bluuebunny/crossref_metadata_2025_split huggingface dataset:
Tracheostomy for paediatric obstructive sleep apnoea: A systematic review
Authors: Fray S , Biello A , Kwan J , Kram Y A , Lu K , Camacho M 
Published: August 2018

AbstractObjectiveTo search the international literature (any language) for publications reporting outcomes of tracheostomy performed to treat obstructive sleep apnoea in children.MethodData sources included: Google Scholar, Cumulative Index to Nursing and Allied Health Literature, Embase, Scopus, and PubMed/Medline. Four authors searched systematically through to 20 January 2018.ResultsA total of 597 studies were screened; 64 were downloaded and 11 met criteria. A total of 196 patients underwent tracheostomy (mean age, 4.2 years; range, newborn to 18 years); 40 had detailed qualitative data and 6 had detailed quantitative data. Apnoea/hypopnoea index showed a 97 per cent reduction (n= 2) and apnoea index showed a 98 per cent reduction (n= 3). Lowest oxygen saturation showed a 34 oxygen saturation point improvement (n= 3). Several patients demonstrated significant improvement in breathing. All identified patients were syndromic, had significant co-morbidities or had severe obstructive sleep apnoea.ConclusionBased on reports of children who have undergone a tracheostomy, for whom there are pre- and post-operative data, tracheostomy appears to be a successful treatment for obstructive sleep apnoea. However, additional research is recommended given the small number of patients in the literature.
An analogue of Khintchine's theorem for self-conformal sets
Authors: BAKER SIMON 
Published: August 2018

AbstractKhintchine's theorem is a classical result from metric number theory which relates the Lebesgue measure of certain limsup sets with the convergence/divergence of naturally occurring volume sums. In this paper we ask whether an analogous result holds for iterated function systems (IFS's). We say that an IFS is approximation regular if we observe Khintchine type behaviour, i.e., if the size of certain limsup sets defined using the IFS is determined by the convergence/divergence of naturally occurring sums. We prove that an IFS is approximation regular if it consists of conformal mappings and satisfies the open set condition. The divergence condition we introduce incorporates the inhomogeneity present within the IFS. We demonstrate via an example that such an approach is essential. We also formulate an analogue of the Duffin–Schaeffer conjecture and show that it holds for a set of full Hausdorff dimension.Combining our results with the mass transference principle of Beresnevich and Velani [4], we prove a general result that implies the existence of exceptional points within the attractor of our IFS. These points are exceptional in the sense that they are “very well approximated”. As a corollary of this result, we obtain a general solution to a problem of Mahler, and prove that there are badly approximable numbers that are very well approximated by quadratic irrationals.The ideas put forward in this paper are introduced in the general setting of iterated function systems that may contain overlaps. We believe that by viewing iterated function systems from the perspective of metric number theory, one can gain a greater insight into the extent to which they overlap. The results of this paper should be interpreted as a first step in this investigation.
A code comparison of the interaction between Milky Way disc and satellites
Authors: Mazzarini Matteo , Just Andreas 
Published: August 2018

AbstractWe present a comparison of previous simulations of the interaction of the Galactic disc with the Milky Way (MW) satellites using superbox-10 with new simulations performed with gadget-2 and ChaNGa. The robust performance of gadget-2 motivates us to employ more recent versions of gadget
to identify the satellite debris in the MW halo, disc and bulge.
Is the Galactic Spiral Potential 2- or 4-arms?
Authors: Grosbøl Preben , Carraro Giovanni 
Published: August 2018

AbstractYoung objects (e.g. OB-associations and HII regions) in the Galaxy outline a 4-armed spiral structure whereas the tangent points of arms observed in the near-infrared indicate a 2-armed pattern. The more important issue is whether the spiral potential in the Galaxy is 2- or 4-armed i.e. if all arms traced by young objects also have a significant mass perturbation associated to them. This can be tested by studying the mean radial velocity of a well defined stellar population across the spiral arms and thereby estimating the surface density change.The current paper presents a preliminary analysis of the radial velocities of a sample of 736 early-type stars toward the Galactic center observed with FLAMES/VLT. A comparison with N-body models in a fixed spiral potential with 2 or 4 arms suggests that no significant mass is associated to the Sagittarius arm. The data are consistent with 2-armed models with pattern speeds in the range of 15-30 km s−1 kpc−1 and relative radial forces of less than 4%.
New Highly r-Process-Enhanced Halo Stars
Authors: Beers Timothy C. , Holmbeck Erika M. , Placco Vinicius M. , Hansen Terese T. , Simon Joshua D. , Thompson Ian , Frebel Anna , Sakari Charli M. 
Published: August 2018

