bluuebunny/crossref_metadata_2025_split huggingface dataset:
Dietary behaviours in the context of nutrition transition: a systematic review and meta-analyses in two African countries
Authors: Rousham Emily K , Pradeilles Rebecca , Akparibo Robert , Aryeetey Richmond , Bash Kristin , Booth Andrew , Muthuri Stella K , Osei-Kwasi Hibbah , Marr Colette M , Norris Tom , Holdsworth Michelle 
Published: March 2020

AbstractObjective:To synthesise evidence of urban dietary behaviours (macronutrients, types of foods, dietary diversity and dietary practices) in two African countries in relation to postulated changes in the context of nutrition transition.Design:Systematic review and meta-analyses, including six online databases and grey literature, 1971–2018 (Protocol CRD42017067718).Setting:Urban Ghana and Kenya.Participants:Population-based studies of healthy adolescents and adults.Results:The forty-seven included studies encompassed 20 726 individuals plus 6526 households. Macronutrients were within WHO-recommended ranges: mean energy intake was 1867 kcal/d (95 % CI 1764, 1969) and the proportions of macronutrients were carbohydrate 61·2 % (58·4, 64·0), fat 25·3 % (22·8, 28·0) and protein 13·7 % (12·3, 15·1). The proportion of population consuming fruit and vegetables was 51·6 %; unhealthy foods, 29·4 %; and sugar-sweetened beverages (SSBs), 39·9 %. Two-thirds (68·8 %) consumed animal-source proteins. Dietary diversity scores were within the mid-range. Meal patterns were structured (typically three meals per day), with evidence lacking on snacking or eating out.Conclusions:Population-level diets fell within WHO macronutrient recommendations, were relatively diverse with structured meal patterns, but some indications of nutrition transition were apparent. The proportion of population consuming fruit and vegetables was low compared to healthy-eating recommendations, and consumption of SSBs was widespread. A paucity of evidence from 1971 to 2010 precluded a longitudinal analysis of nutrition transition. Evidence from these two countries indicates which aspects of dietary behaviours may be contributing to increasing overweight/obesity, namely a low proportion of population consuming fruit and vegetables and widespread consumption of SSBs. These are potential targets for promoting healthier diets.
Homemade infant formula recipes may contain harmful ingredients: a quantitative content analysis of blogs
Authors: Davis Sutton A , Knol Linda L , Crowe-White Kristi M , Turner Lori W , McKinley Erin 
Published: March 2020

AbstractObjective:When breast-feeding is not possible, commercially made human milk substitute is recommended. Some consumers would prefer to make their own homemade infant formula (HIF) and may seek information on this practice from internet sources. The purpose of the current study was to investigate the content of blogs posting HIF recipes.Design:Blog postings were identified through a comprehensive search conducted using the Google search engine and the following search terms along with the term ‘blog’: ‘Make Your Own Baby Formula’, ‘Homemade Baby Formula’, ‘Do It Yourself (DIY) Baby Formula’, ‘DIY Baby Formula’, ‘Baby Formula Recipe’ and ‘All Natural Baby Formula’. A quantitative content analysis of blogs offering recipes for HIF was completed. Blogs that met the inclusion criteria were reviewed for disclaimers, blogger’s credentials, rationale for HIF use, advertisement or sale of recipe ingredients and recipe ingredients.Setting:Worldwide Web.Results:Fifty-nine blogs, featuring one hundred forty-four recipes, met inclusion criteria. Among reviewed blogs, 33·9 % did not provide a disclaimer stating breast milk is the preferred option, 25·4 % recommended consulting a healthcare professional before using, and 76·3 % and 20·3 % either advertised or sold ingredients or recipe kits, respectively. Credentials of bloggers varied and only seven bloggers identified themselves as ‘nutritionists’. The three most frequently mentioned recipe ingredients were whole raw cow’s milk (24·3 %), raw goat’s milk (23·6 %) and liver (14·5 %).Conclusions:Clinicians should be aware of this trend, discuss source of formula with parents, advocate for appropriate infant feeding practices and monitor for side effects.
Young, old, massive: Steps to understanding globular cluster formation
Authors: Harris William E. 
Published: March 2020

