bluuebunny/crossref_metadata_2025_split huggingface dataset:
Psychophysics of the hoverfly: categorical or continuous color discrimination?
Authors: Hannah Lea , Dyer Adrian G , Garcia Jair E , Dorin Alan , Burd Martin 
Published: March 2019

AbstractThere is increasing interest in flies as potentially important pollinators. Flies are known to have a complex visual system, including 4 spectral classes of photoreceptors that contribute to the perception of color. Our current understanding of how color signals are perceived by flies is based on data for the blowfly Lucilia sp., which after being conditioned to rewarded monochromatic light stimuli, showed evidence of a categorical color visual system. The resulting opponent fly color space has 4 distinct categories, and has been used to interpret how some fly pollinators may perceive flower colors. However, formal proof that flower flies (Syrphidae) only use a simple, categorical color process remains outstanding. In free-flying experiments, we tested the hoverfly Eristalis tenax, a Batesian mimic of the honeybee, that receives its nutrition by visiting flowers. Using a range of broadband similar–dissimilar color stimuli previously used to test color perception in pollinating hymenopteran species, we evaluated if there are steep changes in behavioral choices with continuously increasing color differences as might be expected by categorical color processing. Our data revealed that color choices by the hoverfly are mediated by a continuous monotonic function. Thus, these flies did not use a categorical processing, but showed evidence of a color discrimination function similar to that observed in several bee species. We therefore empirically provide data for the minimum color distance that can be discriminated by hoverflies in fly color space, enabling an improved understanding of plant–pollinator interactions with a non-model insect species.
Overcoming long Bayesian run times in integrated fisheries stock assessments
Authors: Monnahan Cole C , Branch Trevor A , Thorson James T , Stewart Ian J , Szuwalski Cody S 
Published: March 2019

AbstractBayesian inference is an appealing alternative to maximum likelihood estimation, but estimation can be prohibitively long for integrated fisheries stock assessments. Here, we investigated potential causes of long run times including high dimensionality, complex model structure, and inefficient Bayesian algorithms for four US assessments written in AD Model Builder (ADMB), both custom built and Stock Synthesis models. The biggest culprit for long run times was overparameterization and they were reduced from months to days by adding priors and turning off estimation for poorly-informed parameters (i.e. regularization), especially for selectivity parameters. Thus, regularization is a necessary step in converting assessments from frequentist to Bayesian frameworks. We also tested the usefulness of the no-U-turn sampler (NUTS), a Bayesian algorithm recently added to ADMB, and the R package adnuts that allows for easy implementation of NUTS and parallel computation. These additions further reduced run times and better sampled posterior distributions than existing Bayesian algorithms in ADMB, and for both of these reasons we recommend using NUTS for inference. Between regularization, a faster algorithm, and parallel computation, we expect models to run 50–50 000 times faster for most current stock assessment models, opening the door to routine usage of Bayesian methods for management of fish stocks.
Postoperative atrial fibrillation after aortic valve replacement is a risk factor for long-term atrial fibrillation
Authors: Carter-Storch Rasmus , Dahl Jordi S , Christensen Nicolaj L , Pecini Redi , Søndergård Eva V , Øvrehus Kristian Altern , Møller Jacob E 
Published: March 2019

