bluuebunny/crossref_metadata_2025_split huggingface dataset:
177Physical functional limitations and psychological distress in people with and without colorectal cancer
Authors: Zhang Yuehan 
Published: September 2021

Abstract

Background
This study aims to quantify physical disability and psychological distress in people with and without colorectal cancer (CRC).

Methods
Questionnaire data (2006-2009) from 267,153 Australian general population members aged ≥45 years participating in the 45 and Up Study (n = 213,231 following exclusions) were linked to cancer registry and hospital admission data, to ascertain CRC status. Modified Poisson regression estimated adjusted prevalence ratios (PRs) for physical disability and psychological distress in participants with versus without CRC.

Results
Compared with participants without CRC (n = 210,836), CRC survivors (n = 2,395) had significantly higher disability prevalence (11.9% versus 19.5%, respectively): PR = 1.11 (95%CI=1.03-1.20); and a similar prevalence of distress (23.1% versus 20.2%): PR = 1.03 (0.94-1.20). Adverse outcomes were associated with certain clinical characteristics. Compared to participants without CRC, CRC survivors diagnosed 5-&lt;10 and ≥10 years, with regional spread and without recent cancer treatment had similar outcomes; survivors with metastatic CRC and recent treatment had 30-60% higher prevalence of disability and distress. Compared to participants with neither CRC nor disability, PRs for distress were 4.71 (4.22-5.26) for those with disability and CRC and 4.22 (4.13-4.31) for those with disability without CRC.

Conclusions
Physical disability is elevated in CRC survivors. Psychological distress is elevated 4- to 5-fold with disability, regardless of CRC diagnosis, with lesser increases around diagnosis and treatment.

Key message
CRC survivors with less advanced disease and who have not been recently diagnosed or treated have physical disability and psychological distress comparable to the general population. Survivors with disability are at particularly high risk of distress.
586Effects of maternal circulating amino acids on offspring birthweight: a Mendelian randomisation analysis
Authors: Zhao Jian , Freathy Rachel , Evans David , Warrington Nicole , Langenberg Claudia , Stewart Isobel , Lotta Luca , Pietzner Maik , Borges Maria Carolina , Lawlor Deborah 
Published: September 2021

Abstract

Background
It is suggested amino acids are critical for fetal growth, but analyses assessing causality are lacking. Mendelian randomisation (MR) can be used to examine causal effects under instrumental variable (IV) assumptions.

Methods
We conducted a two-sample MR study utilizing summary data from genome-wide association studies (GWAS) of amino acids (sample 1, n = 86,507) and of offspring birthweight (sample 2, combined UK Biobank and Early Growth Genetics Consortium, n = 406,063). Seventy-five independent single nucleotide polymorphisms (SNPs) robustly associated with 18 amino acids (p &lt; 4.9 × 10-10) were used as genetic instruments. Wald ratio and inverse variance weighted methods were used in MR main analysis. Sensitivity analyses were performed to explore IV assumption violations. To explore whether there was consistency between SNP-amino acid associations in pregnancy and in the GWAS, the latter were compared to associations in the Born in Bradford cohort.

Results
There was evidence of positive causal effects of maternal alanine (51.9 g birthweight increase per SD increase in amino acid level, 95% CI: 24.2, 79.5), glutamine (51.3 g, 95% CI: 33.5, 69.0), glycine (10.4 g, 95% CI: 1.3, 19.6) and serine (27.1 g, 95% CI: 11.2, 43.0) on birthweight and inverse causal effects of maternal isoleucine (-109.7 g, 95% CI: -194.6, -24.9) and histidine (-41.1 g, 95% CI: -78.5, -3.7) on birthweight. Sensitivity analyses to explore reverse causality and bias due to horizontal pleiotropy supported our findings.

Conclusions
Some maternal circulating amino acids have causal effects on birthweight.

Key messages
MR can be extended to probe effects of maternal nutrition on offspring development.
932Using marginal structural models to account for selection bias in the analysis of legacy effect
Authors: Zhu Lin , Hayen Andrew , Bell Katy 
Published: September 2021

Abstract

Background
Analyses of legacy effects are mainly based on post-trial follow-up study after initial randomized controlled trials (RCT). However, the differential event rates between arms may cause a violation of randomization balance and induce selection bias in the post-trial analysis. We conducted a simulation to illustrate the bias and explore if marginal structural model (MSM) can address it.