AbstractOn observational grounds we now know a huge amount about the characteristics of massive star clusters in galaxies of all types, from the smallest dwarfs to the most massive giants and even into the Intracluster Medium. The old globular clusters (GCs) in particular exhibit a high degree of uniformity across all these environments in their physical properties including scale size, luminosity distribution, metallicity distribution, and age. As survivors of a long period of dynamical evolution, they are “unusual, but not special” among star clusters.The past few years have seen major advances in theoretical modelling that are starting to reveal how these massive star clusters formed in the early stages of galaxy evolution. Several suites of models point to their emergence in GMCs (Giant Molecular Clouds), which provide the turbulent big reservoirs of gas within which star clusters can be built. At cluster masses ∼105M⊙ and above, clusters form hierarchically through a nearly equal combination of direct gas accretion, and mergers with smaller clusters scattered throughout the GMC. GCs and YMCs (young massive clusters) in this high mass range should therefore be composite systems right from birth. To make such high-mass clusters, host GMCs of ∼107M⊙ are needed, and these are most commonly found in galaxies at redshifts z ≳ 2.
Using Gaia for studying Milky Way star clusters
Authors: Vasiliev Eugene 
Published: March 2020

AbstractWe review the implications of the Gaia Data Release 2 catalogue for studying the dynamics of Milky Way globular clusters, focusing on two separate topics.The first one is the analysis of the full 6-dimensional phase-space distribution of the entire population of Milky Way globular clusters: their mean proper motions (PM) can be measured with an exquisite precision (down to 0.05 mas yr−1, including systematic errors). Using these data, and a suitable ansatz for the steady-state distribution function (DF) of the cluster population, we then determine simultaneously the best-fit parameters of this DF and the total Milky Way potential. We also discuss possible correlated structures in the space of integrals of motion.The second topic addresses the internal dynamics of a few dozen of the closest and richest globular clusters, again using the Gaia PM to measure the velocity dispersion and internal rotation, with a proper treatment of spatially correlated systematic errors. Clear rotation signatures are detected in 10 clusters, and a few more show weaker signatures at a level ∼0.05 mas yr−1. PM dispersion profiles can be reliably measured down to 0.1 mas yr−1, and agree well with the line-of-sight velocity dispersion profiles from the literature.
Gaia results for star clusters and dwarf galaxies in the Milky Way
Authors: Massari Davide 
Published: March 2020

AbstractThe second data release of the Gaia mission coupled with ground-based spectroscopic observations has allowed the determination of the orbital parameters for almost all of the Galactic globular clusters, as well as for the known dwarf spheroidal galaxies orbiting the Milky Way. Moreover, it has led to the discovery of dwarf galaxies that were accreted by the Galaxy long ago and that are now completely disrupted. By exploiting their dynamics in combination with the globular clusters age-metallicity relation, we investigated the clusters-to-dwarfs connection. We found that about 60 globulars likely formed in situ, and associated those that were accreted to the dwarf galaxy progenitor they likely formed in.
Stellar-mass Black Holes in Globular Clusters: Dynamical consequences and observational signatures
Authors: Askar Abbas , Giersz Mirek , Arca Sedda Manuel , Askar Ammar , Pasquato Mario , Leveque Agostino 
Published: March 2020

AbstractSizeable number of stellar-mass black holes (BHs) in globular clusters (GCs) can strongly influence the dynamical evolution and observational properties of their host cluster. Using results from a large set of numerical simulations, we identify the key ingredients needed to sustain a sizeable population of BHs in GCs up to a Hubble time. We find that while BH natal kick prescriptions are essential in determining the initial retention fraction of BHs in GCs, the long-term survival of BHs is determined by the size, initial central density and half-mass relaxation time of the GC. Simulated GC models that contain many BHs are characterized by relatively low central surface brightness, large half-light and core radii values. We also discuss novel ways to compare simulated results with available observational data to identify GCs that are most likely to contain many BHs.
Light element discontinuities in the globular cluster NGC 6402 (M14)
Authors: Johnson Christian I. 
Published: March 2020

