bluuebunny/crossref_metadata_2025_split huggingface dataset:
Mothers' Attachment Style as a Predictor of Breastfeeding and Room-Sharing Practices
Authors: Jones Jason D , Beijers Roseriet , Fraley R Chris , Gross Jacquelyn T , Cassidy Jude , de Weerth Carolina 
Published: April 2020

AbstractObjectiveTo prospectively assess breastfeeding and room-sharing practices during the infant’s first 6 months and investigate whether mothers’ own adult attachment style predicts the initiation and course of these recommended parenting behaviors.MethodThis study included 193 mother–infant dyads living in the Netherlands. Diary methodology was used to generate 27 weekly measures of breastfeeding and room-sharing during the infant’s first 6 months. Multilevel mixed effects models were used to examine trajectories of breastfeeding and room-sharing and to test whether mothers’ own adult attachment style predicted the initiation and course of these behaviors, adjusting for covariates.ResultsMost (86%) mothers initiated breastfeeding immediately after birth and the rates of breastfeeding declined steadily over the 6 months (b = −2.47, SE = 0.19, p &lt; .001). Mothers with higher attachment avoidance showed faster decreases in breastfeeding than less avoidant mothers (b = −1.07, SE = 0.21, p &lt; .001). Sixty-four percent of mothers engaged in room-sharing after birth which also decreased steadily over the 6 months (b = −3.51, SE = 0.21, p &lt; .001). Mothers’ attachment style did not predict the initiation or course of room-sharing.ConclusionsGiven the major implications of breastfeeding and room-sharing for infants’ health, safety, and development, the pediatrics community has issued clear guidelines encouraging these behaviors. Yet many new parents do not adhere to the recommended practices. This study identifies mothers’ adult attachment style as a predictor of breastfeeding over time that could be incorporated into interventions for parents.
Belief, Rational and Justified
Authors: Siscoe Robert Weston 
Published: April 2020

AbstractIt is clear that beliefs can be assessed both as to their justification and as to their rationality. What is not as clear, however, is how the rationality and justification of belief relate to one another. Stewart Cohen has stumped for the popular proposal that rationality and justification come to the same thing, that rational beliefs just are justified beliefs, supporting his view by arguing that ‘justified belief’ and ‘rational belief’ are synonymous. In this paper, I will give reason to think that Cohen’s argument is spurious. I will show that ‘rational’ and ‘justified’ occupy two distinct semantic categories—‘rational’ is an absolute gradable adjective and ‘justified’ is a relative gradable adjective—telling against the thought that ‘rational belief’ and ‘justified belief’ are synonymous. I will then argue that the burden of proof is on those who would equate rationality and justification, making the case that those who hold this prominent position face the difficulty of explaining how rationality and justification come to the same thing even though ‘rational’ and ‘justified’ are not synonymous.
On the disc reflection spectroscopy of NS LMXB Serpens X-1: analysis of a recent NuSTAR observation
Authors: Mondal Aditya S , Dewangan G C , Raychaudhuri B 
Published: April 2020

ABSTRACT
We present NuSTAR observation of the atoll type neutron star (NS) low-mass X-ray binary (LMXB) Serpens X-1 (Ser X-1) performed on 2018 February 17. We observed Ser X-1 in a soft X-ray spectral state with 3–79 keV luminosity of LX ∼ 0.4 × 1038 erg s−1 (${\sim}23{{\ \rm per\ cent}}$ of the Eddington luminosity), assuming a distance of 7.7 kpc. A positive correlation between intensity and hardness ratio suggests that the source was in the banana branch during this observation. The broad-band 3–30 keV NuSTAR energy spectrum can be well described either by a three-component continuum model consisting of a disc blackbody, a single temperature blackbody, and a power law or by a two-component continuum model consisting of a disc blackbody and a Comptonization component. A broad iron line ∼5–8 keV and the Compton back-scattering hump peaking at ∼10–20 keV band are clearly detected in the X-ray spectrum. These features are best interpreted by a self-consistent relativistic reflection model. Fits with relativistically blurred disc reflection model suggests that the inner disc radius Rin is truncated prior to the ISCO at (1.9–2.5) RISCO (${\simeq}11.4\!-\!15\, R_{g}\: \text{or}\: 26\!-\!34$ km) and the accretion disc is viewed at a low inclination of i ≃ 16°−20°. The disc is likely to be truncated either by a boundary layer or by the magnetosphere. Based on the measured flux and the mass accretion rate, the maximum radial extension for the boundary layer is estimated to be ∼6.4 Rg from the NS surface. The truncated inner disc in association with pressure from a magnetic field sets an upper limit of B ≤ 1.9 × 109 G.
Galaxy pairs in the Sloan Digital Sky Survey – XIV. Galaxy mergers do not lie on the fundamental metallicity relation
Authors: Bustamante Sebastián , Ellison Sara L , Patton David R , Sparre Martin 
Published: April 2020

