bluuebunny/crossref_metadata_2025_split huggingface dataset:
Avian Coloration Genetics: Recent Advances and Emerging Questions
Authors: Price-Waldman Rosalyn , Stoddard Mary Caswell 
Published: March 2021

AbstractThe colorful phenotypes of birds have long provided rich source material for evolutionary biologists. Avian plumage, beaks, skin, and eggs—which exhibit a stunning range of cryptic and conspicuous forms—inspired early work on adaptive coloration. More recently, avian color has fueled discoveries on the physiological, developmental, and—increasingly—genetic mechanisms responsible for phenotypic variation. The relative ease with which avian color traits can be quantified has made birds an attractive system for uncovering links between phenotype and genotype. Accordingly, the field of avian coloration genetics is burgeoning. In this review, we highlight recent advances and emerging questions associated with the genetic underpinnings of bird color. We start by describing breakthroughs related to 2 pigment classes: carotenoids that produce red, yellow, and orange in most birds and psittacofulvins that produce similar colors in parrots. We then discuss structural colors, which are produced by the interaction of light with nanoscale materials and greatly extend the plumage palette. Structural color genetics remain understudied—but this paradigm is changing. We next explore how colors that arise from interactions among pigmentary and structural mechanisms may be controlled by genes that are co-expressed or co-regulated. We also identify opportunities to investigate genes mediating within-feather micropatterning and the coloration of bare parts and eggs. We conclude by spotlighting 2 research areas—mechanistic links between color vision and color production, and speciation—that have been invigorated by genetic insights, a trend likely to continue as new genomic approaches are applied to non-model species.
The need for alternative plant species interaction models
Authors: Damgaard Christian , Weiner Jacob 
Published: March 2021

Abstract

Aims
The limitations of classical Lotka–Volterra models for analyzing and interpreting competitive interactions among plant species have become increasingly clear in recent years. Three of the problems that have been identified are (i) the absence of frequency-dependence, which is important for long-term coexistence of species, (ii) the need to take unmeasured (often unmeasurable) variables influencing individual performance into account (e.g. spatial variation in soil nutrients or pathogens) and (iii) the need to separate measurement error from biological variation.

Methods
We modified the classical Lotka–Volterra competition models to address these limitations. We fitted eight alternative models to pin-point cover data on Festuca ovina and Agrostis capillaris over 3 years in an herbaceous plant community in Denmark. A Bayesian modeling framework was used to ascertain whether the model amendments improve the performance of the models and increase their ability to predict community dynamics and to test hypotheses.

Important Findings
Inclusion of frequency-dependence and measurement error, but not unmeasured variables, improved model performance greatly. Our results emphasize the importance of comparing alternative models in quantitative studies of plant community dynamics. Only by considering possible alternative models can we identify the forces driving community assembly and change, and improve our ability to predict the behavior of plant communities.
Management of deltopectoral flap failure using a three-stage revision reconstruction: a case report
Authors: Chotipanich Adit , Wongmanee Sombat 
Published: March 2021

Abstract
Although deltopectoral flap failure is uncommon, its management can be difficult. This report presents a case of deltopectoral flap failure successfully rescued by a three-stage revision reconstruction using the postdebridement flap. A 59-year-old patient presented with a pharyngocutaneous fistula due to radionecrosis and subsequently underwent a medially based deltopectoral flap reconstruction for fistula closure. Unfortunately, this operation was unsuccessful because the flap developed necrosis at its distal tip, and the postdebridement flap could not be directly placed on the defect because of its shorter length. A subsequent revision operation successfully closed the fistula using a three-stage reconstruction with the postdebridement flap. Although this three-stage technique can avoid the morbidity associated with additional flap harvesting and can greatly extend the distance to the recipient, it also requires more time to heal and more operations than simply harvesting a new flap.
Inseparable Operations, Trinitarian Missions, and the Necessity of a Christological Pneumatology
Authors: Teer Torey J S 
Published: March 2021

