bluuebunny/crossref_metadata_2025_split huggingface dataset:
Use of encapsulated L-lysine-HCl and DL-methionine improves postprandial amino acid balance in laying hens
Authors: Sun Mingfa , Zhao Jingpeng , Wang Xiaojuan , Jiao Hongchao , Lin Hai 
Published: September 2020

Abstract
The supplementation of dietary limiting amino acids (AA) with crystalline AA makes the use of low-protein diets an option in poultry production. The differing absorption rates of crystalline and protein-bound AA may lead to temporally imbalanced AA in the postabsorptive period. In this study, two experiments were conducted to evaluate the effect of encapsulated L-lysine-HCl (L-Lys-HCl) and DL-methionine (DL-Met) on the laying performance of hens. In exp. 1, a total of 135 forty-seven-wk-old Hy-Line Brown hens were subjected to three dietary treatments for 8 wk: basal diet supplemented with 0.14% L-Lys-HCl and 0.17% DL-Met to satisfy the NRC (1994) total Lys and Met recommendation (control) and basal diet supplemented with encapsulated L-Lys-HCl and DL-Met at the levels of 60% (60CLM, 0.084% L-Lys-HCl and 0.102% DL-Met) or 80% of control (80CLM, 0.112% L-Lys-HCl and 0.136% DL-Met), respectively. In exp. 2, 24 fifty-five-wk-old Hy-Line Brown hens were individually reared in cages and subjected to the same treatments as in exp. 1. The plasma concentrations of free AA and nitrogen metabolites were measured 2, 4, and 6 h after fed. The results showed that dietary AA treatment had no significant influence on body weight (BW), feed intake, laying rate, egg weight, egg mass, or feed efficiency. The expression levels of AA transporters CAT-1, y+LAT1, b0,+AT, B0AT, rBAT, EAAT3, and PepT1 in the duodenum, jejunum, and ileum were not influenced (P &gt; 0.05) by dietary treatment. There was an interaction of dietary AA treatment and time (P &lt; 0.05) and the 80CLM hens exhibited higher concentrations of Lys (P &lt; 0.05) than the controls at 2-h time point. In contrast, plasma Met concentration was not influenced (P &gt; 0.05), while Cys was reduced in the 60CLM hens at every time point. The 80CLM hens had higher taurine concentrations than those receiving the control diet at every postprandial time point. In conclusion, these findings demonstrate that by using encapsulated form, the supplemental levels of synthetic L-Lys-HCl and DL-Met can be effectively reduced by approximately 20% with no negative effect on laying performance. The result suggests that encapsulated Lys and Met may ameliorate the postabsorptive AA balance and contribute to the reduced dietary AA supplemental levels.
Spontaneous migration of a bullet in the cerebrum
Authors: Sezer Can , Gokten Murat , Gezgin İnan , Sezer Aykut , Binboga Ali Burak , Onay Mehmet 
Published: September 2020

Abstract
Herein, we report the case of a 32-year-old man who experienced spontaneous migration of a bullet within the brain following a gunshot injury. Emergent computed tomography revealed the bullet located in the posterosuperior side of mesencephalon. During follow-up after 10 days, the neurological status of the patient had worsened. Computed tomography revealed that the bullet had migrated posteriorly and lodged in the occipital lobe. Although a few studies have reported on the spontaneous migration of a bullet within the brain, the present case is unique as the patient examination changed with migration. We recommend serial imaging and surgery in cases of bullet migration in the brain.
Digitalization of security in the energy sector: evolution of EU law and policy
Authors: Rajavuori Mikko , Huhta Kaisa 
Published: September 2020

Abstract
This article analyses the dynamics and implications of the digitalization of security in the energy sector. Based on an evolutionary review of legal and policy instruments, we map the pace and internal dynamics of the digitalization of security in the European Union over the past 15 years. Our analysis reveals substantial changes in the conceptions and dynamics of security in the energy sector. First, we find that digitalization has only recently penetrated into the core of the energy sector’s security paradigm. Secondly, we uncover a significant disconnect in the conceptualization of the risk as against the opportunities associated with digitalization. Thirdly, we identify the growing influence of cross-sectoral instruments in the energy sector. Fourthly, we find that energy security does not feature in the overarching security discourse relating to the use of data-driven technologies in the energy sector. The findings illustrate the difficulties that managers, policymakers and researchers face when trying to keep up with the rapid technological change in the energy transition and the ensuing evolution of the energy sector’s security paradigm.
Judaism and Temporary Community: Moses Mendelssohn on imperfection and truth
Authors: Atlas Dustin N. 
Published: September 2020

