bluuebunny/crossref_metadata_2025_split huggingface dataset:
Sex dimorphic response to osteocyte miR21 deletion in murine calvaria bone as determined by RNAseq analysis
Authors: Peng Gang , Deosthale Padmini , Pianeta Roquelina , Messersmith Hannah M , Plotkin Lilian I 
Published: April 2024

Abstract
Low levels of microRNA (miR) 21 may explain the higher osteocyte apoptosis with Cx43-deficient and aged female mice. However, miR21 exerts a sex-divergent role in osteocytes, regulating bone mass and architecture through non-cell autonomous effects on osteoblasts and osteoclasts, via sex-specific regulation of osteocyte cytokine production. miR21 deficiency improves bone strength in females, and, to a higher extent, in male miR21-deficient mice. To understand the molecular basis for the effects of miR21 deletion, mRNA was isolated from miR21fl/fl (controls) or miR21-deficient (by deletion in cells expressing Cre recombinase under the control of the 8 kb fragment of the DMP1 promoter: miR21ΔOt mice). miR21 was 50% lower in miR21ΔOt whole calvaria bone compared to control mice of the corresponding sex. RNAseq was performed in 4 samples/sex and genotype. There were 152 genes with &lt;.05 P-value and &gt;1 absolute log2 fold change in the male data analysis, and expression of most genes was higher in the miR21fl/fl group. Two of the genes, Actn3 and Myh4, had a false discovery rate &lt; 0.1. Gene enrichment analysis of significant genes on both KEGG pathways and gene ontology (GO) gene sets shows that the significant genes were enriched in muscle contraction. Some muscle-related genes like Actn3 were included in multiple significant pathways. For females, only 65 genes had P-value &lt;.05 and &gt;1 absolute log2 fold change. Yet, no significant KEGG or GO pathways, including ≥5 significant genes, were seen, and no overlap of significant genes was found between male and female samples. Therefore, deletion of miR21 has a stronger effect on male transcriptome in calvaria, compared to females. Further, no enrichment of any pathway was detected in female samples. Thus, either there are no differences between 2 groups in female or the effect size is small, and a larger sample size is needed to uncover miR21-dependent differences.
Verifying the nonreporting hemolysis index for potassium, phosphate, magnesium, AST, LDH, iron, CA 19-9, and vitamin D, using Beckman Coulter AU5800 and DxI800 automated analyzers
Authors: Sheerin Samuel 
Published: April 2024

Abstract

Background
Hemolysis is a common reason for nonreporting results in biochemistry and is measured using the hemolysis index (HI), with nonreporting limits set for analytes by manufacturers.

Objective
To verify the nonreporting HI limit for potassium, phosphate, magnesium, aspartate aminotransferase (AST), lactate dehydrogenase (LDH), iron, CA19-9, and vitamin D on the Beckman Coulter AU5800/DxI800 analyzers.

Method
Hemolysate was created from EDTA-lined tubes of whole blood using an osmotic shock procedure. The hemolysate underwent serial dilutions with saline and was spiked in paired serum. The delta changes in HI and analyte concentration were measured, assessed using regression analysis, and compared against calculated reference change values.

Results
A linear relationship between increasing HI and increasing analyte concentration (R2 &gt; 0.9) was observed for potassium (y = 0.8864x), phosphate (y = 0.1079x), magnesium (y = 0.0678x), AST (y = 29.035x), and LDH (y = 350x). Increasing HI values did not have a linear effect on iron (y = −0.2544x), CA19-9 (y = 2.7019x), or vitamin D (y = 8.036x) concentrations.

Conclusion
The results from this experiment support increasing the HI nonreporting limit to 100 mg/dL for potassium; 200 mg/dL for magnesium; and 300 mg/dL for phosphate, CA19-9, and vitamin D. The iron assay is not affected by hemolysis as high as 500 mg/dL. The current HI nonreporting limit of 50 mg/dL is appropriate for LDH.
Atmospheric characterization and tighter constraints on the orbital misalignment of WASP-94 A b with HARPS
Authors: Ahrer E , Seidel J V , Doyle L , Gandhi S , Prinoth B , Cegla H M , McDonald C H , Astudillo-Defru N , Ayache E , Nealon R , Veras Dimitri , Wheatley P J , Ehrenreich D 
Published: April 2024