Methods
Our simulation combined an RCT and an extended follow-up study. The scenarios investigated include different settings of direct treatment effect, legacy effect and underlying event rate. To fit the MSM, we used the inverse probability weighting method. The performance of MSM was compared to the standard model with and without adjustment of baseline covariate.

Results
Post-trial analysis without making adjustment resulted in biased estimates, and the bias increased with the underlying event rate and treatment effect. Both MSM and standard baseline covariate adjustment equally corrected for the bias if no patients took treatment after the trial. We are currently undertaking analysis for scenarios where some people continue treatment post-trial, and there is treatment confounder feedback; these results will be presented at the Congress.

Conclusions
Estimation of legacy effects using post-trial data without adjusting for differential survival between randomised treatment arms results in biased estimates. Although both standard covariate adjustment and MSM correct the bias if no patients take treatment in the post-trial period, MSM is expected to be the best method in the more realistic scenario where some patients continue to take treatment, and there is treatment confounder feedback.

Key messages
Post-trial analysis without making adjustment results in biased estimation of legacy effect. Marginal structural models may be used to address the selection bias.
Political (Over)Representation of Public Sector Employees and the Double-Motive Hypothesis: Evidence from Norwegian Register Data (2007–2019)
Authors: Geys Benny , Murdoch Zuzana , Sørensen Rune J 
Published: September 2021

Abstract
Countries have widely diverging regulations regarding the eligibility of public sector employees for political office, and the stringency of such regulations remains fiercely debated. Building on a demand and supply model of political selection, this article contributes to such debates by studying whether and how the incentives of public employees as both consumers and producers of public services (their “double motive”) affects their descriptive political representation. Our analysis employs population-wide individual-level register data covering four Norwegian local elections between 2007 and 2019 (N &gt; 13 million observations). Using predominantly individual-level panel regression models, we find that public employees are strongly overrepresented on election lists and have a higher probability of election (conditional on running). Looking at underlying mechanisms, we provide evidence consistent with the “double motive” of public employees inducing their self-selection into standing for elected office (at higher-ranked ballot positions). Demand-side effects deriving from party and voter selection receive more limited empirical support. We discuss ensuing concerns about the potential substantive representation of policy self-interests by elected public employees.
Quiescent galaxies in a virialized cluster at redshift 2: evidence for accelerated size growth
Authors: Noordeh E , Canning R E A , Willis J P , Allen S W , Mantz A , Stanford S A , Brammer G 
Published: September 2021

ABSTRACT
We present an analysis of the galaxy population in XLSSC 122, an X-ray-selected, virialized cluster at redshift z = 1.98. We utilize Hubble Space Telescope (HST)Wide Field Camera 3 (WFC3) photometry to characterize the activity and morphology of spectroscopically confirmed cluster members. The quiescent fraction is found to be $88^{+4}_{-20}$ per cent within 0.5r500, significantly enhanced over the field value of $20^{+2}_{-2}$ per cent at z ∼ 2. We find an excess of ‘bulge-like’ quiescent cluster members with Sérsic index n &gt; 2 relative to the field. These galaxies are found to be larger than their field counterparts at 99.6 per cent confidence, being on average $63^{+31}_{-24}$ per cent larger at a fixed mass of $M_\star = 5\times 10^{10} \, \mathrm{M}_\odot$. This suggests that these cluster member galaxies have experienced an accelerated size evolution relative to the field at z &gt; 2. We discuss minor mergers as a possible mechanism underlying this disproportionate size growth.
Radiation GRMHD simulations of M87: funnel properties and prospects for gap acceleration
Authors: Yao Philippe Z , Dexter Jason , Chen Alexander Y , Ryan Benjamin R , Wong George N 
Published: September 2021

