bluuebunny/crossref_metadata_2025_split huggingface dataset:
A copia-like retrotransposon insertion in the upstream region of the SHATTERPROOF1 gene, BnSHP1.A9, is associated with quantitative variation in pod shattering resistance in oilseed rape
Authors: Liu Jia , Zhou Rijin , Wang Wenxiang , Wang Hui , Qiu Yu , Raman Rosy , Mei Desheng , Raman Harsh , Hu Qiong 
Published: June 2020

AbstractSeed loss resulting from pod shattering is a major constraint in production of oilseed rape (Brassica napus L.). However, the molecular mechanisms underlying pod shatter resistance are not well understood. Here, we show that the pod shatter resistance at quantitative trait locus qSRI.A9.1 is controlled by one of the B. napus SHATTERPROOF1 homologs, BnSHP1.A9, in a doubled haploid population generated from parents designated R1 and R2 as well as in a diverse panel of oilseed rape. The R1 maternal parental line of the doubled haploid population carried the allele for shattering at qSRI.A9.1, while the R2 parental line carried the allele for shattering resistance. Quantitative RT-PCR showed that BnSHP1.A9 was expressed specifically in flower buds, flowers, and developing siliques in R1, while it was not expressed in any tissue of R2. Transgenic plants constitutively expressing either of the BnSHP1.A9 alleles from the R1 and R2 parental lines showed that both alleles are responsible for pod shattering, via a mechanism that promotes lignification of the enb layer. These findings indicated that the allelic differences in the BnSHP1.A9 gene per se are not the causal factor for quantitative variation in shattering resistance at qSRI.A9.1. Instead, a highly methylated copia-like long terminal repeat retrotransposon insertion (4803 bp) in the promotor region of the R2 allele of BnSHP1.A9 repressed the expression of BnSHP1.A9, and thus contributed to pod shatter resistance. Finally, we showed a copia-like retrotransposon-based marker, BnSHP1.A9R2, can be used for marker-assisted breeding targeting the pod shatter resistance trait in oilseed rape.
Overexpression of the manganese/cadmium transporter OsNRAMP5 reduces cadmium accumulation in rice grain
Authors: Chang Jia-Dong , Huang Sheng , Konishi Noriyuki , Wang Peng , Chen Jie , Huang Xin-Yuan , Ma Jian Feng , Zhao Fang-Jie 
Published: June 2020

Abstract
Rice is a major dietary source of the toxic metal cadmium (Cd), and reducing its accumulation in the grain is therefore important for food safety. We selected two cultivars with contrasting Cd accumulation and generated transgenic lines overexpressing OsNRAMP5, which encodes a major influx transporter for manganese (Mn) and Cd. We used two different promoters to control the expression, namely OsActin1 and maize Ubiquitin. Overexpression of OsNRAMP5 increased Cd and Mn uptake into the roots, but markedly decreased Cd accumulation in the shoots, whilst having a relatively small effect on Mn accumulation in the shoots. The overexpressed OsNRAMP5 protein was localized to the plasma membrane of all cell types in the root tips and lateral root primordia without polarity. Synchrotron X-ray fluorescence mapping showed that the overexpression lines accumulated more Cd in the root tips and lateral root primordia compared with the wild-type. When grown in three Cd-contaminated paddy soils, overexpression of OsNRAMP5 decreased concentration of Cd in the grain by 49–94% compared with the wild type. OsNRAMP5-overexpression plants had decreased Cd translocation from roots to shoots as a result of disruption of its radial transport into the stele for xylem loading, demonstrating the effect of transporter localization and polarity on ion homeostasis.
Evolution of fractality and rotation in embedded star clusters
Authors: Ballone Alessandro , Mapelli Michela , Di Carlo Ugo N , Torniamenti Stefano , Spera Mario , Rastello Sara 
Published: June 2020

ABSTRACT
More and more observations indicate that young star clusters could retain imprints of their formation process. In particular, the degree of substructuring and rotation are possibly the direct result of the collapse of the parent molecular cloud from which these systems form. Such properties can, in principle, be washed-out, but they are also expected to have an impact on the relaxation of these systems. We ran and analysed a set of 10 hydrodynamical simulations of the formation of embedded star clusters through the collapse of turbulent massive molecular clouds. We systematically studied the fractality of our star clusters, showing that they are all extremely substructured (fractal dimension D = 1.0–1.8). We also found that fractality is slowly reduced, with time, on small scales, while it persists on large scales on longer time-scales. Signatures of rotation are found in different simulations at every time of the evolution, even for slightly supervirial substructures, proving that the parent molecular gas transfers part of its angular momentum to the new stellar systems.
A radio continuum and polarization study of the pulsar wind nebula CTB 87 (G74.9+1.2)
Authors: Kothes R , Reich W , Safi-Harb S , Guest B , Reich P , Fürst E 
Published: June 2020