Abstract
A pneumatology that is Christological in emphasis (Christological pneumatology) provides a valuable foil to a Christology that is pneumatological in emphasis (Spirit Christology). Furthermore, a Trinitarian Christological pneumatology offers a robust conception of the person and work of the Holy Spirit that at once acknowledges the centrality of Christ in redemptive history, aligns with orthodox Trinitarianism, and protects against common Trinitarian concerns. The framework of this model lies in a theological complex involving the doctrines of inseparable operations and distinct personal appropriations, the Trinitarian taxis (or order), and the Trinitarian missions. This article provides one step in constructing a theologically viable Christological pneumatology that contributes to the contemporary enrichment of evangelical theology concerning the Holy Spirit.
GARP transcription factors repress Arabidopsis nitrogen starvation response via ROS-dependent and -independent pathways
Authors: Safi Alaeddine , Medici Anna , Szponarski Wojciech , Martin Florence , Clément-Vidal Anne , Marshall-Colon Amy , Ruffel Sandrine , Gaymard Frédéric , Rouached Hatem , Leclercq Julie , Coruzzi Gloria , Lacombe Benoît , Krouk Gabriel 
Published: March 2021

Abstract
Plants need to cope with strong variations of nitrogen availability in the soil. Although many molecular players are being discovered concerning how plants perceive NO3− provision, it is less clear how plants recognize a lack of nitrogen. Following nitrogen removal, plants activate their nitrogen starvation response (NSR), which is characterized by the activation of very high-affinity nitrate transport systems (NRT2.4 and NRT2.5) and other sentinel genes involved in N remobilization such as GDH3. Using a combination of functional genomics via transcription factor perturbation and molecular physiology studies, we show that the transcription factors belonging to the HHO subfamily are important regulators of NSR through two potential mechanisms. First, HHOs directly repress the high-affinity nitrate transporters, NRT2.4 and NRT2.5. hho mutants display increased high-affinity nitrate transport activity, opening up promising perspectives for biotechnological applications. Second, we show that reactive oxygen species (ROS) are important to control NSR in wild-type plants and that HRS1 and HHO1 overexpressors and mutants are affected in their ROS content, defining a potential feed-forward branch of the signaling pathway. Taken together, our results define the relationships of two types of molecular players controlling the NSR, namely ROS and the HHO transcription factors. This work (i) up opens perspectives on a poorly understood nutrient-related signaling pathway and (ii) defines targets for molecular breeding of plants with enhanced NO3− uptake.
Maximum temperatures in evolving protoplanetary discs and composition of planetary building blocks
Authors: Li Min , Huang Shichun , Zhu Zhaohuan , Petaev Michail I , Steffen Jason H 
Published: March 2021

ABSTRACT
The maximum temperature and radial temperature profile in a protoplanetary disc are important for the condensation of different elements in the disc. We simulate the evolution of a set of protoplanetary discs from the collapse of their progenitor molecular cloud cores as well as the dust decoupling within the discs as they evolve. We show how the initial properties of the cloud cores affect the thermal history of the protoplanetary discs using a simple viscous disc model. Our results show that the maximum mid-plane temperature in the disc occurs within 0.5 au. It increases with the initial cloud temperature and decreases with its angular velocity and the viscosity of the disc. From the observed properties of the molecular cloud cores, we find the median value of the maximum temperature is around 1250 K, with roughly 90 per cent of them being less than 1500 K – a value that is lower than the 50 per cent condensation temperatures of most refractory elements. Therefore, only cloud cores with high initial temperatures or low-angular velocities and/or low viscosities within the planet-forming discs will result in refractory-rich planetesimals. To reproduce the volatile depletion pattern of CM, CO, and CV chondrites and the terrestrial planets in Solar system, one must either have rare properties of the initial molecular cloud cores like high core temperature, or other sources of energy to heat the disc to sufficiently high temperatures. Alternatively, the volatile depletion observed in these chondrites may be inherited from the progenitor molecular cloud.
From the CMF to the IMF: beyond the core-collapse model
Authors: Pelkonen V-M , Padoan P , Haugbølle T , Nordlund Å 
Published: March 2021

