bluuebunny/crossref_metadata_2025_split huggingface dataset:
Association of Health-Care System and Survival in African American and Non-Hispanic White Patients With Bladder Cancer
Authors: Kotha Nikhil V , Kumar Abhishek , Qiao Edmund M , Qian Alex S , Voora Rohith S , Nalawade Vinit , Karim Kader A , McKay Rana R , Stewart Tyler F , Rose Brent S 
Published: December 2021

Abstract

Background
African American patients with bladder cancer have inferior outcomes compared with non-Hispanic White (White) patients. We hypothesize that access to health care is a primary determinant of this disparity. We compared outcomes by race for patients with bladder cancer receiving care within the predominant hybrid-payer health-care model of the United States captured in the Surveillance, Epidemiology, and End Results (SEER) database with those receiving care within the equal-access model of the Veterans’ Health Administration (VHA).

Methods
African American and White patients diagnosed with bladder cancer were identified in SEER and VHA. Stage at presentation, bladder cancer–specific mortality (BCM), and overall survival (OS) were compared by race within each health-care system.

Results
The SEER cohort included 122 449 patients (93.7% White, 6.3% African American). The VHA cohort included 36 322 patients (91.0% White, 9.0% African American). In both cohorts, African American patients were more likely to present with muscle-invasive disease and metastases, but the differences between races were statistically significantly smaller in VHA. In SEER multivariable models, African American patients had worse BCM (hazard ratio [HR] = 1.22, 95% confidence interval [CI] = 1.15 to 1.29) and OS (HR = 1.26, 95% CI = 1.20 to 1.31). In contrast within the VHA, African American patients had similar BCM (HR = 0.97, 95% CI = 0.88 to 1.07) and OS (HR = 0.99, 95% CI = 0.93 to 1.05).

Conclusions
In this study of contrasting health-care models, receiving medical care in an equal-access system was associated with reduced differences in stage at presentation and eliminated disparities in survival outcomes for African American patients with bladder cancer. Our findings highlight the importance of reducing financial barriers to care to notably improve health equity and oncologic outcomes for African American patients.
Correlation of MTAP Immunohistochemistry With CDKN2A Status Assessed by Fluorescence In Situ Hybridization and Clinicopathological Features in CNS WHO Grade 2 and 3 Meningiomas: A Single Center Cohort Study
Authors: Sasaki Shoh , Takeda Maiko , Hirose Takanori , Fujii Tomomi , Itami Hiroe , Uchiyama Tomoko , Morita Kohei , Matsuda Ryosuke , Yamada Shuichi , Nakagawa Ichiro , Ohbayashi Chiho 
Published: December 2021

Abstract
CDKN2A homozygous deletion has occasionally been reported in atypical and anaplastic meningiomas and is considered as one of the genetic alterations commonly involved in their recurrence and malignant progression. Methylthioadenosine phosphorylase (MTAP) immunohistochemistry is a promising surrogate marker for CDKN2A homozygous deletion in different cancers but has not been examined in meningiomas. We performed CDKN2A FISH and MTAP immunohistochemistry on specimens from 30 patients with CNS WHO grade 2 (n = 27) and 3 (n = 3) meningiomas, including specimens from primary and recurrent tumors and then determined whether MTAP immunohistochemistry correlated with CDKN2A homozygous deletion and clinicopathological features. CDKN2A homozygous deletion was detected in 12% (3/26) of CNS WHO grade 2 and 67% (2/3) of CNS WHO grade 3 meningiomas; 3 cases exhibited temporal and/or spatial heterogeneity. MTAP loss was in excellent concordance with CDKN2A homozygous deletion (sensitivity; 100%, specificity; 100%). MTAP loss/CDKN2A homozygous deletion correlated with cellular proliferation (mitotic rate; p = 0.001, Ki-67 labeling index; p = 0.03) and poor prognosis (overall survival; p = 0.01, progression free survival; p &lt; 0.001). Thus, MTAP immunostaining can be a surrogate marker for CDKN2A homozygous deletion in meningiomas, and MTAP loss/CDKN2A homozygous deletion may be an important prognostic factor for meningiomas.
Pseudomonas syringaeaddresses distinct environmental challenges during plant infection through the coordinated deployment of polysaccharides
Authors: Krishna Pilla Sankara , Woodcock Stuart Daniel , Pfeilmeier Sebastian , Bornemann Stephen , Zipfel Cyril , Malone Jacob George 
Published: December 2021