ABSTRACT
We present radio continuum and linear polarization observations of the pulsar wind nebula (PWN) CTB 87 (G74.9+1.2) with the Effelsberg 100-m Radio Telescope between 4.75 and 32 GHz. An analysis of these new data including archived low-frequency observations at 1420 and 408 MHz from the Canadian Galactic Plane Survey shows that CTB 87 consists of two distinct emission components: a compact kidney-shaped component, 14 × 8.5 pc2 (7.8 × 4.8 arcmin2) in size and a larger diffuse, spherical, and centrally peaked component of about 30 pc (17 arcmin) in diameter. The kidney-shaped component with a much steeper radio continuum spectrum is highly linearly polarized and likely represents a relic PWN. The diffuse component represents the undisturbed part of the PWN expanding inside a cavity or stellar wind bubble. The previously reported spectral break above 10 GHz is likely the result of missing large-scale emission and insufficient sensitivity of the high-frequency radio continuum observations. The simulation of the system’s evolution yields an age of about 18 000 yr as the result of a Type II supernova explosion with ejecta mass of about 12 M⊙ and explosion energy of about 7 × 1050 erg. We also found evidence for a radio shell in our polarization data that represents the blast wave that entered the molecular cloud complex at a radius of about 13 pc.
Assessing the photometric redshift precision of the S-PLUS survey: the Stripe-82 as a test-case
Authors: Molino A , Costa-Duarte M V , Sampedro L , Herpich F R , Sodré L , Mendes de Oliveira C , Schoenell W , Barbosa C E , Queiroz C , Lima E V R , Azanha L , Muñoz-Elgueta N , Ribeiro T , Kanaan A , Hernandez-Jimenez J A , Cortesi A , Akras S , Lopes de Oliveira R , Torres-Flores S , Lima-Dias C , Castellon J L Nilo , Damke G , Alvarez-Candal A , Jiménez-Teja Y , Coelho P , Pereira E , Montero-Dorta A D , Benítez N , Gonçalves T S , Santana-Silva L , Werner S V , Almeida L A , Lopes P A A , Chies-Santos A L , Telles E , de Souza Thom , C R , Gonçalves D R , de Souza R S , Makler M , Buzzo M L , Placco V M , Nakazono L M I , Saito R K , Overzier R A , Abramo L R 
Published: June 2020

ABSTRACT
In this paper we present a thorough discussion about the photometric redshift (photo-z) performance of the Southern Photometric Local Universe Survey (S-PLUS). This survey combines a seven narrow +5 broad passband filter system, with a typical photometric-depth of r ∼ 21 AB. For this exercise, we utilize the Data Release 1 (DR1), corresponding to 336 deg2 from the Stripe-82 region. We rely on the BPZ2 code to compute our estimates, using a new library of SED models, which includes additional templates for quiescent galaxies. When compared to a spectroscopic redshift control sample of ∼100 k galaxies, we find a precision of σz &lt;0.8 per cent, &lt;2.0 per cent, or &lt;3.0 per cent for galaxies with magnitudes r &lt; 17, &lt;19, and &lt;21, respectively. A precision of 0.6 per cent is attained for galaxies with the highest Odds values. These estimates have a negligible bias and a fraction of catastrophic outliers inferior to 1 per cent. We identify a redshift window (i.e. 0.26 &lt; z &lt; 0.32) where our estimates double their precision, due to the simultaneous detection of two emission lines in two distinct narrow bands; representing a window opportunity to conduct statistical studies such as luminosity functions. We forecast a total of ∼2 M, ∼16 M and ∼32 M galaxies in the S-PLUS survey with a photo-z precision of σz &lt;1.0 per cent, &lt;2.0 per cent, and &lt;2.5 per cent after observing 8000 deg2. We also derive redshift probability density functions, proving their reliability encoding redshift uncertainties and their potential recovering the n(z) of galaxies at z &lt; 0.4, with an unprecedented precision for a photometric survey in the Southern hemisphere.
The manifestation of secondary bias on the galaxy population from IllustrisTNG300
Authors: Montero-Dorta Antonio D , Artale M Celeste , Abramo L Raul , Tucci Beatriz , Padilla Nelson , Sato-Polito Gabriela , Lacerna Ivan , Rodriguez Facundo , Angulo Raul E 
Published: June 2020