AbstractOBJECTIVESPostoperative atrial fibrillation (POAF) is a common complication following cardiac surgery. However, knowledge on the rate of long-term atrial fibrillation (LTAF) after POAF remains unclear. We investigated predictors of POAF in patients with aortic stenosis undergoing surgical aortic valve replacement, and assessed the rate of LTAF during follow-up.METHODSWe prospectively included 96 adult patients with severe aortic stenosis undergoing surgical aortic valve replacement. Patients with previous atrial fibrillation (AF) were excluded. Patients underwent echocardiography, cardiac computed tomography and magnetic resonance imaging immediately prior to surgery. Surgical aortic clamp time and postoperative C-reactive protein (CRP) were documented. POAF was defined as AF recorded within 7 days of surgery. Through chart review, patients were followed up for documented episodes of LTAF occurring more than 7 days after surgery.RESULTSPOAF occurred in 51 patients (53%). It was associated with larger preoperative echocardiographic left atrial volume index (44 ± 12 vs 37 ± 8 ml/m2, P = 0.004), longer aortic clamp time [80 (70–102) vs 72 (62–65) min, P = 0.04] and higher CRP on first postoperative day [80 (64–87) vs 65 (44–83) mg/l, P = 0.001]. Multivariable logistic regression revealed that left atrial volume index [odds ratio (OR) 1.07, 95% confidence interval (CI) 1.02–1.13; P = 0.005] and postoperative CRP (OR 1.03, 95% CI 1.01–1.05; P = 0.006) were the only independent predictors of POAF. During 695 days (25th–75th percentile: 498–859 days) of follow-up, LTAF occurred in 11 patients of whom 10 were in the POAF group (hazard ratio 9.4, 95% CI 1.2–74; P = 0.03).CONCLUSIONSPOAF is predicted by left atrial volume index and postoperative CRP. Patients with POAF have a 9-fold increase risk of developing symptomatic LTAF during follow-up.Clinical trial registration numberClinicalTrials.gov (NCT02316587).
La ‘terza stanza de quadri’ in Palazzo Farnese nel 1644
Authors: Pierguidi Stefano 
Published: March 2019

Abstract
L’articolo punta a stabilire il criterio museografico nell’allestimento della ‘terza stanza de quadri’ in Palazzo Farnese nel 1644, a partire dalla sorprendente presenza in quell’ambiente di molti disegni incorniciati accanto a dipinti su tavola a fondo oro di primo Quattrocento e a poche, importanti tele. Nella stanza era sinteticamente narrata la storia della pittura a Roma dal Quattro al Cinquecento, attraverso soli capolavori, di maestri quasi unicamente appartenenti alla scuola romana.
This article aims to establish the museographic criteria involved in the display of pictures in the ‘third room of paintings’ in the Palazzo Farnese in 1644, beginning with the surprising presence there of many framed drawings next to paintings on panel with gold background of the early fifteenth century and with few modern paintings of great importance. Here the story of painting in Rome in the Quattrocento and Cinquecento was synthetically narrated through masterpieces belonging almost exclusively to the Roman School.
Respect for Home and the Family
Authors: Fiala-Butora János 
Published: March 2019

Abstract
This chapter examines Article 23 of the United Nations Convention on the Rights of Persons with Disabilities. The right to family life and its various components have long been recognized by international human rights law and in regional human rights instruments. Despite this long tradition of protecting the family in human rights law, persons with disabilities have long been subject to serious violations of their right to family life. The prevailing stereotype has considered persons with disabilities asexual, which has led to the denial of their sexual autonomy. The right to family life also encompasses all forms of relationships and parenthood. To be truly equal members of society, persons with disabilities must achieve equality of opportunity in these areas as well. This requires significant attitudinal change, empowerment, dismantling of barriers, and support to experience intimate relationships.
Education
Authors: Anastasiou Dimitris , Gregory Michael , Kauffman James M 
Published: March 2019

Abstract
This chapter examines Article 24 of the United Nations Convention on the Rights of Persons with Disabilities (CRPD), which recognizes the right of persons with disabilities (PWD) to education and lifelong learning, specifying obligations of states parties that are necessary for realizing this right. Consistent with the CRPD as a whole and with other human rights treaties, it seeks to eliminate discrimination against and equalize educational opportunities for PWD. Nevertheless, it is argued that several tensions and ambiguities embodied in Article 24 raise questions about its efficacy for ultimately achieving its important vision. Despite its categorization as an ‘economic, social, and cultural right’, Article 24 appears to operate in practice primarily as an anti-discrimination measure, which inhibits its potential for securing socio-economic justice for all PWD. In this regard, it diverges from the paradigm that has characterized other international statements on the right to education.
Conference of States Parties
Authors: Bantekas Ilias 
Published: March 2019

Abstract
This chapter examines Article 40 of the United Nations Convention on the Rights of Persons with Disabilities (CRPD), which deals with the Conference of States Parties (COSP). The COSP is part of an established tradition whose principal aim is to keep the Convention alive by stimulating actions, collaborations, enforcement, capacity building, and others. The enforcement powers of the COSP are severely limited, if any, and should not therefore be compared to those enjoyed by entities with enforcement powers, such as the UN Security Council or the Council of the European Union. Although the powers and functions of the COSP could be achieved outside the legal person of the COSP on the basis of joint action by CRPD member states, the formal collectivization of member states ensures annual discussions on important and emerging issues affecting disability rights and contributes towards a consistency among a group of equal partners undertaking the same obligations.
Atmospheric mass-loss due to giant impacts: the importance of the thermal component for hydrogen–helium envelopes
Authors: Biersteker John B , Schlichting Hilke E 
Published: March 2019