Abstract
We use the public code ebhlight to carry out 3D radiative general relativistic magnetohydrodynamics (GRMHD) simulations of accretion on to the supermassive black hole in M87. The simulations self-consistently evolve a frequency-dependent Monte Carlo description of the radiation field produced by the accretion flow. We explore two limits of accumulated magnetic flux at the black hole (SANE and MAD), each coupled to several subgrid prescriptions for electron heating that are motivated by models of turbulence and magnetic reconnection. We present convergence studies for the radiation field and study its properties. We find that the near-horizon photon energy density is an order of magnitude higher than is predicted by simple isotropic estimates from the observed luminosity. The radially dependent photon momentum distribution is anisotropic and can be modeled by a set of point-sources near the equatorial plane. We draw properties of the radiation and magnetic field from the simulation and feed them into an analytic model of gap acceleration to estimate the very high energy (VHE) γ-ray luminosity from the magnetized jet funnel, assuming that a gap is able to form. We find luminosities of $\rm \sim 10^{41} \, erg \, s^{-1}$ for MAD models and $\rm \sim 2\times 10^{40} \, erg \, s^{-1}$ for SANE models, which are comparable to measurements of M87’s VHE flares. The time-dependence seen in our calculations is insufficient to explain the flaring behaviour. Our results provide a step towards bridging theoretical models of near-horizon properties seen in black hole images with the VHE activity of M87.
Cosmography using strong-lensing systems and cosmic chronometers
Authors: Lizardo Andrés , Amante Mario H , García-Aspeitia Miguel A , Magaña Juan , Motta V 
Published: September 2021

ABSTRACT
Using a new sub-sample of observed strong gravitational lens systems, for the first time, we present the equation for the angular diameter distance in the y-redshift scenario for cosmography and use it to test the cosmographic parameters. In addition, we also use the observational Hubble data from cosmic chronometers and a joint analysis of both data are performed. Among the most important conclusions are that this new analysis for cosmography using strong-lensing systems (SLSs) is equally competitive to constrain the cosmographic parameters as others presented in literature. Additionally, we present the reconstruction of the effective equation of state inferred from our samples, showing that at z = 0 those reconstructions from SLSs and joint analysis are in concordance with the standard model of cosmology.
General relativistic MHD simulations of non-thermal flaring in Sagittarius A*
Authors: Chatterjee K , Markoff S , Neilsen J , Younsi Z , Witzel G , Tchekhovskoy A , Yoon D , Ingram A , van der Klis M , Boyce H , Do T , Haggard D , Nowak M A 
Published: September 2021

ABSTRACT
Sgr A* exhibits regular variability in its multiwavelength emission, including daily X-ray flares and roughly continuous near-infrared (NIR) flickering. The origin of this variability is still ambiguous since both inverse Compton and synchrotron emission are possible radiative mechanisms. The underlying particle distributions are also not well constrained, particularly the non-thermal contribution. In this work, we employ the GPU-accelerated general relativistic magnetohydrodynamics code H-AMR to perform a study of flare flux distributions, including the effect of particle acceleration for the first time in high-resolution 3D simulations of Sgr A*. For the particle acceleration, we use the general relativistic ray-tracing code bhoss to perform the radiative transfer, assuming a hybrid thermal+non-thermal electron energy distribution. We extract ∼60 h light curves in the sub-millimetre, NIR and X-ray wavebands, and compare the power spectra and the cumulative flux distributions of the light curves to statistical descriptions for Sgr A* flares. Our results indicate that non-thermal populations of electrons arising from turbulence-driven reconnection in weakly magnetized accretion flows lead to moderate NIR and X-ray flares and reasonably describe the X-ray flux distribution while fulfilling multiwavelength flux constraints. These models exhibit high rms per cent amplitudes, $\gtrsim 150{{\ \rm per\ cent}}$ both in the NIR and the X-rays, with changes in the accretion rate driving the 230 GHz flux variability, in agreement with Sgr A* observations.
Cluster assembly times as a cosmological test
Authors: Amoura Yuba , Drakos Nicole E , Berrouet Anael , Taylor James E 
Published: September 2021

ABSTRACT
The abundance of galaxy clusters in the low-redshift Universe provides an important cosmological test, constraining a product of the initial amplitude of fluctuations and the amount by which they have grown since early times. The degeneracy of the test with respect to these two factors remains a limitation of abundance studies. Clusters will have different mean assembly times, however, depending on the relative importance of initial fluctuation amplitude and subsequent growth. Thus, structural probes of cluster age such as concentration, shape, or substructure may provide a new cosmological test that breaks the main degeneracy in number counts. We review analytical predictions for how mean assembly time should depend on cosmological parameters, and test these predictions using cosmological simulations. Given the overall sensitivity expected, we estimate the cosmological parameter constraints that could be derived from the cluster catalogues of forthcoming surveys such as Euclid, the Nancy Grace Roman Space Telescope, eROSITA, or CMB-S4. We show that by considering the structural properties of their cluster samples, such surveys could easily achieve errors of Δσ8 = 0.01 or better.
Timing observations of three Galactic millisecond pulsars
Authors: Lorimer D R , Kawash A M , Freire P C C , Smith D A , Kerr M , McLaughlin M A , Mickaliger M B , Spiewak R , Bailes M , Barr E , Burgay M , Cameron A D , Camilo F , Johnston S , Jankowski F , Keane E F , Keith M , Kramer M , Possenti A 
Published: September 2021

