectroscopy in particular, have great potential for advancing our understanding of extrasolar planets. In combination with other methods of planet detection, direct imaging and spectroscopy will allow us to eventually: 1) study the physical properties of exoplanets (colors, temperatures, etc.) in depth and 2) fully map out the architecture of typical planetary systems. Direct imaging has offered us the first glimpse into the atmospheric properties of young high-mass (3-10 MJup) exoplanets. Deep direct imaging surveys for exoplanets have also yielded the strongest constraints to date on the statistical properties of wide giant exoplanets. A number of extremely high contrast exoplanet imaging instruments have recently come online or will come online within the next year (including Project 1640, SCExAO, SPHERE, GPI, among others). I will discuss future prospects with these instruments.