Abstract
Moses Mendelssohn’s work on imperfection might cause us to rethink the concepts of truth which follow from the Kantian tradition; he offers an alternative, if repressed, way of thinking about truth—one oriented by imperfection, rather than the structure of appearance. Understanding Mendelssohn as a philosopher of imperfection should affect how we read the word ‘truth’ in Modern Jewish philosophy: if imperfection is a fundamental ingredient of human life, then it is not something we must do away with, or annihilate, in order to find truth; it is not an obstacle. Rather—if we, like Mendelssohn, assume that we are incomplete and compromised—any relationship to truth must not seek to overcome imperfection and compromise, but proceed through them.
A flexible analytic model of cosmic variance in the first billion years
Authors: Trapp A C , Furlanetto Steven R 
Published: September 2020

ABSTRACT
Cosmic variance is the intrinsic scatter in the number density of galaxies due to fluctuations in the large-scale dark matter density field. In this work, we present a simple analytic model of cosmic variance in the high-redshift Universe (z ∼ 5–15). We assume that galaxies grow according to the evolution of the halo mass function, which we allow to vary with large-scale environment. Our model produces a reasonable match to the observed ultraviolet (UV) luminosity functions in this era by regulating star formation through stellar feedback and assuming that the UV luminosity function is dominated by recent star formation. We find that cosmic variance in the UV luminosity function is dominated by the variance in the underlying dark matter halo population, and not by differences in halo accretion or the specifics of our stellar feedback model. We also find that cosmic variance dominates over Poisson noise for future high-z surveys except for the brightest sources or at very high redshifts (z ≳ 12). We provide a linear approximation of cosmic variance for a variety of redshifts, magnitudes, and survey areas through the public python package galcv. Finally, we introduce a new method for incorporating priors on cosmic variance into estimates of the galaxy luminosity function and demonstrate that it significantly improves constraints on that important observable.
WASP-186 and WASP-187: two hot Jupiters discovered by SuperWASP and SOPHIE with additional observations by TESS
Authors: Schanche N , Hébrard G , Collier Cameron A , Dalal S , Smalley B , Wilson T G , Boisse I , Bouchy F , Brown D J A , Demangeon O , Haswell C A , Hellier C , Kolb U C , Lopez T , Maxted P F L , Pollacco D L , West R G , Wheatley P J 
Published: September 2020

ABSTRACT
We present the discovery of two new hot Jupiters identified from the Wide-Angle Search for Planets (WASP) survey, WASP-186b and WASP-187b (TOI-1494.01 and TOI-1493.01). Their planetary nature was established from SOPHIE spectroscopic observations, and additional photometry was obtained from Transiting Exoplanet Survey Satellite. Stellar parameters for the host stars are derived from spectral line, infrared flux method, and isochrone placement analyses. These parameters are combined with the photometric and radial velocity data in a Markov chain Monte Carlo method to determine the planetary properties. WASP-186b is a massive Jupiter (4.22 ± 0.18 MJ, 1.11 ± 0.03 RJ) orbiting a mid-F star on a 5.03-d eccentric (e = 0.327 ± 0.008) orbit. WASP-187b is a low-density (0.80 ± 0.09 MJ, 1.64 ± 0.05 RJ) planet in a 5.15-d circular orbit around a slightly evolved early F-type star.
The efficiency of nuclear burning during thermonuclear (Type I) bursts as a function of accretion rate
Authors: Cavecchi Y , Galloway D K , Goodwin A J , Johnston Z , Heger A 
Published: September 2020