AbstractNGC 6402 is one of the most massive globular clusters in the Galaxy but until recently little was known about its detailed chemical composition. Interestingly, recent results have shown that NGC 6402 exhibits a paucity of intermediate composition stars that may be indicative of an early termination of star formation. As a result, NGC 6402 may be important for understanding cluster formation and the order in which various stellar populations are born.
Intermediate-Mass Black Holes in binary rich star clusters
Authors: Šubr Ladislav , Fragione Giacomo , Dabringhausen Jörg 
Published: March 2020

AbstractThree-body interactions of stellar-mass binaries with intermediate mass black holes (IMBHs) in nuclei of globular clusters may produce specific features that may serve as an independent indicator of existence of the IMBHs. By means of direct N-body integrations we follow the dynamical evolution of globular clusters of moderate extension and mass with 50% binary population over a time span of ≍ 0.8 Gyr and compare the cases with and without the primordial binaries as well as with and without the IMBH. We show that (i) presence of the IMBH leads to rapid formation of a density cusp regardless of the initial binary fraction, (ii) binary rich clusters with the IMBH produce high velocity escapers at a rate of ≍ 0.1 Myr−1 and (iii) clusters hosting an IMBH together with high number of binaries form a denser halo of marginally unbound stars than clusters that lack either the IMBH or the binary population.
Detection of White Dwarf companions to Blue Straggler Stars from UVIT observations of M67
Authors: N Sindhu , Subramaniam Annapurni , Geller Aaron M. , Jadhav Vikrant , Knigge Christian , Simunovic Mirko , Leigh Nathan , Shara Michael , Puzia Thomas H. 
Published: March 2020

AbstractWe investigate the old open cluster M67 using ultraviolet photometric data of Ultra-Violet Imaging Telescope in multi-filter far-UV bands. M67, well known for the presence of several blue straggler stars (BSS), has been put to detailed tests to understand their formation pathways. Currently, there are three accepted formation channels: mass transfer due to Roche-lobe overflow in binary systems, stellar mergers either due to dynamical collisions or through coalescence of close binaries. So far, there had not been any confirmed detection of a white dwarf (WD) companion to any of the BSSs in this cluster. Here, we present the detection of WD companions to 5 bright BSSs in M67. The multiwavelength spectral energy distributions covering 0.12 -11.5 μm range, were found to require binary spectral fits for 5 BSSs, consisting of a cool (BSS) and a hot companion. The parameters (Luminosity, Temperature, Radius and Mass) of the hot companions suggest them to be WDs with mass in the range 0.2 - 0.35 M⊙ with Teff ~11000 –24000 K.
Detection of extended Red Clump in the SMC cluster Kron 3
Authors: Nayak P. K. , Subramaniam A. , Subramanian S. , Sahu S. , Mondal C. , Cioni Maria-Rosa L. , Bell C. 
Published: March 2020

AbstractFor the first time, we report the identification of NUV bright red clump (RC) stars and the extension of RC stars over two magnitudes both in color and magnitude axis in NUV vs (NUV – optical) color magnitude diagram. We find that the extension of RC is not due to photometric uncertainties. We suggest that the extension could be an effect of field star contamination. We also suggest that if it is an intrinsic property of the cluster then age and/or metallicity spread within the cluster could be the possible reasons for extended RC.
The properties of nuclear star clusters and their host galaxies
Authors: Seth Anil C. , Neumayer Nadine , Böker Torsten 
Published: March 2020

AbstractNuclear star clusters are found at the centers of most galaxies. They are the densest stellar systems in the Universe, and thus have unique and interesting stellar dynamics. We review how common nuclear star clusters are in galaxies of different masses and types, and then discuss the typical properties of NSCs. We close by discussing the formation of NSCs, and how a picture is emerging of different formation mechanisms being dominant in lower and higher mass galaxies.
Brownian motion of supermassive black holes in galaxy cores
Authors: Di Cintio Pierfrancesco , Ciotti Luca , Nipoti Carlo 
Published: March 2020