ABSTRACT
Observations have indicated that the pre-stellar core mass function (CMF) is similar to the stellar initial mass function (IMF), except for an offset towards larger masses. This has led to the idea that there is a one-to-one relation between cores and stars, such that the whole stellar mass reservoir is contained in a gravitationally bound pre-stellar core, as postulated by the core-collapse model, and assumed in recent theoretical models of the stellar IMF. We test the validity of this assumption by comparing the final mass of stars with the mass of their progenitor cores in a high-resolution star formation simulation that generates a realistic IMF under physical condition characteristic of observed molecular clouds. Using a definition of bound cores similar to previous works we obtain a CMF that converges with increasing numerical resolution. We find that the CMF and the IMF are closely related in a statistical sense only; for any individual star there is only a weak correlation between the progenitor core mass and the final stellar mass. In particular, for high-mass stars only a small fraction of the final stellar mass comes from the progenitor core, and even for low-mass stars the fraction is highly variable, with a median fraction of only about 50 per cent. We conclude that the core-collapse scenario and related models for the origin of the IMF are incomplete. We also show that competitive accretion is not a viable alternative.
Local stellar kinematics and Oort constants from the LAMOST A-type stars
Authors: Wang F , Zhang H-W , Huang Y , Chen B-Q , Wang H-F , Wang C 
Published: March 2021

ABSTRACT
We estimate the solar peculiar velocities and Oort constants using a sample of 5627 A-type stars with $d\lt 0.6\, \rm kpc$ and $|z|\lt 0.1\, \rm kpc$, selected from the LAMOST (Large Sky Area Multi-Object Fiber Spectroscopic Telescope) surveys. The radial and tangential velocities of these A-type stars are fitted by using a non-axisymmetric model. The best-fitting result yields the solar peculiar velocities $(U_\odot ,V_\odot ,W_\odot)=(11.69\pm 0.68, 10.16\pm 0.51, 7.67\pm 0.10)\, \rm km\, s^{-1}$ and Oort constants $A=16.31\pm 0.89\, \rm km\, s^{-1}\, kpc^{-1}$, $B=-11.99\pm 0.79\, \rm km\, s^{-1}\, kpc^{-1}$, $C=-3.10\pm 0.48\, \rm km\, s^{-1}\, kpc^{-1}$, and $K=-1.25\pm 1.04\, \rm km\, s^{-1}\, kpc^{-1}$. $|K+C|\gt 4\, \rm km\, s^{-1}\, kpc^{-1}$ means that there is a radial velocity gradient in the extended local disc, implying that the local disc is in a non-asymmetric potential. Using the derived Oort constants, we derive the local angular velocity $\Omega \, {\approx }\, A-B=28.30\pm 1.19\, \rm km\, s^{-1}\, kpc^{-1}$. By using A-type star sample of different volumes, we further try to evaluate the impacts of the ridge pattern in the R–Vϕ plane on constraining the solar motions and Oort constants. As the volume becomes larger towards the anticentre direction, the values of A and B become larger (implying a steeper slope of the local rotation curve) and the value of V⊙ becomes smaller probably caused by the ridge structure and its signal increasing with distance.
Quantified diffuse light in compact groups of galaxies
Authors: Poliakov Denis , Mosenkov Aleksandr V , Brosch Noah , Koriski Shuki , Rich R Michael 
Published: March 2021

ABSTRACT
The vast majority of stars in galaxy groups are contained within their constituent galaxies. Some small fraction of stars is expected, however, to follow the global dark matter (DM) potential of the group. In compact groups, interactions between the galaxies should be frequent. This leads to a more intensive material stripping from the group members, which finally forms an intra-group light component (IGL). Therefore, the distribution of the IGL should be related to the distribution of the total mass in the compact group and its dynamical status. In this study, we consider the distribution and fraction of the IGL in a sample of 36 Hickson compact groups (HCGs). We use deep observations of these compact groups (down to surface brightness ∼28 mag arcsec−2 in the r band) obtained with the WISE 28-in. telescope. For five HCGs with a bright symmetric IGL component, we carry out multicomponent photometric decomposition to simultaneously fit the galaxy profiles and the IGL. For the remaining groups, we only fit the profiles of their constituent galaxies. We find that the mean surface brightness of the IGL correlates with the mean morphology of the group: it becomes brighter in the groups with a larger fraction of early-type galaxies. On the other hand, the IGL brightness depends on the total luminosity of the group. The IGL profile tends to have a Sérsic index n ∼ 0.5−1, which is generally consistent with the mass density profile of DM haloes in compact groups obtained from cosmological simulations.
The effect of the streaming instability on protoplanetary disc emission at millimetre wavelengths
Authors: Scardoni Chiara E , Booth Richard A , Clarke Cathie J 
Published: March 2021