AbstractThere are roughly 25 very metal-poor (VMP; [Fe/H] &lt; -2.0), highly r-process-enhanced (‘r-II’; [Eu/Fe] &gt; + 1.0) stars currently known, discovered over the past 20+ years. These stars provide nearly pure signatures of r-process events early in the Galactic history. We are conducting a high-resolution follow-up survey of RAVE and other bright targets to identify a total of &gt; 100 r-II stars. Our pilot runs on the du Pont 2.5-m at Las Campanas Observatory and the ARC 3.5-m at Apache Point Observatory have already identified up to fourteen new r-II stars. We are continuing our high-resolution follow-up efforts to constrain the astrophysical site(s) and nature of the r-process.
Kinematic structures found with Gaia DR1/TGAS and RAVE data in the Solar neighbourhood
Authors: Kushniruk I. , Schirmer T. , Bensby T. 
Published: August 2018

AbstractWith the much enlarged stellar sample of 55 831 stars and much increased precision in distances, proper motions, provided by Gaia DR1 TGAS we have shown with the help of the wavelet analysis that the velocity distribution of stars in the Solar neighbourhood contains more kinematic structures than previously known. We detect 19 kinematic structures between scales 3-16 km s−1 at the 3σ confidence level. Among them we identified well-known groups (such as Hercules, Sirius, Coma Berenices, Pleiades, and Wolf 630). We confirmed recently detected groups (such as Antoja12 and Bobylev16). In addition we report here about a new kinematic structure at (U, V) ≈ (37, 8) km s−1. Another three new groups are tentatively detected, but require confirmation.
The APOSTLE simulations: Rotation curves derived from synthetic 21-cm observations
Authors: Oman Kyle A. 
Published: August 2018

AbstractTheapostlecosmological hydrodynamical simulation suite is a collection of twelve regions ~5 Mpc in diameter, selected to resemble the Local Group of galaxies in terms of kinematics and environment, and re-simulated at high resolution (minimum gas particle mass of 104M⊙) using the galaxy formation model and calibration developed for theeagleproject. I select a sample of dwarf galaxies (60 &lt;Vmax/km s−1&lt; 120) from these simulations and construct synthetic spatially- and spectrally-resolved observations of their 21-cm emission. Using the3Dbarolotilted-ring modelling tool, I extract rotation curves from the synthetic data cubes. In many cases, non-circular motions present in the gas disc hinder the recovery of a rotation curve which accurately traces the underlying mass distribution; a large central deficit of dark matter, relative to the predictions of cold dark matter N-body simulations, may then be erroneously inferred.
The age-metallicity structure of the Milky Way disc with APOGEE
Authors: Mackereth J. Ted , Bovy Jo , Schiavon Ricardo P. ,   the SDSS-IV/APOGEE Collaboration
Published: August 2018

AbstractThe best way to trace back the history of star formation and mass assembly of the Milky Way disc is by combining chemical compositions, ages and phase-space information for a large number of disc stars. With the advent of large surveys of the stellar populations of the Galaxy, such data have become available and can be used to pose constraints on sophisticated models of galaxy formation. We use SDSS-III/APOGEE data to derive the first detailed 3D map of stellar density in the Galactic disc as a function of age, [Fe/H] and [α/Fe]. We discuss the implications of our results for the formation and evolution of the disc, presenting new constraints on the disc structural parameters, stellar radial migration and disc flaring. We also discuss how our results constrain the inside out formation of the disc, and determine the surface-mass density contributions at the solar radius for mono-age, mono-[Fe/H] populations.
New Views From Galactoseismology: Rethinking the Galactic Disk-Halo Connection
Authors: Sheffield Allyson A. , Johnston Kathryn V. , Price-Whelan Adrian M. , Tzanidakis Anastasios , Laporte Chervin F. P. , Li Ting , Bergemann Maria , Sesar Branimir , Carlin Jeffrey L. 
Published: August 2018