ABSTRACT
We report observed and derived timing parameters for three millisecond pulsars (MSPs) from observations collected with the Parkes 64-m telescope, Murriyang. The pulsars were found during reprocessing of archival survey data by Mickaliger et al. One of the new pulsars (PSR J1546–5925) has a spin period P = 7.8 ms and is isolated. The other two (PSR J0921–5202 with P = 9.7 ms and PSR J1146–6610 with P = 3.7 ms) are in binary systems around low-mass (${\gt}0.2\, {\rm M}_{\odot }$) companions. Their respective orbital periods are 38.2 and 62.8 d. While PSR J0921–5202 has a low orbital eccentricity e = 1.3 × 10−5, in keeping with many other Galactic MSPs, PSR J1146–6610 has a significantly larger eccentricity, e = 7.4 × 10−3. This makes it a likely member of a group of eccentric MSP–helium white dwarf binary systems in the Galactic disc whose formation is poorly understood. Two of the pulsars are co-located with previously unidentified point sources discovered with the Fermi satellite’s Large Area Telescope, but no γ-ray pulsations have been detected, likely due to their low spin-down powers. We also show that, particularly in terms of orbital diversity, the current sample of MSPs is far from complete and is subject to a number of selection biases.
Combined lensed estimator to probe the post-reionization H i power spectrum
Authors: Arora Urvashi , Dutta Prasun 
Published: September 2021

ABSTRACT
In the post-reionization era, the baryons assembled into the protogalaxies and eventually the present population of the galaxies evolved through merger and evolution. In this work, we discuss a possible probe of the statistical distribution and evolution of the H i density in the post-reionization era. We introduce an estimator of the H i power spectrum from the post-reionization Universe by observing it through the strong gravitational lenses by the nearby galaxy cluster. We also analytically calculate the uncertainties associated with the estimates of the post-EoR power spectrum for the discussed estimator. We access the efficacy of this estimator in the context of 19 galaxy clusters for which the lensing potential has been estimated earlier by various authors. We find that by combining the lensed power spectrum through eight of these cluster lenses, it is possible to estimate the post-reionization H i power spectrum at five-sigma significance for angular multipoles &lt;4000 for a uGMRT observation of 16 MHz bandwidth from redshifts of 1.25, 1.5 with a total of 400 h of observation. With the same setup, for a redshift of 3.0, we need 200 h of total observation time. The estimator also suppresses the diffused galactic foreground, though, the latter is still a dominant contributor to the overall signal and hence need to be estimated and mitigated. We discuss the merits and demerits of the estimator.
Turbulence and its connection to episodic accretion in binary YSOs
Authors: Riaz R , Schleicher D R G , Vanaverbeke S , Klessen Ralf S 
Published: September 2021

ABSTRACT
We report signatures of episodic accretion in young stellar objects (YSOs) that emerge in protobinary configurations in a gravoturbulent gas collapse. We find in most of these protobinary systems strong accretion bursts between the two companions with a recurrence time-scale of about 1 kyr. The accretion rate on to the secondary star typically exceeds that on to the primary with a peak value of 2 × 10−2 M⊙ yr−1 for the former and 6 × 10−3 M⊙ yr−1 for the latter. We propose that the secondary companion, which remains more active in its episodes of accretion bursts, especially for the gas cores with subsonic velocity dispersion, may provide observational opportunities to find traces of episodic accretion in the surrounding gas of the embedded YSOs that are in a binary configuration. Also, protostars evolving as single objects in the same environment show fewer accretion bursts and all together a more steady mass growth history. The prestellar cores with subsonic velocity dispersion exhibit an order of magnitude more intense accretion bursts than in the case of cores with supersonic velocity dispersions. The latter shows the formation of some of the protobinaries in which the primary acts as a more actively accreting companion. This can support these binaries to become systems of extreme mass ratio. Moreover, the YSOs in binary configurations with small semimajor axis a ≈ 50 au and high mass ratio q &gt; 0.7 support phases of intense episodic accretion. The eccentricity, however, seems to play no significant role in the occurrence of accretion bursts.
Laplace surface dynamics, revisited: satellites, exoplanets, and debris with distant, eccentric companions
Authors: Farhat Mohammad A , Touma Jihad R 
Published: September 2021