AbstractWe investigate the dynamics of supermassive black holes (SMBHs) in galactic cores by means of a semi-analytic model based on the Langevin equation, including dynamical friction and stochastic noise accounting for the gravitational interactions with stars. The model is validated against direct N-body simulations of intermediate-mass black holes in stellar clusters where a realistic number of particles is accessible. For the galactic case, we find that the SMBH experiences a Brownian-like motion with a typical displacement from the geometric center of the Galaxy of a few parsecs, for system parameters compatible with M87.
Growth of intermediate mass black holes in first star clusters
Authors: Sakurai Yuya , Yoshida Naoki , Fujii Michiko S. 
Published: March 2020

AbstractWe study runaway stellar collisions in primordial star clusters and formation of intermediate mass black holes (IMBHs). Using cosmological simulations, we identify eight atomic-cooling halos in which the star clusters form. We follow stellar and dark matter (DM) dynamics for 3Myr using hybrid N-body simulations. We find that the runaway stellar collisions occur in all star clusters and IMBHs with masses ∼400–1900M⊙ form. Performing additional N-body simulations, we explore evolutions of the IMBHs in the star clusters for 15 Myr. The IMBH masses grow via stellar tidal disruption events (TDEs) to ∼700–2500 M⊙. The TDE rates are ∼0.3–1.3 Myr−1. DM motions affect the star cluster evolutions and reduce the TDE rates. The IMBHs may subsequently grow to SMBHs by gas supply through galaxy mergers or large-scale gas inflows, or they may remain within or around the clusters.
The Role of “black hole burning” in the evolution of dense star clusters
Authors: Kremer Kyle , Ye Claire S. , Chatterjee Sourav , Rodriguez Carl L. , Rasio Frederic A. 
Published: March 2020

AbstractAs self-gravitating systems, dense star clusters exhibit a natural diffusion of energy from their innermost to outermost regions, leading to a slow and steady contraction of the core until it ultimately collapses under gravity. However, in spite of the natural tendency toward “core collapse,” the globular clusters (GCs) in the Milky Way exhibit a well-observed bimodal distribution in core radii separating the core-collapsed and non-core-collapsed clusters. This suggests an internal energy source is at work, delaying the onset of core collapse in many clusters. Over the past decade, a large amount of work has suggested that stellar black holes (BHs) play a dynamically-significant role in clusters throughout their entire lifetimes. Here we review our latest understanding of BH populations in GCs and demonstrate that, through their dynamical interaction with their host cluster, BHs can naturally explain the distinction between core-collapsed and non-core-collapsed clusters through a process we call “black hole burning.”
Dynamically stable models for galaxies
Authors: Dabringhausen Jörg , Šubr Ladislav , Feldmeier-Krause Anja 
Published: March 2020

AbstractA popular approach to model galaxies is Schwarzschild’s method. For this method, a grid of sample orbits of stars in an external potential is calculated, and a model for the stellar system is obtained through attributing specific weights to the orbits in a superposition of them. The models created with Schwarzschild’s method can fit many observed properties of the modeled stellar system with high precision. However, systems that are stationary as Schwarzschild models may therefore exhibit a strong time evolution if they are translated into more realistic self-gravitating models. The issue is highlighted with the Galactic center as an example.
Internal kinematics of Globular Clusters: Current state of the art, issues, and what to expect from the future
Authors: Bellini Andrea 
Published: March 2020

AbstractThe advent of the Gaia mission is bringing astrometry to a new renaissance. Although Gaia will make important breakthroughs in many different scientific areas, stars in the crowded central fields of globular clusters (GCs) and at the faint end of the color-magnitude diagram are and will be out of Gaia’s reach. The Hubble Space Telescope (HST) is an excellent astrometric tool that has allowed us to distinguish and measure positions and brightness of faint stars in pencil-beam fields down to the very center of some GCs. Gaia and HST are two wonderful, complementary tools, but are yet far from being able to offer a complete dynamical picture of GCs. There is now great prefiguration for what the next-generation telescopes will be able to do, both ground- and space-based. This document highlights strengths and weaknesses of different facilities at different spatial and spectral regimes.
Interaction of stars hosting planets with Sgr A* black hole
Authors: Davari Nazanin , Capuzzo-Dolcetta Roberto , Spurzem Rainer 
Published: March 2020

