bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Measurement of the Splash-back Radius of Dark Matter Halos
Authors: Xu Weiwei , Shan Huanyuan , Li Ran , Yao Ji , Wang Chunxiang , Li Nan , Zhang Chaoli 
Published: August 2024

Abstract
In the hierarchical evolution framework of cosmology, larger halos grow through matter accretion and halo mergers. To clarify halo evolution, we need to define the halo mass and radius physically. However, the pseudoevolution problem makes the process difficult. Thus, we aim to measure the splash-back radius (R
sp), a physically defined halo radius for a large number of halos with various mass and redshift, and to determine the most important parameters that affect it. We use the typical definition of splash-back radius as the radius with the steepest radial density profile. In this work, we measure the splash-back radius of dark matter halos within the mass of 1013
M
⊙ to 3 × 1015
M
⊙ and redshifts spanning 0.08–0.65. This is the measurement of the R
sp in the largest range of halo mass and redshift. Using the shear catalog of the Dark Energy Camera Legacy Survey Data Release 8, we investigate the splash-back radius of halos associated with galaxies and galaxy clusters identified in the various catalogs. Our finding reveals a trend wherein massive halos demonstrate a larger splash-back radius, and the normalized splash-back radius (R
sp/R
200m) shows a U-shaped mass evolution. The upturn in these relations mainly comes from the contribution of massive halos with low redshifts. We further find the splash-back radius increases with the peak height, while the normalized splash-back radius has a negative relation with the peak height. We also find that R
sp ≳ R
200m for most halos, indicating their low accretion rates. Our result is consistent with previous literature across a wide range of mass, redshift, and peak height, as well as the simulation work from More et al.
C3NN: Cosmological Correlator Convolutional Neural Network an Interpretable Machine-learning Framework for Cosmological Analyses
Authors: Gong Zhengyangguang , Halder Anik , Bohrdt Annabelle , Seitz Stella , Gebauer David 
Published: August 2024

Abstract
Modern cosmological research in large-scale structure has witnessed an increasing number of machine-learning applications. Among them, convolutional neural networks (CNNs) have received substantial attention due to their outstanding performance in image classification, cosmological parameter inference, and various other tasks. However, many models based on CNNs are criticized as “black boxes” due to the difficulties in relating their outputs intuitively and quantitatively to the cosmological fields under investigation. To overcome this challenge, we present the Cosmological Correlator Convolutional Neural Network (C3NN)—a fusion of CNN architecture and cosmological N-point correlation functions (NPCFs). We demonstrate that its output can be expressed explicitly in terms of the analytically tractable NPCFs. Together with other auxiliary algorithms, we can open the “black box” by quantitatively ranking different orders of the interpretable outputs based on their contribution to classification tasks. As a proof of concept, we demonstrate this by applying our framework to a series of binary classification tasks using Gaussian and log-normal random fields and relating its outputs to the NPCFs describing the two fields. Furthermore, we exhibit the model’s ability to distinguish different dark energy scenarios (w
0 = −0.95 and −1.05) using N-body simulated weak-lensing convergence maps and discuss the physical implications coming from their interpretability. With these tests, we show that C3NN combines advanced aspects of machine learning architectures with the framework of cosmological NPCFs, thereby making it an exciting tool to extract physical insights in a robust and explainable way from observational data.
Spatially Resolved Analysis of Stellar Populations in NGC 2992: Impact of Active Galactic Nucleus Feedback
Authors: Xu 许 Xiaoyu 啸宇 , Wang Junfeng , Li Zhiyuan , Chen Yanmei 
Published: August 2024

Abstract
In NGC 2992, a galaxy-scale ionized gas outflow driven by active galactic nuclei (AGNs) has long been recognized, yet its impact on the host galaxy has remained elusive. In this paper, we utilize data from the archival Very Large Telescope/MUSE to present a spatially resolved analysis of stellar populations in this galaxy. Two different stellar population templates are employed to fit the stellar continuum, allowing us to determine the light-weighted stellar age, metallicity, the fraction of the young stellar population (age <100 Myr, P
Y), and the average age and metallicity of P
Y. Our results reveal the presence of a very young stellar population (≤40 Myr) within the dust lane and nearly along the galaxy’s major axis. The light-weighted stellar age and the fraction of P
Y show negative trends along the major and minor axes. The average age and metallicity of P
Y present positive trends with increasing distance, except along the northern direction of the major axis. Within the circumnuclear region (<1 kpc), the distribution of the young stellar population is spatially anticorrelated with the AGN outflow cone. The highest fraction of P
Y is observed at the outskirts of the nuclear radio bubble in the northern region near the nucleus. Considering the coupling efficiency and timescales, we propose that the AGN outflow in this galaxy may exert both negative and positive feedback on its host. Additionally, the star formation and the AGN activities could be attributed to the interaction between NGC 2992 and NGC 2993.
JWST Photometry of Globular Clusters in A2744. II. Luminosity and Color Distributions
Authors: Harris William E. , Reina-Campos Marta 
Published: August 2024