ABSTRACT
We measured the thermonuclear burning efficiency as a function of accretion rate for the Type I X-ray bursts of five low-mass X-ray binary systems. We chose sources with measured neutron star spins and a substantial population of bursts from a large observational sample. The general trend for the burst rate is qualitatively the same for all sources; the burst rate first increases with the accretion rate up to a maximum, above which the burst rate declines, despite the increasing accretion rate. At higher accretion rates, when the burst rate decreases, the α-value (the ratio of accretion energy and burst energy) increases by up to a factor of 10 above that in the rising burst rate regime. These observations are contrary to the predictions of 1D numerical models, but can be explained as the consequence of a zone of stable burning on the neutron star surface, which expands with increasing accretion rate. The stable burning also ‘pollutes’ the unstable burning layer with ashes, contributing to the change in burst properties measured in the falling burst rate regime. We find that the mass accretion rate at which the burst rate begins to decrease is anticorrelated with the spin of the neutron star. We conclude that the neutron star spin is a key factor, moderating the nuclear burning stability, via the local accretion rate and fuel composition over the star.
The first shear measurements from precision weak lensing
Authors: Gurri Pol , Taylor Edward N , Fluke Christopher J 
Published: September 2020

ABSTRACT
We present an end-to-end methodology to measure the effects of weak lensing on individual galaxy–galaxy systems exploiting their kinematic information. Using this methodology, we have measured a shear signal from the velocity fields of 18 weakly lensed galaxies. We selected a sample of systems based only on the properties of the sources, requiring them to be bright (apparent i-band magnitude &lt;17.4) and in the nearby Universe ($z$ &lt; 0.15). We have observed the velocity fields of the sources with WiFeS, an optical IFU on a 2.3 m telescope, and fitted them using a simple circular motion model with an external shear. We have measured an average shear of 〈γ〉 = 0.020 ± 0.008 compared to a predicted 〈γpred〉 = 0.005 obtained using median stellar-to-halo relationships from the literature. While still a statistical approach, our results suggest that this new weak lensing methodology can overcome some of the limitations of traditional stacking-based techniques. We describe in detail all the steps of the methodology and make publicly available all the velocity maps for the weakly lensed sources used in this study.
Power-law energy distributions of small-scale impulsive events on the active Sun: results from IRIS
Authors: Vilangot Nhalil Nived , Nelson Chris J , Mathioudakis Mihalis , Doyle J Gerry , Ramsay Gavin 
Published: September 2020

ABSTRACT
Numerous studies have analysed inferred power-law distributions between frequency and energy of impulsive events in the outer solar atmosphere in an attempt to understand the predominant energy supply mechanism in the corona. Here, we apply a burst detection algorithm to high-resolution imaging data obtained by the Interface Region Imaging Spectrograph to further investigate the derived power-law index, γ, of bright impulsive events in the transition region. Applying the algorithm with a constant minimum event lifetime (of either 60 s or 110 s) indicated that the target under investigation, such as Plage and Sunspot, has an influence on the observed power-law index. For regions dominated by sunspots, we always find γ &lt; 2; however, for data sets where the target is a plage region, we often find that γ &gt; 2 in the energy range (∼1023, ∼1026) erg. Applying the algorithm with a minimum event lifetime of three time-steps indicated that cadence was another important factor, with the highest cadence data sets returning γ &gt; 2 values. The estimated total radiative power obtained for the observed energy distributions is typically 10–25 per cent of what would be required to sustain the corona indicating that impulsive events in this energy range are not sufficient to solve coronal heating. If we were to extend the power-law distribution down to an energy of 1021 erg, and assume parity between radiative energy release and the deposition of thermal energy, then such bursts could provide 25–50 per cent of the required energy to account for the coronal heating problem.
Fast estimation of aperture mass statistics – I. Aperture mass variance and an application to the CFHTLenS data
Authors: Porth Lucas , Smith Robert E , Simon Patrick , Marian Laura , Hilbert Stefan 
Published: September 2020