ABSTRACT
We use the improved IllustrisTNG300 magnetohydrodynamical cosmological simulation to revisit the effect that secondary halo bias has on the clustering of the central galaxy population. With a side length of 205 h−1 Mpc and significant improvements on the subgrid model with respect to previous Illustris simulations, IllustrisTNG300 allows us to explore the dependencies of galaxy clustering over a large cosmological volume and halo mass range. We show at high statistical significance that the halo assembly bias signal (i.e. the secondary dependence of halo bias on halo formation redshift) manifests itself on the clustering of the galaxy population when this is split by stellar mass, colour, specific star formation rate, and surface density. A significant signal is also found for galaxy size: at fixed halo mass, larger galaxies are more tightly clustered than smaller galaxies. This effect, in contrast to the rest of the dependencies, seems to be uncorrelated with halo formation time, with some small correlation only detected for halo spin. We also explore the transmission of the spin bias signal, i.e. the secondary dependence of halo bias on halo spin. Although galaxy spin retains little information about the total halo spin, the correlation is enough to produce a significant galaxy spin bias signal. We discuss possible ways to probe this effect with observations.
A thirty-four billion solar mass black hole in SMSS J2157–3602, the most luminous known quasar
Authors: Onken Christopher A , Bian Fuyan , Fan Xiaohui , Wang Feige , Wolf Christian , Yang Jinyi 
Published: June 2020

ABSTRACT
From near-infrared spectroscopic measurements of the Mg ii emission line doublet, we estimate the black hole (BH) mass of the quasar, SMSS J215728.21–360215.1, as being (3.4 ± 0.6) × 1010 M⊙ and refine the redshift of the quasar to be z = 4.692. SMSS J2157 is the most luminous known quasar, with a 3000 Å luminosity of (4.7 ± 0.5) × 1047 erg s−1 and an estimated bolometric luminosity of 1.6 × 1048 erg s−1, yet its Eddington ratio is only ∼0.4. Thus, the high luminosity of this quasar is a consequence of its extremely large BH – one of the most massive BHs at z &gt; 4.
Testing MOdified Gravity (MOG) theory and dark matter model in Milky Way using the local observables
Authors: Davari Zahra , Rahvar Sohrab 
Published: June 2020

ABSTRACT
In this paper, we have investigated one of the alternative theories to dark matter named MOdified Gravity (MOG) by testing its ability to describe the local dynamics of the Milky Way (MW) in vertical and transverse directions with the baryonic matter. MOG is designed to interpret the dynamics of galaxies and cluster of galaxies without the need for dark matter. We use local observational data such as the vertical dispersion, rotation curve, surface density, and number density of stars in the Milky Way to obtain the parameters of MOG and the baryonic component of MW by implementing a Bayesian approach to the parameter estimation based on a Markov Chain Monte Carlo method. We compare our results with the dark matter model of MW. The two models of MOG and cold dark matter are able to describe equally well the rotation curve and the vertical dynamics of stars in the local MW. The best values for the free parameters of MOG in this analysis are obtained as α = 8.99 ± 0.02 and μ = 0.054 ± 0.005 kpc−1. Also, we obtain the parameters of the generalized gNFW model in the dark matter model. Our best value of bulge mass from MOG is $(1.06 \pm 0.26)\times 10^{10}\, \rm M_{\odot }$, which is consistent with the estimations form the microlensing observations.
The fate of disc galaxies in IllustrisTNG clusters
Authors: Joshi Gandhali D , Pillepich Annalisa , Nelson Dylan , Marinacci Federico , Springel Volker , Rodriguez-Gomez Vicente , Vogelsberger Mark , Hernquist Lars 
Published: June 2020