Abstract
Deep JWST imaging of the giant galaxy cluster A2744, at redshift z = 0.308, is used to explore the features of its rich population of globular clusters (GCs), building on our initial survey of the system. We use the photometry of more than 10,000 GCs over a 3 mag range to construct the GC luminosity function and color distribution. These results now specifically account for photometric incompleteness as a function of location relative to the five giant galaxies that dominate the gravitational potential of A2744. The total GC population in A2744 is estimated at N
GC ≥ 1.1 × 105, consistent with its high total mass. We also directly compare the observed distributions with theoretical predictions for GC populations drawn from the recent EMP-Pathfinder simulations, viewed at the same 3.5 Gyr look-back time as the cluster. The simulations match the observations well, with the only notable disagreement being that the simulations predict larger numbers of GCs at high metallicity formed after z ≃ 2 than are seen in the data.
Simulated Coronal Mass Ejections on a Young Solar-type Star and the Associated Instantaneous Angular Momentum Loss
Authors: Xu Yu , Alvarado-Gómez Julián D. , Tian Hui , Poppenhäger Katja , Guerrero Gustavo , Liu Xianyu 
Published: August 2024

Abstract
Coronal mass ejections (CMEs) on stars can change the stars’ magnetic field configurations and mass-loss rates during the eruption and propagation and therefore, may affect the stars’ rotation properties on long timescales. The dynamics of stellar CMEs and their influence on the stellar angular momentum loss rate are not yet well understood. In order to start investigating these CME-related aspects on other stars, we conducted a series of magnetohydrodynamic simulations of CMEs on a solar-type star of moderate activity levels. The propagation and evolution of the CMEs were traced in the three-dimensional outputs and the temporal evolution of their dynamic properties (such as masses, velocities, and kinetic energies) were determined. The simulated stellar CMEs are more massive and energetic than their solar analog, which is a result of the stronger magnetic field on the surface of the simulated star than that of the Sun. The simulated CMEs display masses ranging from ∼1016 to ∼1018 g and kinetic energies from ∼1031 to ∼1033 erg. We also investigated the instantaneous influence of the CMEs on the star’s angular momentum loss rate. Our results suggest that angular momentum can either be added to or removed from the star during the evolution of CME events. We found a positive correlation between the amplitude of the angular momentum loss rate variation and the CME’s kinetic energy as well as mass, suggesting that more energetic/massive CMEs have a higher possibility to add angular momentum to the star.
Denser Environments Cultivate Larger Galaxies: A Comprehensive Study beyond the Local Universe with 3 Million Hyper Suprime-Cam Galaxies
Authors: Ghosh অরিত্র Aritra  ঘোষ , Urry C. Megan , Powell Meredith C. , Shimakawa Rhythm , van den Bosch Frank C. , Nagai Daisuke , Mitra Kaustav , Connolly Andrew J. 
Published: August 2024

Abstract
The relationship between galaxy size and environment has remained enigmatic, with over a decade of conflicting results. We present one of the first comprehensive studies of the variation of galaxy radius with environment beyond the local Universe and demonstrate that large-scale environmental density is correlated with galaxy radius independent of stellar mass and galaxy morphology. We confirm with >5σ confidence that galaxies in denser environments are up to ∼25% larger than their equally massive counterparts with similar morphology in less dense regions of the Universe. We achieve this result by correlating projected two-dimensional densities over ∼360 deg2 with the structural parameters of ∼3 million Hyper Suprime-Cam galaxies at 0.3 ≤ z < 0.7 with

log
M

/

M

⊙

≥
8.9

. Compared to most previous studies, this sample is ∼100–10,000 times larger and goes ∼1 dex deeper in mass completeness. We demonstrate that past conflicting results have been driven by small sample sizes and a lack of robust measurement uncertainties. We verify the presence of the above correlation separately for disk-dominated, bulge-dominated, star-forming, and quiescent subpopulations. We find the strength of the correlation to be dependent on redshift, stellar mass, and morphology. The correlation is strongest at lower redshifts and systematically weakens or disappears beyond z ≥ 0.5. At z ≥ 0.5, more massive galaxies still display a statistically significant correlation. Although some existing theoretical frameworks can be selectively invoked to explain some of the observed correlations, our work demonstrates the need for more comprehensive theoretical investigations of the correlation between galaxy size and environment.
Unraveling the Trigger Mechanism of Explosive Reconnection in Partially Ionized Solar Plasma
Authors: Zafar Abdullah , Ni Lei , Lin Jun , Ali Ahmad 
Published: August 2024