ABSTRACT
Systems of super-Earths and mini-Neptunes display striking variety in planetary bulk density and composition. Giant impacts are expected to play a role in the formation of many of these worlds. Previous works, focused on the mechanical shock caused by a giant impact, showed that these impacts can eject large fractions of the planetary envelope, offering a partial explanation for the observed compositional diversity. Here, we examine the thermal consequences of giant impacts, and show that the atmospheric loss caused by these effects can significantly exceed that caused by mechanical shocks for hydrogen–helium (H/He) envelopes. During a giant impact, part of the impact energy is converted into thermal energy, heating the rocky core and envelope. We find that the ensuing thermal expansion of the envelope can lead to a period of sustained, rapid mass-loss through a Parker wind, partly or completely eroding the H/He envelope. The degree of atmospheric loss depends on the planet’s orbital distance from its host star and its initial thermal state, and hence age. Close-in planets and younger planets are more susceptible to impact-triggered atmospheric loss. For planets where the heat capacity of the core is much greater than the envelope’s heat capacity (envelope mass fractions ≲4 per cent), the impactor mass required for significant atmospheric removal is Mimp/Mp ∼ μ/μc ∼ 0.1, approximately the ratio of the heat capacities of the envelope and core. Conversely, when the envelope dominates the planet’s heat capacity, complete loss occurs when the impactor mass is comparable to the envelope mass.
System initial mass function of the 25 Ori group from planetary-mass objects to intermediate/high-mass stars
Authors: Suárez Genaro , Downes Juan José , Román-Zúñiga Carlos , Cerviño Miguel , Briceño César , Petr-Gotzens Monika G , Vivas Katherina 
Published: March 2019

Abstract
The stellar initial mass function (IMF) is an essential input for many astrophysical studies but only in a few cases has it been determined over the whole cluster mass range, limiting the conclusions about its nature. The 25 Orionis group (25 Ori) is an excellent laboratory for investigating the IMF across the entire mass range of the population, from planetary-mass objects to intermediate/high-mass stars. We combine new deep optical photometry with optical and near-infrared data from the literature to select 1687 member candidates covering a 1.1° radius area in 25 Ori. With this sample we derived the 25 Ori system IMF from 0.012 to 13.1 M⊙. This system IMF is well described by a two-segment power law with Γ = −0.74 ± 0.04 for m &lt; 0.4 M⊙ and Γ = 1.50 ± 0.11 for m ≥ 0.4 M⊙. It is also well described over the whole mass range by a tapered power-law function with Γ = 1.10 ± 0.09, mp = 0.31 ± 0.03 and β = 2.11 ± 0.09. The best lognormal representation of the system IMF has mc = 0.31 ± 0.04 and σ = 0.46 ± 0.05 for m &lt; 1 M⊙. This system IMF does not present significant variations with the radii. We compared the resultant system IMF as well as the brown dwarf/star ratio of 0.16 ± 0.03 that we estimated for 25 Ori with that of other stellar regions with diverse conditions and found no significant discrepancies. These results support the idea that general star-formation mechanisms are probably not strongly dependent on environmental conditions. We found that the substellar and stellar objects in 25 Ori do not have any preferential spatial distributions and confirmed that 25 Ori is a gravitationally unbound stellar association.
Radiative transfer of hydrogen lines from supernova remnant shock waves: contributions of 2s-state hydrogen atoms
Authors: Shimoda Jiro , Laming J Martin 
Published: March 2019