AbstractPrior to infection, phytopathogenic bacteria face a challenging environment on the plant surface, where they are exposed to nutrient starvation and abiotic stresses. Pathways enabling surface adhesion, stress tolerance, and epiphytic survival are important for successful plant pathogenesis. Understanding the roles and regulation of these pathways is therefore crucial to fully understand bacterial plant infections. The phytopathogen Pseudomonas syringae pv. tomato (Pst) encodes multiple polysaccharides that are implicated in biofilm formation, stress survival, and virulence in other microbes. To examine how these polysaccharides impact Pst epiphytic survival and pathogenesis, we analysed mutants in multiple polysaccharide loci to determine their intersecting contributions to epiphytic survival and infection. In parallel, we used qRT–PCR to analyse the regulation of each pathway. Pst polysaccharides are tightly coordinated by multiple environmental signals. Nutrient availability, temperature, and surface association strongly affect the expression of different polysaccharides under the control of the signalling protein genes ladS and cbrB and the second messenger cyclic-di-GMP. Furthermore, functionally redundant, combinatorial phenotypes were observed for several polysaccharides. Exopolysaccharides play a role in mediating leaf adhesion, while α-glucan and alginate together confer desiccation tolerance. Our results suggest that polysaccharides play important roles in overcoming environmental challenges to Pst during plant infection.
COVID-19 Vaccine Hesitancy Among Deployed Personnel in a Joint Environment
Authors: Higginson Jason D , Tumin Dmitry , Kuehhas Timothy C , DeLozier-Hooks Susan E , Powell Carl A , Ramirez Dale D , Dabelić Anja , Basso Michael R 
Published: December 2021

ABSTRACT

Introduction
In the United States, vaccine hesitancy has been identified as a major barrier to vaccination against COVID-19, but attitudes toward COVID-19 vaccination among military personnel are not well understood. We evaluated the prevalence and correlates of COVID-19 vaccine consent or refusal among deployed personnel in a joint environment.

Materials and Methods
Deidentified data were retrospectively extracted from the electronic medical record of the Military Health System in May 2021. All personnel currently assigned to the deployment area of operations were included in the analysis if their choice to receive the vaccine was known. Personnel characteristics were compared by vaccine acceptance status using chi-square tests, Fisher’s exact tests, or correlation coefficients. This analysis was exempted from Institutional Review Board review.

Results
The sample included 1,809 individuals, primarily members of the Army (72%) and members of Reserve (53%) or National Guard (27%) units. In the overall sample, 61% accepted the vaccine, with vaccine acceptance rates being lowest among Black or African American personnel (54%; P = .03 for comparison across racial groups) and members of Reserve or National Guard units (59%; P &lt; .001 for comparison by component). No differences in vaccine acceptance were found according to sex or health status (including prior COVID-19 infection).

Conclusions
Overall vaccine acceptance was greater among deployed military personnel than that reported in the U.S. population as a whole. However, lower vaccine acceptance among personnel from marginalized populations suggests a need to ensure that all service members have sufficient opportunities to have a frank and ongoing discussion with health care providers to address concerns related to vaccination. Additionally, lower vaccine acceptance among Reserve and National Guard personnel indicates a need for innovative educational approaches to counter vaccine hesitancy in the premobilization phase of deployment.
Protostellar outflows: a window to the past
Authors: Rohde P F , Walch S , Seifried D , Whitworth A P , Clarke S D 
Published: December 2021