ABSTRACT
In recent observational studies, star-forming galaxies have been shown to follow a relation often dubbed the fundamental metallicity relation (FMR). This relation links the stellar mass of a galaxy with its star formation rate (SFR) and its gas-phase metallicity. Specifically, the FMR predicts that galaxies, at a given stellar mass, exhibit lower metallicities for higher SFRs. This trend is qualitatively consistent with observations of galaxy pairs, which have been robustly shown to experience increasing gas-phase metallicity dilution and enhanced star formation activity with decreasing projected separation. In this work, we show that, despite the qualitative consistency with FMR expectations, the observed O/H dilution in galaxy pairs of the Sloan Digital Sky Survey is stronger than what is predicted by the FMR. We conclude that the evolutionary phase of galaxies interacting with companions is not encoded in the FMR, and thus, mergers constitute a clearly defined population of outliers. We find that galaxies in pairs are consistent with the FMR only when their separation is larger than 110 kpc. Finally, we also quantify the local environment of the pairs using the number of galaxy neighbours within 2 Mpc, N2, and the projected separation to the second closest galaxy, r2. We find that pairs are more sensitive to a second companion than to the local galaxy density, displaying less elevated SFRs with smaller values of r2.
Predictions for measuring the 21-cm multifrequency angular power spectrum using SKA-Low
Authors: Mondal Rajesh , Shaw Abinash Kumar , Iliev Ilian T , Bharadwaj Somnath , Datta Kanan K , Majumdar Suman , Sarkar Anjan K , Dixon Keri L 
Published: April 2020

ABSTRACT
The light-cone effect causes the mean as well as the statistical properties of the redshifted 21-cm signal ${T_{\rm b}}(\hat{\boldsymbol {n}}, \nu)$ to change with frequency ν (or cosmic time). Consequently, the statistical homogeneity (ergodicity) of the signal along the line-of-sight (LoS) direction is broken. This is a severe problem particularly during the Epoch of Reionization (EoR) when the mean neutral hydrogen fraction ($\bar{x}_{\rm {H\,{\small I}}}$) changes rapidly as the Universe evolves. This will also pose complications for large bandwidth observations. These effects imply that the 3D power spectrum P(k) fails to quantify the entire second-order statistics of the signal as it assumes the signal to be ergodic and periodic along the LoS. As a proper alternative to P(k), we use the multifrequency angular power spectrum (MAPS) ${\mathcal {C}}_{\ell }(\nu _1,\nu _2)$, which does not assume the signal to be ergodic and periodic along the LoS. Here, we study the prospects for measuring the EoR 21-cm MAPS using future observations with the upcoming SKA-Low. Ignoring any contribution from the foregrounds, we find that the EoR 21-cm MAPS can be measured at a confidence level ≥5σ at angular scales ℓ ∼ 1300 for total observation time tobs ≥ 128 h across ∼44 MHz observational bandwidth. We also quantitatively address the effects of foregrounds on MAPS detectability forecast by avoiding signal contained within the foreground wedge in $({\boldsymbol {k}}_\perp , k_\parallel)$ plane. These results are very relevant for the upcoming large bandwidth EoR experiments as previous predictions were all restricted to individually analysing the signal over small frequency (or equivalent redshift) intervals.
From stellar haloes to intracluster light: the physics of the Intra-Halo Stellar Component in cosmological hydrodynamical simulations
Authors: Cañas Rodrigo , Lagos Claudia del P , Elahi Pascal J , Power Chris , Welker Charlotte , Dubois Yohan , Pichon Christophe 
Published: April 2020