AbstractWe present preliminary results from a study exploring the origin of Milky Way substructures, and show initial evidence of a common “kicked-out” formation mechanism for two low-latitude substructures. In this scenario, stars in these substructures formed in the disk and were subsequently “kicked-out” by an external perturbation, such as the merger of an accreted satellite, which created an oscillation in the Galactic disk. To test this origin scenario, we found the fraction of different stellar populations – M giants and RR Lyrae stars – in the Monoceros Ring (also known as GASS) and A13, supplementing a study of stellar populations in the Triangulum-Andromeda cloud. This work provides: (1) the first analysis of the GASS and A13 features based upon their stellar populations; and (2) preliminary evidence of disk stars in the Milky Way that have been relocated to the disk-halo interface due to vertical oscillations of the Milky Way’s disk.
Open cluster study in LAMOST DR3
Authors: Zhong Jing , Chen Li , Zhang Chaoli , Shao Zhengyi , Hou Jinliang 
Published: August 2018

AbstractIn studying Galactic open clusters based on LAMOST DR3, we deliberately selected several nearby cluster, which have relatively large projection area and reliable proper motion measurements. For each cluster, we firstly determine the typical proper motion distribution profiles in the cluster-core and the outskirt region, respectively, and perform field-star decontamination on the cluster area. We then calculate kinematic membership probability for each star in the cluster area and cross-match the highly probable members with LAMOST DR3 spectral catalog. Based on enhanced signal of cluster-member radial velocity distribution emerging from the whole field, we have also obtained reliable radial velocity membership probability for each star. Finally, we perform isochrones fitting with MCMC technique to study basic properties of these cluster, including age, metallicity, and distance modulus.
Study of the thick disc of the Milky Way from a population synthesis model
Authors: Nasello G. , Robin A. C. , Reylé C. , Lagarde N. 
Published: August 2018

AbstractThe thick disc is a major component of the Milky Way but its epoch of formation and characteristics are still not yet well constrained. The Besançon Galaxy Model (BGM, Robin et al. 2003) is a population synthesis model based on a scenario of formation and evolution of the Galaxy, a star formation history, and a set of stellar evolution models. Thanks to Lagarde et al. (2017), new evolutionary tracks have been introduced into the Besancon Galaxy Model (STAREVOL, Lagarde et al. 2012) to provide global asteroseismic and surface chemical properties along the evolutionary stages. This updated Galaxy model will allow us to constrain the thick disc structure and history using the Markov Chain Monte Carlo fitting method (MCMC). We show preliminary results applying this MCMC method on the 2MASS photometric survey.
Kinematic trends in young and old stars
Authors: Wojno Jennifer , Kordopatis Georges , Steinmetz Matthias , McMillan Paul J. ,   the RAVE collaboration
Published: August 2018

AbstractUsing RAVE DR5, we explore the age, kinematic, and chemical correlations of a sample of 30,000 FGK stars. We separate a sample of turnoff stars into two age groups: young and old. For each of the two age groups, we calculate kinematic trends as a function of Galactocentric radius (R), for different metallicity ([Fe/H]) bins. For both young and old stars, we measure a negative gradient in ∂〈VR〉/∂R. In addition, for young stars we find a correlation between the magnitude of the slope and metallicity, with the most metal-rich bins having the steepest gradient and the most metal-poor bins having a flatter trend.
NLTE abundances of C, O, Ca, Ti, and Fe in the reference BAF-type stars
Authors: Sitnova Tatyana , Ryabchikova Tatyana , Alexeeva Sofya , Mashonkina Lyudmila 
Published: August 2018

AbstractWe present accurate methods of abundance determination based on the non-local thermodynamic equilibrium (NLTE) line formation for carbon, oxygen, calcium, titanium, and iron in the atmospheres of BAF-type stars. For C I-II, O I, Ca I-II, and Ti I-II, their comprehensive model atoms were described in our previous papers. A fairly complete model atom of Fe I-II is first applied in this study. We determine the NLTE abundances of the nine BAF-type stars with well-determined atmospheric parameters, using high-resolution and high signal-to-noise ratio spectral observations in the broad wavelength range, from the UV to the IR. For C, Ca, Ti, and Fe, NLTE leads to consistent abundances from the lines of the two ionisation stages. The C I, Ca II, and Fe II emission lines were detected in the near IR spectrum of the late B-type subgiant star HD 160762. They are well reproduced in the classical hydrostatic model atmosphere, when applying our NLTE methods.
Galactoseismology in the Age of Gaia
Authors: Widrow Lawrence M. , Chequers Matthew H. 
Published: August 2018