ABSTRACT
During the early phases of low-mass star formation, episodic accretion causes the ejection of high-velocity outflow bullets, which carry a fossil record of the driving protostar’s accretion history. We present 44 SPH simulations of $1\, {{\mathrm{M}}}_{\odot }$ cores, covering a wide range of initial conditions, and follow the cores for five free-fall times. Individual protostars are represented by sink particles, and the sink particles launch episodic outflows using a sub-grid model. The Optics algorithm is used to identify individual episodic bullets within the outflows. The parameters of the overall outflow and the individual bullets are then used to estimate the age and energetics of the outflow, and the accretion events that triggered it, and to evaluate how reliable these estimates are, if observational uncertainties and selection effects (like inclination) are neglected. Of the commonly used methods for estimating outflow ages, it appears that those based on the length and speed of advance of the lobe are the most reliable in the early phases of evolution, and those based on the width of the outflow cavity and the speed of advance are most reliable during the later phases. We describe a new method that is almost as accurate as these methods, and reliable throughout the evolution. In addition, we show how the accretion history of the protostar can be accurately reconstructed from the dynamics of the bullets if each lobe contains at least two bullets. The outflows entrain about 10 times more mass than originally ejected by the protostar.
Influence of Comptonization region over the ambiance of accretion disc in active galactic nucleus
Authors: Sriram K , Nour D , Choi C S 
Published: December 2021

ABSTRACT
Understanding the radiative and physical structures of inner region of a few 100 pc of active galactic nucleus (AGNs) is important to constrain the causes of their activities. Although the X-ray emission from the Comptonization region/corona and the accretion disc regulates the broad-line emission regions and torus structures, the exact mutual dependency is not understood well. We performed correlation studies for X-ray, mid-infrared, and different components of Balmer emission lines for the selected sample of AGNs. Almost 10 different parameters and their interdependencies were explored in order to understand the underlying astrophysics. We found that the X-ray luminosity has a linear dependency on the various components of broad Balmer emission lines (e.g. L$_{\text{2-10 keV}}\, \propto$ L$^{0.78}_{\text{H}\beta ^{\text{B}}}$) and found a strong dependency on the optical continuum luminosity (L$_{\text{2-10 keV}}\, \propto$ L$^{0.86}_{5100\, \mathring{\rm A}}$). For a selected sample, we also observed a linear dependency between X-ray and mid-infrared luminosity (L$_{\text{2-10 keV}}\, \propto$ L$^{0.74}_{6\, \mu \text{m}}$). A break point was observed in our correlation studies for X-ray power-law index, Γ, and mass of black hole at ∼ log (M/M⊙) = 8.95. Similarly, the relations between Γ and full width at half-maximum (FWHM) of H α and H β broad components show breaks at FWHMH α = 7642 ± 657 km s−1 and FWHMH β = 7336 ± 650 km s−1. However, more data are required to confine the breaks locations exactly. We noted that Γ and Eddington ratios are negatively correlated to Balmer decrements in our selected sample. We analysed and discussed about the implications of new findings in terms of interaction AGN structures.
Imaging sensitivity of a linear interferometer array on lunar orbit
Authors: Shi Yuan , Xu Yidong , Deng Li , Wu Fengquan , Wu Lin , Huang Qizhi , Zuo Shifan , Yan Jingye , Chen Xuelei 
Published: December 2021

ABSTRACT
Ground-based observation at frequencies below 30 MHz is hindered by the ionosphere of the Earth and radio frequency interference. To map the sky at these low frequencies, we have proposed the Discovering the Sky at the Longest wavelength mission (DSL, also known as the ‘Hongmeng’ mission, which means ‘Primordial Universe’ in Chinese) concept, which employs a linear array of micro-satellites orbiting the Moon. Such an array can make interferometric observations achieving good angular resolutions despite the small size of the antennas. However, it differs from the conventional ground-based interferometer array or even the previous orbital interferometers in many aspects, new data-processing methods need to be developed. In this work, we make a series of simulations to assess the imaging quality and sensitivity of such an array. We start with an input sky model and a simple orbit model, generate mock interferometric visibilities, and then reconstruct the sky map. We consider various observational effects and practical issues, such as the system noise, antenna response, and Moon blockage. Based on the quality of the recovered image, we quantify the imaging capability of the array for different satellite numbers and array configurations. For the first time, we make practical estimates of the point source sensitivity for such a lunar orbit array, and predict the expected number of detectable sources for the mission. Depending on the radio source number distribution which is still very uncertain at these frequencies, the proposed mission can detect 102–104 sources during its operation.
The galaxy–halo size relation of low-mass galaxies in FIRE
Authors: Rohr Eric , Feldmann Robert , Bullock James S , Çatmabacak Onur , Boylan-Kolchin Michael , Faucher-Giguère Claude-André , Kereš Dušan , Liang Lichen , Moreno Jorge , Wetzel Andrew 
Published: December 2021