ABSTRACT
We study the Intra-Halo Stellar Component (IHSC) of Milky Way-mass systems up to galaxy clusters in the Horizon-AGN cosmological hydrodynamical simulation. We identify the IHSC using an improved phase-space galaxy finder algorithm which provides an adaptive, physically motivated, and shape-independent definition of this stellar component, that can be applied to haloes of arbitrary masses. We explore the IHSC mass fraction – total halo’s stellar mass, $f_{M_{*,\mathrm{IHSC}}} - M_{*}$, relation, and the physical drivers of its scatter. We find that on average, the $f_{M_{*,\mathrm{IHSC}}}$ increases with total stellar mass, with the scatter decreasing strongly with mass from 2 dex at $M_{*,\mathrm{tot}}\simeq 10^{11}\, \mathrm{M}_\odot$ to 0.3 dex at group masses. At high masses, $M_{*,\mathrm{tot}}\gt 10^{11.5}\, \mathrm{M}_\odot$, $f_{M_{*,\mathrm{IHSC}}}$ increases with the number of substructures, and with the mass ratio between the central galaxy and largest satellite, at fixed M*, tot. From mid-size groups and systems below $M_{*,\mathrm{tot}}\lt 10^{12}\, \mathrm{M}_\odot$, we find that the central galaxy’s stellar rotation-to-dispersion velocity ratio, V/σ, displays the strongest (anti)-correlation with $f_{M_{*,\mathrm{IHSC}}}$ at fixed M*, tot of all the galaxy and halo properties explored, transitioning from $f_{M_{*,\mathrm{IHSC}}}\lt 0.1$ per cent for high V/σ, to $f_{M_{*,\mathrm{IHSC}}}\approx 5$ per cent for low V/σ galaxies. By studying the $f_{M_{*,\mathrm{IHSC}}}$ temporal evolution, we find that, in the former, mergers not always take place, but if they did, they happened early (z &gt; 1), while the high $f_{M_{*,\mathrm{IHSC}}}$ population displays a much more active merger history. In the case of massive groups and galaxy clusters, $M_{*,\mathrm{tot}}\gtrsim 10^{12}\, \mathrm{M}_\odot$, a fraction $f_{M_{*,\mathrm{IHSC}}}\approx 10-20$ per cent is reached at z ≈ 1 and then they evolve across lines of constant $f_{M_{*,\mathrm{IHSC}}}$ modulo some small perturbations. Because of the limited simulation’s volume, the latter is only tentative and requires a larger sample of simulated galaxy clusters to confirm.
Multiwavelength cross-correlation analysis of the simulated cosmic web
Authors: Gheller C , Vazza F 
Published: April 2020

ABSTRACTWe used magnetohydrodynamical cosmological simulations to investigate the cross-correlation between different observables (i.e. X-ray emission, Sunyaev–Zeldovich (SZ) signal at 21 cm, H i temperature decrement, diffuse synchrotron emission, and Faraday Rotation) as a probe of the diffuse matter distribution in the cosmic web. We adopt a uniform and simplistic approach to produce synthetic observations at various wavelengths, and we compare the detection chances of different combinations of observables correlated with each other and with the underlying galaxy distribution in the volume. With presently available surveys of galaxies and existing instruments, the best chances to detect the diffuse gas in the cosmic web outside of haloes is by cross-correlating the distribution of galaxies with SZ observations. We also find that the cross-correlation between the galaxy network and the radio emission or the Faraday Rotation can already be used to limit the amplitude of extragalactic magnetic fields, well outside of the cluster volume usually explored by existing radio observations, and to probe the origin of cosmic magnetism with the future generation of radio surveys.
Polar planets around highly eccentric binaries are the most stable
Authors: Chen Cheng , Lubow Stephen H , Martin Rebecca G 
Published: April 2020