ABSTRACT
We present high spectral resolution observations of the hot Jupiter WASP-94 A b using the HARPS instrument on ESO’s 3.6-m telescope in La Silla, Chile. We probed for Na absorption in its atmosphere as well as constrained the previously reported misaligned retrograde orbit using the Rossiter–McLaughlin effect. Additionally, we undertook a combined atmospheric retrieval analysis with previously published low-resolution data. We confirm the retrograde orbit as well as constrain the orbital misalignment with our measurement of a projected spin-orbit obliquity of λ = 123.0 ± 3.0°. We find a tentative detection of Na absorption in the atmosphere of WASP-94 A b, independent of the treatment of the Rossiter–McLaughlin effect in our analysis (3.6σ and 4.4σ). We combine our HARPS high-resolution data with low-resolution data from the literature and find that while the posterior distribution of the Na abundance results in a tighter constraint than using a single data set, the detection significance does not improve (3.2σ), which we attribute to degeneracies between the low- and high-resolution data.
On the detection and precise localization of merging black holes events through strong gravitational lensing
Authors: Wempe Ewoud , Koopmans Léon V E , Wierda A Renske A C , Hannuksela Otto A , Van Den Broeck Chris 
Published: April 2024

ABSTRACT
To unlock the full spectrum of astrophysical and cosmological applications of gravitational-wave detections, it is essential to localize the associated black hole mergers to high precision inside their host galaxies. One possible method to achieve this is to compare the properties of multiple detections of gravitationally lensed binary black hole merger events with the properties of strong gravitational lens systems located in the joint sky localization of the gravitational-wave detections. In this work, we simulate the population of binary black hole mergers lensed by galaxy-scale lenses and detectable by LIGO-Virgo-Kagra in the coming decade and the population of galaxy-scale strong lenses that will be detected by Euclid. We use these simulations to investigate the prospects for localizing strongly lensed binary black hole mergers inside the lensed galaxies of ‘Euclid-like’ galaxy-scale strong lenses. We find that for 20–$50\, \rm \%$ of strongly lensed gravitational-wave events the lens system is detectable with Euclid, if the event falls in its survey footprint. Of these, we expect to correctly identify the strongly lensed host galaxy as likely (with posterior probability) host galaxy – based on Bayesian evidence ranking of candidate hosts – for 34.6–$21.9\,\mathrm{ per\,cent}$ of quadruply lensed gravitational-wave events when given an a priori 1–5 $\deg ^{2}$ gravitational-wave-only sky localization. For triply and doubly lensed gravitational-wave events, this becomes 29.8–$14.9\,\mathrm{ per\,cent}$ and 16.4–$6.6\,\mathrm{ per\,cent}$ respectively. If successfully identified, however, the localization can be better than a fraction of the host-galaxy size, i.e. of order milli-arcseconds. A first detection in the coming decade, however, probably requires dedicated deep and high-resolution follow-ups and continued upgrades in the current and planned gravitational-wave detectors.
Increasing the power of weak lensing data with multipole-based intrinsic alignment estimators
Authors: Singh Sukhdeep , Shakir Ali , Jagvaral Yesukhei , Mandelbaum Rachel 
Published: April 2024

ABSTRACT
It has long been known that galaxy shapes align coherently with the large-scale density field. Characterizing this effect is essential to interpreting measurements of weak gravitational lensing, the deflection of light from distant galaxies by matter overdensities along the line of sight, as it also produces coherent galaxy alignments that we wish to interpret in terms of a cosmological model. Existing direct measurements of intrinsic alignments using galaxy samples with high-quality shape and redshift measurements typically use well-understood but sub-optimal projected estimators, which do not make good use of the information in the data when comparing those estimators to theoretical models. We demonstrate a more optimal estimator, based on a multipole expansion of the correlation functions or power spectra, for direct measurements of galaxy intrinsic alignments. We show that even using the lowest order multipole alone increases the significance of inferred model parameters using simulated and real data, without any additional modelling complexity. We apply this estimator to measurements of parameters of the non-linear alignment model using data from the Sloan Digital Sky survey, demonstrating consistent results with a factor of ∼2 greater precision in parameter fits to intrinsic alignments models. This result is functionally equivalent to quadrupling the survey area, but without the attendant costs – thereby demonstrating the value in using this new estimator in current and future intrinsic alignments measurements using spectroscopic galaxy samples.
Disentanglement of the chemodynamical assembly: mapping the Milky Way discs
Authors: Cantelli Elvis , Teixeira Ramachrisna 
Published: April 2024