AbstractRecent observations from SEGUE, RAVE, and LAMOST have revealed tantalizing evidence that the local stellar disk of the Milky Way is in a state of disequilibrium. In particular, the disk appears to exhibit bending and breathing waves normal to its midplane within 2 kiloparsecs of our position within the disk. There also appear to be bending waves or corrugations at larger Galactocentric radii. These waves may be linked to other time-dependent disk phenomena such as the bar, spiral structure, and warp, or they may be the result of a passing dark matter subhalo or dwarf galaxy. Here, we discuss the observational evidence for these waves, the theory of bending and breathing waves in (simulated) stellar disks, and implications of disequilibrium for attempts to determine the local vertical force and dark matter density (the Oort problem). We also discuss the types of analyses that one might do with the Gaia
database.
Impacts of Radial Mixing on the Galactic Thick and Thin Disks
Authors: Kawata Daisuke 
Published: August 2018

AbstractUsing N-body simulations of the Galactic disks, we qualitatively study how the metallicity distributions of the thick and thin disk stars are modified by radial mixing induced by the bar and spiral arms. We show that radial mixing drives a positive vertical metallicity gradient in the mono-age disk population whose initial scale-height is constant and initial radial metallicity gradient is tight and negative. On the other hand, if the initial disk is flaring, with scale-height increasing with galactocentric radius, radial mixing leads to a negative vertical metallicity gradient, which is consistent with the current observed trend. We also discuss impacts of radial mixing on the metallicity distribution of the thick disk stars. By matching the metallicity distribution of N-body models to the SDSS/APOGEE data, we argue that the progenitor of the Milky Way’s thick disk should not have a steep negative metallicity gradient.
PARSEC evolutionary tracks and isochrones including seismic properties
Authors: Montalbán J. , Bressan A. , Girardi L. , Rodrigues T. , Bossini D. , Miglio A. , Scuflaire R. , Trabucchi M. , Marigo P. 
Published: August 2018

AbstractIn the recent years it has been generally accepted that seismic parameters add an important observational constraint for the study of stellar populations and galaxy evolution. Padova-Trieste (PARSEC) evolutionary tracks are widely used to characterise stellar objects and stellar populations. Stellar models at the base of these studies suffer from uncertainties and, more important, degeneracy among different input parameters: stellar mass, chemical composition, central chemical mixing, age, etc. Adding seismic properties to the classic parameters for stars at different evolutionary states, from the H main-sequence to the asymptotic giant branch, is a powerful tool to calibrate physical processes in stellar models, and hence to improve our interpretation of Galactic and extra-Galactic observations.
High-precision abundances of elements in stars with asteroseismic ages
Authors: Nissen P. E. , Aguirre V. Silva , Christensen-Dalsgaard J. , Collet R. , Grundahl F. , Slumstrup D. 
Published: August 2018

AbstractHigh-precision abundances of elements have been derived from HARPS-N spectra of F and G main-sequence stars having ages determined from oscillation frequencies delivered by the Kepler mission. The tight relations between abundance ratios of refractory elements, e.g., [Mg/Fe] and [Y/Mg], and stellar age previously found for solar twin stars are confirmed. These relations provide new information on nucleosynthesis and Galactic evolution. Abundance ratios between volatile and refractory elements, e.g., [C/Fe] and [O/Fe], show on the other hand a significant scatter at a given age, which may be related to planet-star interactions. This is a potential problem for chemical tagging studies.
Stellar multiplicity in the Milky Way Galaxy
Authors: Stonkutė E. , Church R. P. , Feltzing S. , Johnson J. A. 
Published: August 2018