ABSTRACT
We study the orbital stability of a non-zero mass, close-in circular orbit planet around an eccentric orbit binary for various initial values of the binary eccentricity, binary mass fraction, planet mass, planet semimajor axis, and planet inclination by means of numerical simulations that cover 5 × 104 binary orbits. For small binary eccentricity, the stable orbits that extend closest to the binary (most stable orbits) are nearly retrograde and circulating. For high binary eccentricity, the most stable orbits are highly inclined and librate near the so-called generalized polar orbit which is a stationary orbit that is fixed in the frame of the binary orbit. For more extreme mass ratio binaries, there is a greater variation in the size of the stability region (defined by initial orbital radius and inclination) with planet mass and initial inclination, especially for low binary eccentricity. For low binary eccentricity, inclined planet orbits may be unstable even at large orbital radii (separation ${\gt}5 \, a_{\rm b}$). The escape time for an unstable planet is generally shorter around an equal mass binary compared with an unequal mass binary. Our results have implications for circumbinary planet formation and evolution and will be helpful for understanding future circumbinary planet observations.
Evolution of planar magnetic structure within the stream interaction region and its connection with a recurrent Forbush decrease
Authors: Shaikh Zubair I , Raghav Anil N , Vichare Geeta 
Published: April 2020

ABSTRACT
In general, stream interaction region (SIR)-induced Forbush decreases are recurrent and low magnitude in nature. The diffusion–convection associated with the SIR plays an important role in their modulation. Here, we study the evolution of planar magnetic structure (PMS) within the SIR and its contribution to cosmic ray modulation. Interestingly, we found the presence of PMS structures within the SIR from the leading part of the SIR to the minimum of the cosmic ray intensity in two events. The PMS may have originated due to the high compression caused by the fast solar wind, which amplifies and aligns the pre-existing discontinuities in the ambient slow solar wind. The study also suggests that the existence of PMS, enhanced initial mass function (IMF) strength, and associated turbulent regions decreases the perpendicular diffusion coefficient and causes a decrease in the cosmic ray intensity observed on Earth. Moreover, a slow decrease in IMF magnitude concurs with the recovery phase of cosmic ray intensity.
PRMT7 regulates RNA-binding capacity and protein stability in Leishmania parasites
Authors: Ferreira Tiago R , Dowle Adam A , Parry Ewan , Alves-Ferreira Eliza V C , Hogg Karen , Kolokousi Foteini , Larson Tony R , Plevin Michael J , Cruz Angela K , Walrad Pegine B 
Published: April 2020

Abstract
RNA binding proteins (RBPs) are the primary gene regulators in kinetoplastids as transcriptional control is nearly absent, making Leishmania an exceptional model for investigating methylation of non-histone substrates. Arginine methylation is an evolutionarily conserved protein modification catalyzed by Protein aRginine Methyl Transferases (PRMTs). The chromatin modifier PRMT7 is the only Type III PRMT found in higher eukaryotes and a restricted number of unicellular eukaryotes. In Leishmania major, PRMT7 is a cytoplasmic protein implicit in pathogenesis with unknown substrates. Using comparative methyl-SILAC proteomics for the first time in protozoa, we identified 40 putative targets, including 17 RBPs hypomethylated upon PRMT7 knockout. PRMT7 can modify Alba3 and RBP16 trans-regulators (mammalian RPP25 and YBX2 homologs, respectively) as direct substrates in vitro. The absence of PRMT7 levels in vivo selectively reduces Alba3 mRNA-binding capacity to specific target transcripts and can impact the relative stability of RBP16 in the cytoplasm. RNA immunoprecipitation analyses demonstrate PRMT7-dependent methylation promotes Alba3 association with select target transcripts and thus indirectly stabilizes mRNA of a known virulence factor, δ-amastin surface antigen. These results highlight a novel role for PRMT7-mediated arginine methylation of RBP substrates, suggesting a regulatory pathway controlling gene expression and virulence in Leishmania. This work introduces Leishmania PRMTs as epigenetic regulators of mRNA metabolism with mechanistic insight into the functional manipulation of RBPs by methylation.
Phage T7 DNA mimic protein Ocr is a potent inhibitor of BREX defence
Authors: Isaev Artem , Drobiazko Alena , Sierro Nicolas , Gordeeva Julia , Yosef Ido , Qimron Udi , Ivanov Nikolai V , Severinov Konstantin 
Published: April 2020