ABSTRACT
To date, studies of Laplace surface dynamics have concerned themselves with test particle orbits of fixed shape and orientation in the combined field of an oblate central body (to which the particle is bound) and a distant, inclined companion, which is captured to quadrupolar order. While amply sufficient for satellites around planets on near-circular orbits, the quadrupolar approximation fails to capture essential dynamical features induced by a wide binary companion (be it a star, a planet, or a black hole) on a fairly eccentric orbit. With similar astronomical settings in mind, we extend the classical Laplace framework to higher multipoles and map out the backbone of stationary orbits, now made complex by the broken axial symmetry. Eccentric and inclined Laplace equilibria, which had been presaged in systems of large enough mutual inclination, are here delineated over a broad range of mutually inclined perturbations. We recover them for test particles in the field of a hot Jupiter and a wide eccentric stellar binary, highlighting their relevance for the architecture of multi-planet systems in binaries. We then extend and deploy our machinery closer to home, as we consider the secular dynamics of trans-Neptunian objects (TNOs) in the presence of a putative ninth planet. We show how generalized Laplace equilibria seed islands for trans-Neptunian objects to be sheltered around, islands within chaotic seas that we capture via Poincaré sections, while highlighting a beautiful interplay between Laplace and Kozai–Lidov secular dynamical structures. An eminently classical tale revived for the exoplanetary 21st century!
Kidney tubule health, mineral metabolism and adverse events in persons with CKD in SPRINT
Authors: Ascher Simon B , Scherzer Rebecca , Estrella Michelle M , Berry Jarett D , de Lemos James A , Jotwani Vasantha K , Garimella Pranav S , Malhotra Rakesh , Bullen Alexander L , Katz Ronit , Ambrosius Walter T , Cheung Alfred K , Chonchol Michel , Killeen Anthony A , Ix Joachim H , Shlipak Michael G ,   for the SPRINT Research Group
Published: September 2021

Abstract

Background
Measures of kidney tubule health are risk markers for acute kidney injury (AKI) in persons with chronic kidney disease (CKD) during hypertension treatment, but their associations with other adverse events (AEs) are unknown.

Methods
Among 2377 Systolic Blood Pressure Intervention Trial (SPRINT) participants with CKD, we measured at baseline eight urine biomarkers of kidney tubule health and two serum biomarkers of mineral metabolism pathways that act on the kidney tubules. Cox proportional hazards models were used to evaluate biomarker associations with risk of a composite of pre-specified serious AEs (hypotension, syncope, electrolyte abnormalities, AKI, bradycardia and injurious falls) and outpatient AEs (hyperkalemia and hypokalemia).

Results
At baseline, the mean age was 73 ± 9 years and mean estimated glomerular filtration rate (eGFR) was 46 ± 11 mL/min/1.73 m2. During a median follow-up of 3.8 years, 716 (30%) participants experienced the composite AE. Higher urine interleukin-18, kidney injury molecule-1, neutrophil gelatinase-associated lipocalin (NGAL) and monocyte chemoattractant protein-1 (MCP-1), lower urine uromodulin (UMOD) and higher serum fibroblast growth factor-23 were individually associated with higher risk of the composite AE outcome in multivariable-adjusted models including eGFR and albuminuria. When modeling biomarkers in combination, higher NGAL [hazard ratio (HR) = 1.08 per 2-fold higher biomarker level, 95% confidence interval (CI) 1.03–1.13], higher MCP-1 (HR = 1.11, 95% CI 1.03–1.19) and lower UMOD (HR = 0.91, 95% CI 0.85–0.97) were each associated with higher composite AE risk. Biomarker associations did not vary by intervention arm (P &gt; 0.10 for all interactions).

Conclusions
Among persons with CKD, several kidney tubule biomarkers are associated with higher risk of AEs during hypertension treatment, independent of eGFR and albuminuria.