ABSTRACT
In this paper, we investigate whether overdensity formation via streaming instability is consistent with recent multiwavelength Atacama Large Millimeter Array (ALMA) observations in the Lupus star-forming region. We simulate the local action of streaming instability in 2D using the code athena, and examine the radiative properties at mm wavelengths of the resulting clumpy dust distribution by focusing on two observable quantities: the optically thick fraction ff (in ALMA band 6) and the spectral index α (in bands 3–7). By comparing the simulated distribution in the ff–α plane before and after the action of streaming instability, we observe that clump formation causes ff to drop, because of the suppression of emission from grains that end up in optically thick clumps. α, instead, can either increase or decline after the action of streaming instability; we use a simple toy model to demonstrate that this behaviour depends on the sizes of the grains whose emission is suppressed by being incorporated in optically thick clumps. In particular, the sign of evolution of α depends on whether grains near the opacity maximum at a few tenths of a mm end up in clumps. By comparing the simulation distributions before/after clump formation to the data distribution, we note that the action of streaming instability drives simulations towards the area of the plane where the data are located. We furthermore demonstrate that this behaviour is replicated in integrated disc models provided that the instability is operative over a region of the disc that contributes significantly to the total mm flux.
Exploring the contamination of the DES-Y1 cluster sample with SPT-SZ selected clusters
Authors: Grandis S , Mohr J J , Costanzi M , Saro A , Bocquet S , Klein M , Aguena M , Allam S , Annis J , Ansarinejad B , Bacon D , Bertin E , Bleem L , Brooks D , Burke D L , Carnero Rosel A , Carrasco Kind M , Carretero J , Castander F J , Choi A , da Costa L N , De Vincente J , Desai S , Diehl H T , Dietrich J P , Doel P , Eifler T F , Everett S , Ferrero I , Floyd B , Fosalba P , Frieman J , García-Bellido J , Gaztanaga E , Gruen D , Gruendl R A , Gschwend J , Gupta N , Gutierrez G , Hinton S R , Hollowood D L , Honscheid K , James D J , Jeltema T , Kuehn K , Lahav O , Lidman C , Lima M , Maia M A G , March M , Marshall J L , Melchior P , Menanteau F , Miquel R , Morgan R , Myles J , Ogando R , Palmese A , Paz-Chinchón F , Plazas A A , Reichardt C L , Romer A K , Sanchez E , Scarpine V , Serrano S , Sevilla-Noarbe I , Singh P , Smith M , Suchyta E , Swanson M E C , Tarle G , Thomas D , To C , Weller J , Wilkinson R D , Wu H 
Published: March 2021

ABSTRACT
We perform a cross validation of the cluster catalogue selected by the red-sequence Matched-filter Probabilistic Percolation algorithm (redMaPPer) in Dark Energy Survey year 1 (DES-Y1) data by matching it with the Sunyaev–Zel’dovich effect (SZE) selected cluster catalogue from the South Pole Telescope SPT-SZ survey. Of the 1005 redMaPPer selected clusters with measured richness $\hat{\lambda }\gt 40$ in the joint footprint, 207 are confirmed by SPT-SZ. Using the mass information from the SZE signal, we calibrate the richness–mass relation using a Bayesian cluster population model. We find a mass trend λ ∝ MB consistent with a linear relation (B ∼ 1), no significant redshift evolution and an intrinsic scatter in richness of σλ = 0.22 ± 0.06. By considering two error models, we explore the impact of projection effects on the richness–mass modelling, confirming that such effects are not detectable at the current level of systematic uncertainties. At low richness SPT-SZ confirms fewer redMaPPer clusters than expected. We interpret this richness dependent deficit in confirmed systems as due to the increased presence at low richness of low-mass objects not correctly accounted for by our richness-mass scatter model, which we call contaminants. At a richness $\hat{\lambda }=40$, this population makes up ${\gt}12{{\ \rm per\ cent}}$ (97.5 percentile) of the total population. Extrapolating this to a measured richness $\hat{\lambda }=20$ yields ${\gt}22{{\ \rm per\ cent}}$ (97.5 percentile). With these contamination fractions, the predicted redMaPPer number counts in different plausible cosmologies are compatible with the measured abundance. The presence of such a population is also a plausible explanation for the different mass trends (B ∼ 0.75) obtained from mass calibration using purely optically selected clusters. The mean mass from stacked weak lensing (WL) measurements suggests that these low-mass contaminants are galaxy groups with masses ∼3–5 × 1013 M⊙ which are beyond the sensitivity of current SZE and X-ray surveys but a natural target for SPT-3G and eROSITA.
Dynamical tides in neutron stars: the impact of the crust
Authors: Passamonti A , Andersson N , Pnigouras P 
Published: March 2021