AbstractWe present our models of the effect of binaries on high-resolution spectroscopic surveys. We want to determine how many binary stars will be observed, whether unresolved binaries will contaminate measurements of chemical abundances, and how we can use spectroscopic surveys to better constrain the population of binary stars in the Galaxy. Using a rapid binary-evolution algorithm that enables modelling of the most complex binary systems we generate a series of large binary populations in the Galactic disc and evaluate the results. As a first application we use our model to study the binary fraction in APOGEE giants. We find tentative evidence for a change in binary fraction with metallicity.
Using open clusters as tracers of the galactic disk history
Authors: Santrich Orlando J. Katime , Rossi Silvia , Abuchaim Yuri , Gonçalves Geraldo 
Published: August 2018

AbstractOpen clusters are important objects to study the galactic structure and its dynamical behavior as well as the stellar formation and evolution. We carried out a spectroscopic analysis to derive atmospheric parameters and chemical composition for 52 giant stars within 9 galactic open clusters. We have used the high-resolution spectra from FEROS, HARPS and UVES in the ESO archive. The methodology used is based on LTE-hypothesis. Abundances of C, N, O, Na, Mg, Al, Si, Ca, Ti, Cr, Ni, YII, LaII, CeII, and NdII were calculated. Although most of these clusters present spectroscopic analysis in the literature, some CNO and s-process abundances were not previously estimated or were calculated with high uncertainties. Several lines of such elements were identified and used to calculate new abundances and improve some previous one.
Chemical and dynamical analysis of Open Clusters from OCCASO data. The case of NGC 6705
Authors: Casamiquela Laia , Carrera Ricardo , Balaguer-Núñez Lola , Jordi Carme , Chiappini Cristina , Antoja Teresa , Miret-Roig Núria 
Published: August 2018

AbstractThe OCCASO survey targets intermediate-age and old OCs visible from the Northern hemisphere. OCCASO provides homogeneous radial velocities, atmospheric parameters, and individual abundances from high-resolution spectroscopy (R&gt;65,000) of Red Clump stars. We present a first insight into the homogeneously analyzed chemical abundances obtained fror 18 Northern OCs from OCCASO data. Our sample includes an interesting inner disk OC, NGC 6705, analyzed in the literature with inconclusive results about its α abundances. From OCCASO data this is an α-enhanced OC from the analysis of Si, Ca, Ti, Mg and O, despite its young age.
Reconstructing the star formation history of the Solar neighbourhood with Gaia
Authors: Bernard Edouard J. 
Published: August 2018

AbstractTaking advantage of the Gaia DR1, we combined TGAS parallaxes with the Tycho-2 and APASS photometry to calculate the star formation history (SFH) of the solar neighbourhood within 250 pc using the colour-magnitude diagram fitting technique. Our dynamically-evolved SFH is in excellent agreement with that calculated from the Hipparcos catalogue within 80 pc of the Sun, showing an enhanced star formation rate (SFR) in the past ~4 Gyr. We then correct the SFR for the disc thickening with age to obtain a SFR that is representative of the whole solar cylinder, and show that even with an extreme correction our results are not consistent with an exponentially decreasing SFR as found by recent studies. Finally, we discuss how this technique can be applied out to ~5 kpc thanks to the next Gaia data releases, which will allow us to quantify the SFH of the thin disc, thick disc and halo in situ.
HSC Wide and Deep Imaging Survey for the Milky Way Satellite Galaxies
Authors: Komiyama Yutaka 
Published: August 2018

AbstractWe have carried out an imaging survey for Local Group dwarf spheroidal galaxy Ursa Minor (UMi) using Hyper Suprime-Cam (HSC) on the 8.2m Subaru Telescope. Wide and deep data obtained by HSC enable us to investigate the extent of UMi which is revealed to extend out to twice the nominal tidal radius. The fraction of binary systems is also investigated from the morphology of the main sequence and estimated to be ~0.4.
Detect the density profile with LAMOST K giants
Authors: Xu Yan , Liu Chao 
Published: August 2018

AbstractThe density distribution of the Milky Way halo is detected with 5351 LAMOST DR3 metal poor K giants using a nonparametric method. The nonparametric fitting method is a model independent way to estimate the halo density distribution while to a large extent avoiding the influence of the halo substucture. We show that the K giants density profile can be fitted well by single power law. We found no indication of a break in the power law index. The powerlaw index n = 5.0−0.64+0.64. The data show that the stellar halo is flattened at smaller radii, and becomes more spherical farther from the Galactic center. The flattening q(r=15Kpc)is about0.64, q(20Kpc) is about 0.8, q(30Kpc) is about 0.96.