Abstract
BREX (for BacteRiophage EXclusion) is a superfamily of common bacterial and archaeal defence systems active against diverse bacteriophages. While the mechanism of BREX defence is currently unknown, self versus non-self differentiation requires methylation of specific asymmetric sites in host DNA by BrxX (PglX) methyltransferase. Here, we report that T7 bacteriophage Ocr, a DNA mimic protein that protects the phage from the defensive action of type I restriction–modification systems, is also active against BREX. In contrast to the wild–type phage, which is resistant to BREX defence, T7 lacking Ocr is strongly inhibited by BREX, and its ability to overcome the defence could be complemented by Ocr provided in trans. We further show that Ocr physically associates with BrxX methyltransferase. Although BREX+ cells overproducing Ocr have partially methylated BREX sites, their viability is unaffected. The result suggests that, similar to its action against type I R–M systems, Ocr associates with as yet unidentified BREX system complexes containing BrxX and neutralizes their ability to both methylate and exclude incoming phage DNA.
QEMSCAN as a Method of Semi-Automated Crystal Size Distribution Analysis: Insights from Apollo 15 Mare Basalts
Authors: Bell S K , Joy K H , Pernet-Fisher J F , Hartley M E 
Published: April 2020

Abstract
Crystal size distribution analysis is a non-destructive, quantitative method providing insights into the crystallization histories of magmas. Traditional crystal size distribution data collection requires the manual tracing of crystal boundaries within a sample from a digital image. Although this manual method requires minimal equipment to perform, the process is often time-intensive. In this study we investigate the feasibility of using the Quantitative Evaluation of Minerals by SCANing electron microscopy (QEMSCAN) software for semi-automated crystal size distribution analysis. Four Apollo 15 mare basalt thin sections were analysed using both manual and QEMSCAN crystal size distribution data collection methods. In most cases we observe an offset between the crystal size distribution plots produced by QEMSCAN methods compared with the manual data, leading to differences in calculated crystal residence times and nucleation densities. The source of the discrepancy is two-fold: (1) the touching particles processor in the QEMSCAN software is prone to segmenting overlapping elongate crystals into multiple smaller crystals; (2) this segmentation of elongate crystals causes estimates of true 3D crystal habit to vary between QEMSCAN and manual data. The reliability of the QESMCAN data appears to be a function of the crystal texture and average crystal shape, both of which influence the performance of the touching particles processor. Despite these limitations, QEMSCAN is able to produce broadly similar overall trends in crystal size distribution plots to the manual approach, in a considerably shorter time frame. If an accurate crystal size distribution is required to calculate crystal residence time or nucleation density, we recommend that QEMSCAN should only be used after careful consideration of the suitability of the sample texture and average crystal shape.
Measurement Properties of the Craniocervical Flexion Test: A Systematic Review
Authors: Araujo Francisco Xavier de , Ferreira Giovanni E , Scholl Schell Maurício , Castro Marcelo Peduzzi de , Ribeiro Daniel Cury , Silva Marcelo Faria 
Published: April 2020

Abstract

Objective
Patients with neck pain commonly have altered activity of the neck muscles. The craniocervical flexion test (CCFT) is used to assess the function of the deep neck flexor muscles in patients with musculoskeletal neck disorders. Systematic reviews summarizing the measurement properties of the CCFT are outdated. The objective of this study was to systematically review the measurement properties of the CCFT for assessing the deep neck flexor muscles.

Methods
The data sources MEDLINE, EMBASE, Physiotherapy Evidence Database, Cochrane Central Register of Controlled Trials, Scopus, and Science Direct were searched in April 2019. Studies of any design that reported at least 1 measurement property of the CCFT for assessing the deep neck flexor muscles were selected. Two reviewers independently extracted data and rated the risk of bias of individual studies using the COnsensus-based Standards for the selection of health Measurement INstruments (COSMIN) risk-of-bias checklist. The overall rating for each measurement property was classified as “positive,” “indeterminate,” or “negative.” The overall rating was accompanied with a level of evidence.

Results
Fourteen studies were included in the data synthesis. The ratings were positive, and the level of evidence was moderate for interrater and intrarater reliability and convergent validity. There was conflicting rating and level of evidence for discriminative validity. Measurement error was indeterminate, with an unknown level of evidence. Responsiveness was negative, with a limited level of evidence. A limitation of this study was that only papers published in English were included.

Conclusions
The CCFT is a valid and reliable test that can be used in clinical practice as an assessment test. Because of the conflicting and low-quality evidence, caution is advised when using the CCFT as a discriminative test and as an outcome measure. Future better-designed studies are warranted.