AbstractWe present some preliminary results of our ongoing project about planetary systems around S-stars in the vicinity of Sgr A* black hole. Since S-stars might have migrated in the Galactic Centre (GC) from elsewhere, they probably still keep their planetary systems throughout their voyage. In this work, we study the destiny of their putative planetary systems after close interaction with the central black hole of our galaxy.
The relationship between globular cluster parameters and abundance variations
Authors: Nataf David M. 
Published: March 2020

AbstractWe discuss a meta-analysis of the association of abundance variations in globular cluster stars with the present-day stellar mass and metallicity of globular clusters. Using data for 42 globular clusters that are well-sampled from either or both of prior literature studies and the APOGEE survey, we confirm prior findings that increasing aluminum abundance variations in globular clusters are positively correlated with increasing present-day stellar mass or decreasing metallicity. We also demonstrate that the ratio of aluminum abundance variations to either nitrogen abundance variations or sodium abundance variations is itself positively correlated with decreasing metallicity and increasing stellar mass of globular clusters. This suggests that there were at least two non-supernovae chemical polluters that were active in the early universe.
Thirteen facts that you need to know on multiple populations in globular clusters
Authors: Milone Antonino P. 
Published: March 2020

AbstractI review the methods, mostly developed in the last decade, that are commonly used to identify and characterize multiple populations (MPs) in Globular Clusters (GCs) based on photometry. I summarize the results from the recent surveys of MPs with the Hubble Space Telescope (HST) and ground-based facilities and provide a list of the main properties of MPs as inferred from these studies.
Alternating direction method of multiplier for solving electromagnetic inverse scattering problems
Authors: Liu Jian , Zhou Huilin , Chen Liangbing , Ouyang Tao 
Published: March 2020

AbstractIn this paper, a novel alternating direction method of multiplier (ADMM) is proposed to solve the inverse scattering problems. The proposed method is suitable for a wide range of applications with electromagnetic detection. In order to solve the internal ill-posed problem of the integral equation and make the reconstructed images more closer to the ground truth, first, the augmented Lagrangian method is introduced to transform the complex constrained optimization problem into the extremum problem of unconstrained cost function. Therefore, two artificial regularization factors of the cost function are optimized. Then, this proposed method decomposes the unconstrained global problem in the inversion process into three linear sub-problem forms of contrast source function, contrast function, and dual variables. And the form of the updated algebra for each sub-problem is not complicated. By cross-iterating and updating contrast source function, contrast function, and dual variables, the global minimization of the cost function can be accurately found. Finally, the proposed method is compared with the existing well-known iterative method for solving the inverse scattering problem. Both the numerical and experimental tests verify the validity and accuracy of the proposed ADMM.
A flexible broadband antenna for IoT applications
Authors: Al-Sehemi Abdullah , Al-Ghamdi Ahmed , Dishovsky Nikolay , Atanasova Gabriela , Atanasov Nikolay 
Published: March 2020

AbstractA flexible broadband antenna with high radiation efficiency for the Internet of Things (IoT) applications is presented. The design is based on a U-shaped and a triangular-shaped radiator with two tuning stubs. A 50 Ω coplanar waveguide (CPW) transmission line is employed to feed the antenna. The proposed antenna is fabricated on a flexible substrate from a composite synthesized by mixing natural rubber with SiO2 as a filler. The radiating elements, along with the CPW, are built using a highly conductive woven fabric. Results show that the antenna has a simulated and measured impedance bandwidth of 0.856–2.513 GHz and covers the most commonly used wireless communication standards and technologies for IoT applications. The radiation efficiency of the antenna reaches over 75% throughout the operating frequency band with satisfactory radiation patterns and gain. The flexible antenna was also tested under bending conditions. The presented results demonstrate that bending has a minor effect on the antenna performance within the target frequency range. The measured results show a good agreement with simulations.