ABSTRACT
We explore an alternative method to the usual shear correlation function approach for the estimation of aperture mass statistics in weak lensing survey data. Our approach builds on the direct estimator method. In this paper, to test and validate the methodology, we focus on the aperture mass dispersion. After computing the signal and noise for a weighted set of measured ellipticites we show how the direct estimator can be made into a linear order algorithm that enables a fast and efficient computation. We then investigate the applicability of the direct estimator approach in the presence of a real survey mask with holes and chip gaps. For this we use a large ensemble of full ray-tracing mock simulations. By using various weighting schemes for combining information from different apertures we find that inverse variance weighting the individual aperture estimates with an aperture completeness greater than 70 per cent yields an answer that is in close agreement with the correlation function approach. We then apply this approach to the CFHTLenS as a pilot scheme and find that our method recovers to high accuracy the official result for the variance of both the E- and B-mode signal. We then explore the cosmological information content of the direct estimator using the Fisher information approach. We show that there is a only modest loss in cosmological information from the rejection of apertures that are of low completeness. This method unlocks the door to efficient methods for recovering higher order aperture mass statistics in linear order operations.
Shock–multicloud interactions in galactic outflows – I. Cloud layers with lognormal density distributions
Authors: Banda-Barragán W E , Brüggen M , Federrath C , Wagner A Y , Scannapieco E , Cottle J 
Published: September 2020

ABSTRACT
We report three-dimensional hydrodynamical simulations of shocks (${\cal M_{\rm shock}}\ge 4$) interacting with fractal multicloud layers. The evolution of shock–multicloud systems consists of four stages: a shock-splitting phase in which reflected and refracted shocks are generated, a compression phase in which the forward shock compresses cloud material, an expansion phase triggered by internal heating and shock re-acceleration, and a mixing phase in which shear instabilities generate turbulence. We compare multicloud layers with narrow ($\sigma _{\rho }=1.9\bar{\rho }$) and wide ($\sigma _{\rho }=5.9\bar{\rho }$) lognormal density distributions characteristic of Mach ≈ 5 supersonic turbulence driven by solenoidal and compressive modes. Our simulations show that outflowing cloud material contains imprints of the density structure of their native environments. The dynamics and disruption of multicloud systems depend on the porosity and the number of cloudlets in the layers. ‘Solenoidal’ layers mix less, generate less turbulence, accelerate faster, and form a more coherent mixed-gas shell than the more porous ‘compressive’ layers. Similarly, multicloud systems with more cloudlets quench mixing via a shielding effect and enhance momentum transfer. Mass loading of diffuse mixed gas is efficient in all models, but direct dense gas entrainment is highly inefficient. Dense gas only survives in compressive clouds, but has low speeds. If normalized with respect to the shock-passage time, the evolution shows invariance for shock Mach numbers ≥10 and different cloud-generating seeds, and slightly weaker scaling for lower Mach numbers and thinner cloud layers. Multicloud systems also have better convergence properties than single-cloud systems, with a resolution of eight cells per cloud radius being sufficient to capture their overall dynamics.
η Carinae: high angular resolution continuum, H30α and He30α ALMA images
Authors: Abraham Zulema , Beaklini Pedro P B , Cox Pierre , Falceta-Gonçalves Diego , Nyman Lars-Åke 
Published: September 2020

ABSTRACT
We present images of η Carinae in the recombination lines H30α and He30α and the underlying continuum with 50 mas resolution (110 au), obtained with ALMA. For the first time, the 230 GHz continuum image is resolved into a compact core, coincident with the binary system position, and a weaker extended structure to the NW of the compact source. Iso-velocity images of the H30α recombination line show at least 16 unresolved sources with velocities between −30 and −65 km s−1 distributed within the continuum source. A NLTE model, with density and temperature of the order of 107 cm−3 and 104 K, reproduce both the observed H30α line profiles and their underlying continuum flux densities. Three of these sources are identified with Weigelt blobs D, C, and B; estimating their proper motions, we derive ejection times (in years) of 1952.6, 1957.1, and 1967.6, respectively, all of which are close to periastron passage. Weaker H30α line emission is detected at higher positive and negative velocities, extending in the direction of the Homunculus axis. The He30α recombination line is also detected with the same velocity of the narrow H30α line. Finally, the close resemblance of the H30α image with that of an emission line that was reported in the literature as HCO+(4–3) led us to identify this line as H40δ instead, an identification that is further supported by modelling results. Future observations will enable to determine the proper motions of all the compact sources discovered in the new high angular resolution data of η Carinae.
J-factor estimation of Draco, Sculptor, and Ursa Minor dwarf spheroidal galaxies with the member/foreground mixture model
Authors: Horigome Shun-ichi , Hayashi Kohei , Ibe Masahiro , Ishigaki Miho N , Matsumoto Shigeki , Sugai Hajime 
Published: September 2020