ABSTRACTWe study the stellar morphological evolution of disc galaxies within clusters in the TNG50 and TNG100 runs from the IllustrisTNG simulation suite. We select satellites of masses 109.7 ≤ M*, z = 0/M⊙ ≤ 1011.6 residing in clusters of masses 1014 ≲ M200c, z = 0/M⊙ ≤ 1014.6 at z = 0 and that were discs at accretion according to a kinematic morphology indicator (the circularity fraction). These are traced from the time of accretion to z = 0 and compared to a control sample of central galaxies mass-matched at accretion. Most cluster discs become non-discy by z = 0, in stark contrast with the control discs, of which a significant fraction remains discy over the same timescales. Cluster discs become non-discy accompanied by gas removal and star formation quenching, loss of dark matter, and little growth or a loss of stellar mass. In contrast, control discs transform while also losing gas mass and quenching, but growing significantly in dark matter and stellar mass. Most cluster satellites change morphologies on similar timescales regardless of stellar mass, in ∼0.5–4 Gyr after accretion. Cluster discs that experienced more numerous and closer pericentric passages show the largest change in morphology. Morphological change in all cases requires the presence of a gravitational perturbation to drive stellar orbits to non-discy configurations, along with gas removal/heating to prevent replenishment of the disc through continued star formation. For cluster discs, the perturbation is impulsive tidal shocking at pericentres and not tidal stripping of outer disc stellar material, whereas for control discs, a combination of mergers and feedback from active galactic nuclei appears to be the key driving force behind morphological transformations.
Imprint of local environment on fast radio burst observations
Authors: Lu Wenbin , Phinney E Sterl 
Published: June 2020

ABSTRACT
When fast radio burst (FRB) waves propagate through the local (${\lesssim}\rm 1\, pc$) environment of the FRB source, electrons in the plasma undergo large-amplitude oscillations. The finite-amplitude effects cause the effective plasma frequency and cyclotron frequency to be dependent on the wave strength. The dispersion measure and rotation measure should therefore vary slightly from burst to burst for a repeating source, depending on the luminosity and frequency of the individual burst. Furthermore, free–free absorption of strong waves is suppressed due to the accelerated electrons’ reduced energy exchange in Coulomb collisions. This allows bright low-frequency bursts to propagate through an environment that would be optically thick to low-amplitude waves. Given a large sample of bursts from a repeating source, it would be possible to use the deficit of low-frequency and low-luminosity bursts to infer the emission measure of the local intervening plasma and its distance from the source. Information about the local environment will shed light on the nature of FRB sources.
Smoking Assessment and Current Smoking Status Among Adolescents in Primary Care Settings
Authors: Bailey Steffani R , Fankhauser Katie , Marino Miguel , Schmidt Teresa , Giebultowicz Sophia , Ezekiel-Herrera David , Heintzman John 
Published: June 2020

Abstract

Introduction
Initiating tobacco use in adolescence increases the risk of nicotine dependence and continued use into adulthood. Primary care visits provide opportunities for the assessment and treatment of tobacco use; however, little is known about prevalence and correlates of assessing smoking status and current use among adolescents in these settings.

Aims and Methods
Using electronic health record data from the OCHIN network, we identified adolescents with greater than or equal to one primary care visit to a study clinic (n = 366 clinics from 15 US states) during January 1, 2016 to December 31, 2017. We estimated odds ratios of smoking assessment and current smoking status by patient covariates.

Results
Of 140 887 patients, 87.4% were assessed for smoking. Being Latino or Black (adjusted odds ratio = 1.22, 95% confidence interval: 1.13–1.32; adjusted odds ratio = 1.17, 95% confidence interval: 1.07–1.29, respectively, vs. non-Hispanic White), publicly insured, having more visits, and having an asthma diagnosis or other respiratory symptoms were associated with higher odds of assessment. Odds were lower if the patient was male and uninsured. Of those assessed, 1.6% identified as current smokers. Being older, having more visits, an asthma diagnosis, other respiratory symptoms, and lower household income was associated with higher odds of being a current smoker. Latinos and Blacks had lower odds than non-Hispanic Whites.

Conclusions
Although some commonly reported tobacco-related disparities were not present, smoking assessment and current smoking status differed significantly by most patient demographics. Implementation of adolescent tobacco assessment protocols and the development of interventions to target subpopulations of adolescents with higher rates of smoking could mitigate disparate rates of assessment and smoking, respectively.