ABSTRACT
The formation and structure of the Milky Way have a fundamental role in our understanding of the universe and its evolution, and thanks to the Gaia mission and large spectroscopic surveys, we live an exceptional moment of data availability, allowing us to trace the building blocks of the Galactic disc and their relations. In this sense, we propose here the exploration of a large data set in a top-down fashion, elaborating a similarity map of the local Galactic volume in order to segregate and characterize its main components, searching for hints about their relations. We have used the t-SNE algorithm with chemical, orbital and kinematic properties of the stars to produce 2D manifolds and dissect their structure by isolating populations to further analyse their behaviour. The young thin disc could be clearly separated from the older thick disc, also showing a puzzling transition zone with hints about the aftermath of the Gaia–Sausage–Enceladus merger. Moving groups and resonant features also appear prominently in the maps, splitting the disc into inner and outer portions as consequence of the resonances produced by the Galactic bar. The dynamical halo appears as an extreme end related to the heated portion of the thick disc, showing sub-structures corresponding to known accreted populations. Open and globular clusters also appear in their chemical/evolutionary context. We present details of the developed strategy, an overview of the different populations and their relations, as well as a discussion and insights of our results in the scenario of Galactic evolution.
On the inefficiency of particle re-acceleration mechanisms in the cores of massive stellar clusters
Authors: Vieu T , Härer L , Reville B 
Published: April 2024

ABSTRACT
We consider scenarios for non-thermal particle acceleration and re-acceleration in the central cores of compact massive star clusters, aided by insights from high-resolution hydrodynamic simulations. We show that (i) particles are unlikely to interact with many shocks during their lifetimes in the core; (ii) colliding flows do not produce hard spectra; and (iii) turbulent re-acceleration in the core is suppressed. Inefficient re-acceleration mechanisms are not expected to produce hard components nor to increase the maximum energy within the cores of massive star clusters. Models in which the observed ultra-high-energy gamma rays originate in the core of massive stellar clusters are thus disfavoured.
A comparative study of outflow structures of two classes of gamma-ray bursts
Authors: Liao Mao , Chen Jia-Ming , Li Ting , Peng Zhao-Yang 
Published: April 2024

ABSTRACT
The outflow structures of gamma-ray bursts (GRBs) can provide insights into the origins and radiation mechanisms of these cosmic explosions. We systematically study the GRB outflow structures by modelling their afterglow light curves and check if the structures of long gamma-ray bursts (LGRBs) and short gamma-ray bursts (SGRBs) are different. The sample consists of Swift-XRT afterglows with sufficient coverage and known redshift, which includes 195 well-fit LGRBs and 13 well-fit SGRBs. The model we use is a two-parameter ‘boosted fireball’ model, which consists of a family of outflows, with shapes varying smoothly from a quasi-spherical outflow to a highly collimated jet. We use the jetfit package to fit afterglow light curves and obtain the jet parameters. We find that there are no statistical differences in the distributions of jet parameters between LGRBs and SGRBs by performing K–S test and 74 per cent of the ratios of the observer angle to jet opening angle are in the range of 0.2 to 1. Our analysis indicates that the majority of GRB afterglows are viewed off-axis and there has no statistical difference between LGRBs and SGRBs. We also find that both the LGRBs and SGRBs exhibit two similar correlations: the jet opening angle is positively correlated with the observer angle, with the correlation coefficient 0.61 for LGRBs and 0.63 for SGRBs; the circumburst density is inversely correlated with the explosion energy with the correlation coefficient −0.89 for LGRBs and −0.69 for SGRBs. Our results suggest that the outflow structures are similar for the LGRBs and SGRBs.
The XUV-driven escape of the planets around TOI-431 and ν2 Lupi
Authors: King George W , Corrales Lía R , Fernández Fernández Jorge , Wheatley Peter J , Malsky Isaac , Osborn Ares , Armstrong David 
Published: April 2024