Abstract
Radiative transfer in hydrogen lines in supernova remnant (SNR) shock waves is studied taking into account the population of the hydrogen atom 2s-state. Measurements of Balmer line emission, especially of H α, are often relied on to derive physical conditions in the SNR shock. On the other hand, Lyman series photons, especially Ly β, are mostly absorbed by upstream hydrogen atoms. As a result, atoms are excited to the 3p state, and then emit H α by the spontaneous transition from 3p to 2s. Thus, the nature of H α depends on how many Ly β photons are converted to H α photons. Moreover, the Balmer lines can be scattered by the 2s-state hydrogen atoms, which are excited not only by collisional excitation but also by the Lyman–Balmer conversion. It is shown for example that the H α photons are scattered if the shock propagates into an H i cloud with a density of ∼30 cm−3 and a size of ∼1 pc. We find that the line profile of H α becomes asymmetric resulting from the difference between line centre frequencies among the transitions from 3s to 2p, from 3p to 2s, and from 3d to 2p. We also find that the broad-to-narrow ratio of H α, which is often used to estimate the ion-electron temperature equilibrium, varies at most ≃ 10 per cent depending on the ionization degree of the upstream medium because of incomplete conversion of Lyman lines to Balmer lines.
Chemical analysis of CH stars – III. Atmospheric parameters and elemental abundances
Authors: Purandardas Meenakshi , Goswami Aruna , Goswami Partha Pratim , Shejeelammal J , Masseron Thomas 
Published: March 2019

Abstract
Elemental abundances of CH stars can provide observational constraints for theoretical studies on the nucleosynthesis and evolution of low- and intermediate-mass stars. However, available abundance data in literature are quite scanty. In our pursuit to generate a homogeneous data base of elemental abundances of CH stars we have performed a detailed chemical abundance study for a sample of 12 potential CH star candidates based on high-resolution spectroscopy. We present first time abundance analysis for the objects HE0308–1612, CD−281082, HD30443, and HD87853. For the other objects, although limited information is available, detailed chemical composition studies are missing. Our analysis shows CD−281082 to be a very metal-poor object with [Fe/H] = −2.45 and enriched in carbon with [C/Fe] = 2.19. With a ratio of [Ba/Eu] ∼ 0.02 the star satisfies the classification criteria of a CEMP-r/s star. The objects CD−382151 with [Fe/H] = −2.03 and HD30443 with [Fe/H] ∼ −1.68 are found to show the characteristic properties of CH stars. HE0308–1612 and HD87853 are found to be moderately metal poor with [Fe/H] ∼ −0.73; while HE0308–1612 is moderately enhanced with carbon ([C/Fe] ∼ 0.78) and shows the spectral properties of CH stars, the abundance of carbon could not be estimated for HD87853. Among the two moderately metal-poor objects, HD87080 ([Fe/H] = −0.48) shows near solar carbon abundance, and HD176021 ([Fe/H] = −0.63) is mildly enhanced in carbon with [C/Fe] = 0.52. HD176021 along with HD202020 a known binary, exhibit the characteristic properties of CH stars as far as the heavy element abundances are concerned. Five objects in our sample show spectral properties that are normally seen in barium stars.
Quasar Sightline and Galaxy Evolution (QSAGE) survey – I. The galaxy environment of O vi absorbers up to z = 1.4 around PKS 0232−04
Authors: Bielby R M , Stott J P , Cullen F , Tripp T M , Burchett J N , Fumagalli M , Morris S L , Tejos N , Crain R A , Bower R G , Prochaska J X 
Published: March 2019