ABSTRACT
Galaxy sizes correlate closely with the sizes of their parent dark matter haloes, suggesting a link between halo formation and galaxy growth. However, the precise nature of this relation and its scatter remains to be understood fully, especially for low-mass galaxies. We analyse the galaxy–halo size relation (GHSR) for low-mass ($M_\star \sim 10^{7-9}\, {\rm M}_\odot$) central galaxies over the past 12.5 billion years with the help of cosmological volume simulations (FIREbox) from the Feedback in Realistic Environments (FIRE) project. We find a nearly linear relationship between the half-stellar mass galaxy size R1/2 and the parent dark matter halo virial radius Rvir. This relation evolves only weakly since redshift z = 5: $R_{1/2}\, [{\rm kpc}] = (0.053\pm 0.002)(R_{\rm vir}/35\, {\rm kpc})^{0.934\pm 0.054}$, with a nearly constant scatter $\langle \sigma \rangle = 0.084\, [{\rm dex}]$. While this ratio is similar to what is expected from models where galaxy disc sizes are set by halo angular momentum, the low-mass galaxies in our sample are not angular momentum supported, with stellar rotational to circular velocity ratios vrot/vcirc ∼ 0.15. Introducing redshift as another parameter to the GHSR does not decrease the scatter. Furthermore, this scatter does not correlate with any of the halo properties we investigate – including spin and concentration – suggesting that baryonic processes and feedback physics are instead critical in setting the scatter in the GHSR. Given the relatively small scatter and the weak dependence of the GHSR on redshift and halo properties for these low-mass central galaxies, we propose using galaxy sizes as an independent method from stellar masses to infer halo masses.
II. The effect of axisymmetric and spatially varying equilibria and flow on MHD wave modes: cylindrical geometry
Authors: Skirvin S J , Fedun V , Silva Suzana S A , Verth G 
Published: December 2021

ABSTRACT
Magnetohydrodynamic (MHD) waves are routinely observed in the solar atmosphere. These waves are important in the context of solar physics as it is widely believed they can contribute to the energy budget of the solar atmosphere and are a prime candidate to contribute towards coronal heating. Realistic models of these waves are required representing observed configurations such that plasma properties can be determined more accurately, since they cannot be measured directly. This work utilizes a previously developed numerical technique to find permittable eigenvalues under different non-uniform equilibrium conditions in a Cartesian magnetic slab geometry. Here, we investigate the properties of magnetoacoustic waves under non-uniform equilibria in a cylindrical geometry. Previously obtained analytical results are retrieved to emphasize the power and applicability of this numerical technique. Further case studies investigate the effect that a radially non-uniform plasma density and non-uniform plasma flow, modelled as a series of Gaussian profiles, have on the properties of different MHD waves. For all cases the dispersion diagrams are obtained and spatial eigenfunctions calculated which display the effects of the equilibrium inhomogeneity. It is shown that as the equilibrium non-uniformity is increased, the radial spatial eigenfunctions are affected and extra nodes introduced, similar to the previous investigation of a magnetic slab. Furthermore, azimuthal perturbations are increased with increasing inhomogeneity introducing vortical motions inside the waveguide. Finally, 2D and 3D representations of the velocity fields are shown which may be useful for observers for wave mode identification under realistic magnetic waveguides with ever increasing instrument resolution.
Scaling pair count to next galaxy surveys
Authors: Plaszczynski S , Campagne J E , Peloton J , Arnault C 
Published: December 2021