Implications
Clinical guidelines recommend screening adolescents for tobacco use in primary care settings. We found that most adolescents seen in US safety-net primary care clinics were assessed for smoking. We also found that smoking assessment and current smoking status differed significantly by most patient demographics. Implementing tobacco assessment protocols specific to adolescents could mitigate disparate rates of assessment and ensure accurate documentation of all forms of tobacco use, given the evolution of alternative tobacco products and poly use among adolescents. Interventions to target subpopulations of adolescents with higher smoking rates are needed to prevent the negative health effects of continued smoking.
Basic concepts and unique features of human circadian rhythms: implications for human health
Authors: Yamanaka Yujiro 
Published: June 2020

Abstract
Most physiological functions and behaviors exhibit a robust approximately 24-hour rhythmicity (circadian rhythm) in the real world. These rhythms persist under constant conditions, but the period is slightly longer than 24 hours, suggesting that circadian rhythms are endogenously driven by an internal, self-sustained oscillator. In mammals, including humans, the central circadian pacemaker is located in the hypothalamic suprachiasmatic nucleus. The primary zeitgeber for this pacemaker is bright sunlight, but nonphotic time cues also affect circadian rhythms. The human circadian system uniquely exhibits spontaneous internal desynchronization between the sleep-wake cycle and core body temperature rhythm under constant conditions and partial entrainment of the sleep-wake cycle in response to nonphotic time cues. Experimental and clinical studies of human circadian rhythms must take into account these unique features. This review covers the basic concepts and unique features of the human circadian system, the mechanisms underlying phase adjustment of the circadian rhythms by light and nonphotic time cues (eg, physical exercise), and the effects of eating behavior (eg, chewing frequency) on the circadian rhythm of glucose metabolism.
Chronic Primary Headache Subjects Have Greater Forward Head Posture than Asymptomatic and Episodic Primary Headache Sufferers: Systematic Review and Meta-analysis
Authors: Elizagaray-Garcia Ignacio , Beltran-Alacreu Hector , Angulo-Díaz Santiago , Garrigós-Pedrón Miriam , Gil-Martínez Alfonso 
Published: June 2020

AbstractObjectiveTo summarize the cervical physical examination characteristics in subjects with chronic primary headache and compare those with a healthy population and a population with episodic primary headache.DesignSystematic review and meta-analysis.SubjectsHumans ≥18 years old. At least one of the study groups should be constituted by subjects diagnosed with one of the chronic primary headache subtypes according to the International Classification of Headache Disorders, 3rd Edition.ComparisonNeck physical examination outcomes of subjects with chronic primary headache compared with a healthy population or subjects with episodic primary headache.OutcomesForward head posture (FHP), cervical range of movement, motor control, neck muscle activity, and reproduction and resolution of symptoms.MethodsTwo reviewers assessed independently the MEDLINE, EMBASE, WOS, MEDES, PEDro, and CINAHL databases to select observational studies. First, both implemented an agreement for a search strategy. Then, they screened independently for duplicates, titles, abstracts, and full-text information. A meta-analysis was conducted to compare measures between groups.ResultsTwelve studies (N = 1,083) with moderate quality (mean ± SD = 7.75 ± 1.48 on the Newcastle Ottawa Scale) were selected for the qualitative analysis. The meta-analysis showed that patients with chronic primary headache presented greater forward head posture than asymptomatic participants (N = 275, Hg = 0.68, 95% CI = 0.25–1.1, Z = 3.14, P &lt; 0.01) and patients with episodic primary headache (N = 268, Hg = 0.39, 95% CI = 0.13–0.65, Z = 2.98, P &lt; 0.01).ConclusionsThere is moderate to strong evidence that patients with chronic primary headache present greater FHP than asymptomatic individuals and moderate evidence that patients with chronic primary headache present greater forward head posture than those with episodic primary headache.
Ideological Bubbles and Two Types of Conservatives
Authors: Schildkraut Deborah J , Berry Jeffrey M , Glaser James M 
Published: June 2020

Abstract
For several years, and through different administrations, surveys have shown that self-identified liberals are more likely than self-identified conservatives to avoid interactions with and exposure to ideological disagreement. In this study, we demonstrate that this ideological asymmetry in outgroup avoidance can be partially explained by the well-established tendency of self-identified conservatives to hold moderate or liberal policy preferences. Using a nationally representative survey, we show that ideologically consistent conservatives look more like liberals (almost all of whom are ideologically consistent) in their tendency to engage in behaviors that promote ideologically homogeneous social networks. Inconsistent conservatives, on the other hand, are more likely to have ideologically heterogeneous social networks, making them less likely to clash with those on the other side and thus less likely to retreat from engagement, even if they hold conservative identities. This set of findings offers insight into the contours of polarization in contemporary America.