ABSTRACT
We present the first results from a study of O vi absorption around galaxies at z &lt; 1.44 using data from a near-infrared grism spectroscopic Hubble Space Telescope Large Programme, the Quasar Sightline and Galaxy Evolution (QSAGE) survey. QSAGE is the first grism galaxy survey to focus on the circumgalactic medium at z ∼ 1, providing a blind survey of the galaxy population. The galaxy sample is H α flux limited (f(H α) &gt; 2 × 10−17 erg s−1 cm−2) at 0.68 &lt; z &lt; 1.44, corresponding to ≳0.2–0.8 M⊙ yr−1. In this first of 12 fields, we combine the galaxy data with high-resolution STIS and COS spectroscopy of the background quasar to study O vi in the circumgalactic medium. At z ∼ 1, we find O vi absorption systems up to b ∼ 350 kpc (∼4Rvir) from the nearest detected galaxy. Further, we find ${\sim }50{{\ \rm per\ cent}}$ of ≳1 M⊙ yr−1 star-forming galaxies within 2Rvir show no associated O vi absorption to a limit of at least N(O vi) = 1013.9 cm−2. That we detect O vi at such large distances from galaxies and that a significant fraction of star-forming galaxies show no detectable O vi absorption disfavours outflows from ongoing star formation as the primary medium traced by these absorbers. Instead, by combining our own low- and high-redshift data with existing samples, we find tentative evidence for many strong (N(O vi) &gt; 1014 cm−2) O vi absorption systems to be associated with M⋆ ∼ 109.5–10 M⊙ mass galaxies (Mhalo ∼ 1011.5–12 M⊙ dark matter haloes), and infer that they may be tracing predominantly collisionally ionized gas within the haloes of such galaxies.
Spectroscopic confirmation and modelling of two lensed quadruple quasars in the Dark Energy Survey public footprint
Authors: Spiniello C , Sergeyev A V , Marchetti L , Tortora C , Napolitano N R , Shalyapin V , Agnello A , Getman F I , Vaccari M , Serjeant S , Koopmans L V E , Baker A J , Jarrett T H , Covone G , Vernardos G 
Published: March 2019

ABSTRACT
Quadruply lensed quasars are extremely rare objects, but incredibly powerful cosmological tools. Only few dozen are known in the whole sky. Here we present the spectroscopic confirmation of two new quadruplets WG0214-2105 and WG2100-4452 discovered by Agnello & Spiniello (2018) within the Dark Energy Survey public footprints. We have conducted spectroscopic follow-up of these systems with the Southern African Large Telescope as part of a program that aims at confirming the largest possible number of strong gravitational lenses in the equatorial and Southern hemisphere. For both systems, we present the sources spectra that allowed us to estimate their redshifts and unambiguously confirm their lensing nature. For the brighter deflector (WG2100-4452) we measure the spectroscopic redshift and the stellar velocity dispersion from optical absorption lines in the spectrum. For the other system we infer the lens redshift from photometry, being the quality of the spectra not good enough. We obtain photometry for both lenses, directly from multiband images, isolating the lenses from the quasars. One of the quadruplets, WG0214-2105, was also observed by Pan-STARRS, allowing us to estimate the apparent brightness of each quasar image at two different epochs, and thus to find evidence for flux variability. This result could suggest a microlensing event for the faintest components, although intrinsic variability cannot be excluded with only two epochs. Finally, we present simple lens models for both quadruplets, obtaining Einstein radii, singular isothermal ellipsoid velocity dispersions, ellipticities, and position angles of the lenses, as well as time-delay predictions assuming a concordance cosmological model.
Private foundations and the conflict of laws
Authors: Goldsworth John Graham 
Published: March 2019

Abstract
The straightforward nature of private foundations compared with trusts may not be apparent where a private foundation is formed under one jurisdiction’s laws but administered elsewhere if the lex fori introduces concepts that are unforeseen at the time that the private foundation is entered into. This possibility should be guarded against by an examination both of the private foundation’s constitutional documents and the conflict of law rules of a likely forum to hear disputes.
MglA functions as a three-state GTPase to control movement reversals of Myxococcus xanthus
Authors: Galicia Christian , Lhospice Sébastien , Fernández Varela Paloma , Trapani Stefano , Zhang Wenhua , Navaza Jorge , Mignot Tâm , Cherfils Jacqueline 
Published: March 2019

AbstractIn Myxococcus xanthus, directed movement is controlled by inter-dependent pole-to-pole oscillations of the small GTPase MglA, its GAP MglB and the RomR protein. However, these proteins have strikingly different oscillatory regimes such that MglA is segregated from MglB and RomR at reversal activation. The molecular mechanism whereby information is exchanged between the lagging and leading poles resulting in MglA detachment from the leading pole during reversals has remained unknown. Here, we show that MglA has two GTP-bound forms, one of which is insensitive to MglB (MglA-GTP*) and is re-sensitized to MglB by a feedback mechanism operated by MglA-GDP. By identifying the region of MglB that is critical for its association to the lagging pole, we demonstrate that MglA-GTP* is functional in vivo. These data suggest that MglA-GDP acts as a soluble messenger to convert polar MglA-GTP* into a diffusible MglA-GTP species, explaining MglA re-localization to the opposite pole during reversals.