ABSTRACT
One of the leading mechanisms invoked to explain the existence of the radius valley is atmospheric mass-loss driven by X-ray and extreme-ultraviolet irradiation, with this process stripping the primordial envelopes of young, small planets to produce the observed bimodal distribution. We present an investigation into the TOI-431 and ν2 Lupi planetary systems, both of which host planets either side of the radius valley, to determine if their architectures are consistent with evolution by the X-ray/ultraviolet (XUV) mechanism. With XMM–Newton, we measure the current X-ray flux of each star, and see evidence for a stellar flare in the TOI-431 observations. We then simulate the evolution of all of the transiting planets across the two systems in response to the high-energy irradiation over their lifetimes. We use the measured X-ray fluxes as an anchor point for the XUV time evolution in our simulations, and employ several different models of estimating mass-loss rates. While the simulations for TOI-431 b encountered a problem with the initial calculated radii, we estimate a likely short (∼Myr) timespan for primordial envelope removal using reasonable assumptions for the initial planet. ν2 Lupi b is likely harder to strip, but is achieved in a moderate fraction of our simulations. None of our simulations stripped any of the lower density planets of their envelope, in line with prediction. We conclude that both systems are consistent with expectations for generation of the radius valley through XUV photoevaporation.
Disentangling the anisotropic radio sky: Fisher forecasts for 21 cm arrays
Authors: Zhang Zheng , Bull Philip , Glasscock Katrine A 
Published: April 2024

ABSTRACT
The existence of a radio synchrotron background (RSB) excess is implied by a number of measurements, including excess emission seen by the Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission (ARCADE 2) and Long Wavelength Array (LWA) experiments. Highly sensitive wideband radio arrays, of the kind used to measure the cosmic 21 cm signal, provide a promising way to further constrain the RSB excess through its anisotropy, providing additional insight into its origin. We present a framework for evaluating the potential of 21 cm arrays to disentangle different components of the diffuse radio sky based on the combination of their frequency spectrum and angular power spectrum. The formalism is designed to calculate uncertainties due to the intrinsic cosmic variance alone or together with instrumental noise. In particular, we predict the potential for measuring the anisotropy of a broad generalized class of excess radio background models using the low-frequency Hydrogen Epoch of Reionization Array (HERA) as an example. We find that a HERA-like array can distinguish an RSB excess from other sky components based on its angular clustering and spectral dependence, even if these are quite similar to one or more of the other components – but only in the case that the RSB excess is relatively bright.
Cosmological constraints on early dark energy from the full shape analysis of eBOSS DR16
Authors: Gsponer Rafaela , Zhao Ruiyang , Donald-McCann Jamie , Bacon David , Koyama Kazuya , Crittenden Robert , Simon Théo , Mueller Eva-Maria 
Published: April 2024

ABSTRACT
We evaluate the effectiveness of early dark energy (EDE) in addressing the Hubble tension using the luminous red galaxy (LRG), quasar (QSO), and emission line galaxy (ELG) samples from the completed eBOSS survey. We perform cosmological parameter measurements based on full shape analysis of the power spectrum employing the effective field theory of large-scale structure (EFTofLSS). EDE is known to strongly suffer from volume projection effects, complicating cosmological constraints’ interpretation. To quantify the volume projection effects within an EDE full shape analysis, we explore the impact of different prior choices on the nuisance parameters of EFTofLSS through an extensive mock study. We compare classical Gaussian priors to the non-informative Jeffreys prior, known to mitigate volume projection effects in ΛCDM. Our full shape analysis combines eBOSS and BOSS data with Planck, external Baryon Acoustic Oscillation (BAO), PantheonPlus, and SH0ES supernova data. EDE reduces the tension from 5.2σ to 3σ compared to ΛCDM, yielding $H_0=71.73_{-0.86}^{+0.82}$ km s−1 Mpc−1 with $f_\mathrm{EDE} = 0.1179_{-0.022}^{+0.025}$ (Gaussian priors) and $H_0=72.03_{-0.87}^{+0.82}$ km s−1 Mpc−1 with $f_\mathrm{EDE} = 0.1399_{-0.022}^{+0.023}$ (Jeffreys prior). Although the Hubble tension is mitigated compared to ΛCDM, the inclusion of eBOSS data amplifies the tension within EDE from 2σ to 3σ, in contrast to the full shape analysis of BOSS data with Planck, external BAO, PantheonPlus, and SH0ES. This highlights the significance of incorporating additional large-scale structure data in discussions concerning models aiming to resolve the Hubble tension.
Contemporary trends in the incidence and timing of spinal metastases: A population-based study
Authors: Shakil Husain , Malhotra Armaan K , Badhiwala Jetan H , Karthikeyan Vishwathsen , Essa Ahmad , He Yingshi , Fehlings Michael G , Sahgal Arjun , Dea Nicolas , Kiss Alex , Witiw Christopher D , Redelmeier Donald A , Wilson Jefferson R 
Published: April 2024