ABSTRACT
Dwarf spheroidal galaxies (dSphs) are promising targets of indirect detection experiments searching for dark matter (DM) at present Universe. Towards robust prediction for the amount of signal flux originating in DM annihilation inside dSphs, a precise determination of DM distributions as well as J-factors of the dSphs is particularly important. In this work, we estimate those of Draco, Sculptor, and Ursa Minor dSphs by an improved statistical method in which both foreground stars and dSph member stars are simultaneously taken into account. We define the likelihood function of the method as the so-called conditional one to remove sampling bias of observed stellar data. This improved method enables us to estimate DM distributions and J-factors of the dSphs directly from observed stellar data contaminated by foreground stars without imposing stringent membership criteria on the measured quantities.
The application of the adiabatic compression scenario to the radio relic in the galaxy cluster Abell 3411−3412
Authors: Button Charissa , Marchegiani Paolo 
Published: September 2020

ABSTRACT
Although radio relics are understood to originate in intracluster shock waves resulting from merger shocks, the most widely used model for describing this (re-)acceleration process at shock fronts, the diffusive shock acceleration (DSA) model, has several challenges, including the fact that it is inefficient at low shock Mach numbers. In light of these challenges, it is worthwhile to consider alternative mechanisms. One possibility is the adiabatic compression by a shock wave of a residual fossil electron population which has been left over from a radio galaxy jet. This paper applies this model to the relic hosted in the merging galaxy cluster Abell 3411−3412, where a radio bridge between the relic and a radio galaxy has been observed, with the aim to reproduce the spatial structure of the spectral index of the relic. Four scenarios are presented, in which different effects are investigated, such as effects behind the shock front and different shock strengths. The results show that the adiabatic compression model can reproduce the observed spectral indices across the relic for a shock Mach number that is lower than the value required by the DSA-type modelling of this relic and is in accordance with the values derived from X-ray observations, if other mechanisms, such as an expansion phase or post-shock turbulence, are effective behind the shock front.
SDSS-IV MaNGA: the indispensable role of bars in enhancing the central star formation of low-z galaxies
Authors: Lin Lin , Li Cheng , Du Cheng , Wang Enci , Xiao Ting , Bureau Martin , Fraser-McKelvie Amelia , Masters Karen , Lin Lihwai , Wake David , Hao Lei 
Published: September 2020

ABSTRACT
We analyse two-dimensional maps and radial profiles of EW(Hα), EW(HδA), and Dn(4000) of low-redshift galaxies using integral field spectroscopy from the MaNGA survey. Out of ≈1400 nearly face-on late-type galaxies with a redshift z &lt; 0.05, we identify 121 “turnover” galaxies that each have a central upturn in EW(Hα), EW(HδA), and/or a central drop in Dn(4000), indicative of ongoing/recent star formation. The turnover features are found mostly in galaxies with a stellar mass above ∼1010 M⊙ and NUV – r colour less than ≈5. The majority of the turnover galaxies are barred, with a bar fraction of 89 ± 3 per cent. Furthermore, for barred galaxies, the radius of the central turnover region is found to tightly correlate with one-third of the bar length. Comparing the observed and the inward extrapolated star formation rate surface density, we estimate that the central SFR have been enhanced by an order of magnitude. Conversely, only half of the barred galaxies in our sample have a central turnover feature, implying that the presence of a bar is not sufficient to lead to a central SF enhancement. We further examined the SF enhancement in paired galaxies, as well as the local environment, finding no relation. This implies that the environment is not a driving factor for central SF enhancement in our sample. Our results reinforce both previous findings and theoretical expectation that galactic bars play a crucial role in the secular evolution of galaxies by driving gas inflow and enhancing the star formation and bulge growth in the centre.