ABSTRACT
Counting pairs of galaxies or stars according to their distance is at the core of real-space correlation analyses performed in astrophysics and cosmology. Upcoming galaxy surveys (LSST, Euclid) will measure properties of billions of galaxies challenging our ability to perform such counting in a minute-scale time relevant for the usage of simulations. The problem is only limited by efficient access to the data, hence belongs to the big data category. We use the popular Apache Spark framework to address it and design an efficient high-throughput algorithm to deal with hundreds of millions to billions of input data. To optimize it, we revisit the question of non-hierarchical sphere pixelization based on cube symmetries and develop a new one dubbed the ‘Similar Radius Sphere Pixelization’ (SARSPix) with very close to square pixels. It provides the most adapted indexing over the sphere for all distance-related computations. Using LSST-like fast simulations, we compute autocorrelation functions on tomographic bins containing between a hundred million to one billion data points. In each case, we achieve the construction of a standard pair-distance histogram in about 2 min, using a simple algorithm that is shown to scale, over a moderate number of nodes (16–64). This illustrates the potential of this new techniques in the field of astronomy where data access is becoming the main bottleneck. They can be easily adapted to other use-cases as nearest-neighbours search, catalogue cross-match or cluster finding. The software is publicly available from https://github.com/astrolabsoftware/SparkCorr.
A simple time-dependent method for calculating spirals: applications to eccentric planets in protoplanetary discs
Authors: Zhu Zhaohuan , Zhang Raymond M 
Published: December 2021

ABSTRACT
Spirals in protoplanetary discs have been used to locate the potential planet in discs. Since only the spiral shape from a circularly orbiting perturber is known, most previous works assume that the planet is in a circular orbit. We develop a simple semi-analytical method to calculate the shape of the spirals launched by an eccentric planet. We assume that the planet emits wavelets during its orbit, and the wave fronts of these propagating wavelets form the spirals. The resulting spiral shape from this simple method agrees with numerical simulations exceptionally well. The spirals excited by an eccentric planet can detach from the planet, bifurcate, or even cross each other, which are all reproduced by this simple method. The spiral’s bifurcation point corresponds to the wavelet that is emitted when the planet’s radial speed reaches the disc’s sound speed. Multiple spirals can be excited by an eccentric planet (more than five spirals when e ≳ 0.2). The pitch angle and pattern speed are different between different spirals and can vary significantly across one spiral. The spiral wakes launched by high-mass eccentric planets steepen to spiral shocks and the crossing of spiral shocks leads to distorted or broken spirals. With the same mass, a more eccentric planet launches weaker spirals and induces a shallower gap over a long period of time. The observed unusually large/small pitch angles of some spirals, the irregular multiple spirals, and the different pattern speeds between different spirals may suggest the existence of eccentric perturbers in protoplanetary discs.
Inside–out planet formation: VI. oligarchic coagulation of planetesimals from a pebble ring?
Authors: Cai Maxwell X , Tan Jonathan C , Portegies Zwart Simon 
Published: December 2021

ABSTRACT
Inside–Out Planet Formation (IOPF) is a theory addressing the origin of Systems of Tightly-Packed Inner Planets (STIPs) via in situ formation and growth of the planets. It predicts that a pebble ring is established at the pressure maximum associated with the dead zone inner boundary (DZIB) with an inner disc magnetorotational instability (MRI)-active region. Using direct N-body simulations, we study the collisional evolution of planetesimals formed from such a pebble ring, in particular, examining whether a single dominant planet emerges. We consider a variety of models, including some in which the planetesimals are continuing to grow via pebble accretion. We find that the planetesimal ring undergoes oligarchic evolution, and typically turns into 2 or 3 surviving oligarchs on nearly coplanar and circular orbits, independent of the explored initial conditions or form of pebble accretion. The most massive oligarchs typically consist of about $70{{\ \rm per\ cent}}$ of the total mass, with the building-up process typically finishing within ∼105 yr. However, a relatively massive secondary planet always remains with $\sim 30\!-\!65{{\ \rm per\ cent}}$ of the mass of the primary. Such secondary planets have properties that are inconsistent with the observed properties of the innermost pairs of planets in STIPs. Thus, for IOPF to be a viable theory for STIP formation, it needs to be shown how oligarchic growth of a relatively massive secondary from the initial pebble ring can be avoided. We discuss some potential additional physical processes that should be included in the modelling and explored as next steps.