ABSTRACT
We consider the dynamical tidal response of a neutron star in an inspiralling binary, focussing on the impact of the star’s elastic crust. Within the context of Newtonian gravity, we add the elastic aspects to the theoretical formulation of the problem and quantify the dynamical excitation of different classes of oscillation modes. The results demonstrate the expectation that the fundamental mode dominates the tidal response and show how the usual tidal deformability (and the Love number) emerge in the static limit. In addition, we consider to what extent the different modes may be excited to a level where the breaking strain of the crust would be exceeded (locally). The results show that the fundamental mode may fracture the crust during the late stages of inspiral. This is also the case for the first gravity mode, which reaches the breaking threshold in strongly stratified stars. In our models with a fluid ocean, interface modes associated with the crust-ocean transition may also induce crust fracture. If this happens, it does so earlier in the inspiral, at a lower orbital frequency.
Trends in the Socioeconomic Inequalities Related to Second-Hand Smoke Exposure as Verified by Urine Cotinine Levels Among Nonsmoking Adults: Korea National Health and Nutrition Examination Survey 2008–2018
Authors: Kang Seo Young , Lim Min Kyung , Cho Hong-Jun 
Published: March 2021

Abstract

Introduction
The expansion of smoke-free policies has reduced the prevalence of second-hand smoke (SHS) exposure; however, declines differ according to socioeconomic positions. We evaluated the trends in socioeconomic inequalities related to SHS exposure in nonsmoking Korean adults from 2008 to 2018.

Methods
We analyzed 30,027 nonsmoking adults from the Korea National Health and Nutrition Examination Survey 2008 to 2018. We evaluated trends in urine cotinine levels, self-reported prevalence of SHS exposure at workplaces and homes, and people exhibiting nonmeasurable urine cotinine levels between 2008 and 2018. To evaluate the yearly decline differences of urine cotinine levels according to socioeconomic positions, we calculated the interaction effects of year and education, household incomes, and occupation from linear regression analysis.

Results
In the last 11 years, the geometric means of urine cotinine levels decreased from 3.53 (95% CI 2.96–4.19) ng/mL to 0.60 (0.57–0.64) ng/mL in males, and from 2.36 (2.03–2.73) ng/mL to 0.53 (0.51–0.56) ng/mL in females. The prevalence of SHS exposure at workplaces and homes also declined. In the multivariate model, the interaction effects between education and years were significant; therefore, indicating a substantial yearly decline of urine cotinine levels in higher educated individuals. The interaction effects between household incomes and years were only significant among males; the interaction effects between occupations and years were not significant.

Conclusions
SHS exposure in nonsmoking Korean adults has consistently decreased; however, socioeconomic inequalities related to SHS exposure by education level have widened. Policies targeting socioeconomically disadvantaged populations should be implemented to decrease the disparities of SHS exposure.

Implications
Along with tobacco control policies, the prevalence of self-reported and urinary cotinine verified SHS exposure has decreased in the last 11 years. In contrast, the socioeconomic inequalities related to SHS exposure by education level have increased over time. This study emphasizes the need for implementing tobacco control policies to reduce disparities of SHS exposure.