Abstract

Background
Spinal metastases are a significant complication of advanced cancer. In this study, we assess temporal trends in the incidence and timing of spinal metastases and examine underlying patient demographics and primary cancer associations.

Methods
In this population-based retrospective cohort study, health data from 2007 to 2019 in Ontario, Canada were analyzed (n = 37, 375 patients identified with spine metastases). Primary outcomes were annual incidence of spinal metastasis, and time to metastasis after primary diagnosis.

Results
The age-standardized incidence of spinal metastases increased from 229 to 302 cases per million over the 13-year study period. The average annual percent change (AAPC) in incidence was 2.2% (95% CI: 1.4% to 3.0%) with patients aged ≥85 years demonstrating the largest increase (AAPC 5.2%; 95% CI: 2.3% to 8.3%). Lung cancer had the greatest annual incidence, while prostate cancer had the greatest increase in annual incidence (AAPC 6.5; 95% CI: 4.1% to 9.0%). Lung cancer patients were found to have the highest risk of spine metastasis with 10.3% (95% CI: 10.1% to 10.5%) of patients being diagnosed at 10 years. Gastrointestinal cancer patients were found to have the lowest risk of spine metastasis with 1.0% (95% CI: 0.9% to 1.0%) of patients being diagnosed at 10 years.

Conclusions
The incidence of spinal metastases has increased in recent years, particularly among older patients. The incidence and timing vary substantially among different primary cancer types. These findings contribute to the understanding of disease trends and emphasize a growing population of patients who require subspecialty care.
Chromothripsis is rare in IDH-mutant gliomas compared to IDH-wild-type glioblastomas whereas whole-genome duplication is equally frequent in both tumor types
Authors: Sourty Baptiste , Basset Laëtitia , Fontaine Alix , Garcion Emmanuel , Rousseau Audrey 
Published: April 2024

Abstract

Background
Adult-type diffuse gliomas comprise IDH (isocitrate dehydrogenase)-mutant astrocytomas, IDH-mutant 1p/19q-codeleted oligodendrogliomas (ODG), and IDH-wild-type glioblastomas (GBM). GBM displays genome instability, which may result from 2 genetic events leading to massive chromosome alterations: Chromothripsis (CT) and whole-genome duplication (WGD). These events are scarcely described in IDH-mutant gliomas. The better prognosis of the latter may be related to their genome stability compared to GBM.

Methods
Pangenomic profiles of 297 adult diffuse gliomas were analyzed at initial diagnosis using SNP arrays, including 192 GBM and 105 IDH-mutant gliomas (61 astrocytomas and 44 ODG). Tumor ploidy was assessed with Genome Alteration Print and CT events with CTLPScanner and through manual screening. Survival data were compared using the Kaplan–Meier method.

Results
At initial diagnosis, 37 GBM (18.7%) displayed CT versus 5 IDH-mutant gliomas (4.7%; P = .0008), the latter were all high-grade (grade 3 or 4) astrocytomas. WGD was detected at initial diagnosis in 18 GBM (9.3%) and 9 IDH-mutant gliomas (5 astrocytomas and 4 oligodendrogliomas, either low- or high-grade; 8.5%). Neither CT nor WGD was associated with overall survival in GBM or in IDH-mutant gliomas.

Conclusions
CT is less frequent in IDH-mutant gliomas compared to GBM. The absence of CT in ODG and grade 2 astrocytomas might, in part, explain their genome stability and better prognosis, while CT might underlie aggressive biological behavior in some high-grade astrocytomas. WGD is a rare and early event occurring equally in IDH-mutant gliomas and GBM.