Abstract
Plasmoid instability usually accounts for the onset of fast reconnection events observed in astrophysical plasmas. However, the measured reconnection rate from observations can be one order of magnitude higher than that derived from magnetohydrodynamic (MHD) simulations. In this study, we present the results of magnetic reconnection in the partially ionized low solar atmosphere based on 2.5D MHD simulations. The whole reconnection process covers two different fast reconnection phases. In the first phase, the slow Sweet–Parker reconnection transits to the plasmoid-mediated reconnection, and the reconnection rate reaches about 0.02. In the second phase, a faster explosive reconnection appears, with the reconnection rate reaching above 0.06. At the same time, a sharp decrease in plasma temperature and density at the principle X-point is observed, which is associated with the strong radiative cooling, the ejection of hot plasma from the local reconnection region, or the motion of the principle X-point from a hot and dense region to a cool and less dense region along the narrow current sheet. This causes gas pressure depletion and increases magnetic diffusion at the main X-point, resulting in the local Petschek-like reconnection and a violent and rapid increase in the reconnection rate. This study for the first time reveals a common phenomenon where the plasmoid-dominated reconnection transits to an explosive faster reconnection with a rate approaching the order of 0.1 in partially ionized plasma in the MHD scale.
Hadronuclear Interactions in Active Galactic Nuclei Jets as the Origin of the Diffuse High-energy Neutrino Background
Authors: Xue Rui , Wang Ze-Rui , Joshi Jagdish C. , Li Wei-Jian 
Published: August 2024

Abstract
The origin of diffuse high-energy neutrinos from TeV to PeV energies detected by the IceCube Observatory remains a mystery. In our previous work, we have shown that hadronuclear (p − p) interactions in active galactic nuclei (AGNs) jets could be important and generate detectable very-high-energy emissions. Here, we further explore these interactions in the AGN jets based on their luminosity function. The diffuse neutrino flux and corresponding γ-ray flux have been calculated and compared with observational data. In our modeling, two beaming patterns are considered separately. To make sure that the corresponding γ-ray flux does not overshoot the diffuse γ-ray background, we find that if the neutrino production region in a jet is opaque to γ-rays, p − p interactions in AGN jets with a small viewing angle (the blazar case) are able to interpret the PeV neutrino background. Similarly, AGN jets with a large viewing angle (the radio galaxy case) may interpret the TeV neutrino background. While, if the neutrino production region is transparent to γ-rays, only blazars have the potential to interpret the diffuse neutrino background around the PeV band. Some caveats are also discussed.
Detecting Gravitational-wave Bursts from Black Hole Binaries in the Galactic Center with LISA
Authors: Knee Alan M. , McIver Jess , Naoz Smadar , Romero-Shaw Isobel M. , Hoang Bao-Minh , Grishin Evgeni 
Published: August 2024

Abstract
Stellar-mass black hole binaries (BHBs) in galactic nuclei are gravitationally perturbed by the central supermassive black hole (SMBH) of the host galaxy, potentially inducing strong eccentricity oscillations through the eccentric Kozai–Lidov mechanism. These highly eccentric binaries emit a train of gravitational-wave (GW) bursts detectable by the Laser Interferometer Space Antenna (LISA)—a planned space-based GW detector—with signal-to-noise ratios up to ∼100 per burst. In this work, we study the GW signature of BHBs orbiting our galaxy’s SMBH, Sgr A*, which are consequently driven to very high eccentricities. We demonstrate that an unmodeled approach using a wavelet decomposition of the data effectively yields the time-frequency properties of each burst, provided that the GW frequency peaks between 10−3 and 10−1 Hz. The wavelet parameters may be used to infer the eccentricity of the binary, measuring

log

10

(
1
−
e
)

within an error of 20%. Our proposed search method can thus constrain the parameter space to be sampled by complementary Bayesian inference methods, which use waveform templates or orthogonal wavelets to reconstruct and subtract the signal from LISA data.
Impacts on Ocean Worlds Are Sufficiently Frequent and Energetic to Be of Astrobiological Importance
Authors: MacKenzie Shannon M. , Pontefract Alexandra , Daly R. Terik , Buffo Jacob J. , Osinski Gordon R. , Cline Christopher J. , Cintala Mark J. , Craft Kathleen L. , Kinczyk Mallory J. , Hedgepeth Joshua , Hörst Sarah M. , Méndez Abel , Pearce Ben K. D. , Stickle Angela M. , Vance Steven D. 
Published: August 2024

Abstract
Evidence for the beneficial role of impacts in the creation of urable or habitable environments on Earth prompts the question of whether meteorite impacts could play a similar role at other potentially urable/habitable worlds like Enceladus, Europa, and Titan. In this work, we demonstrate that to first order, impact conditions on these worlds are likely to have been consistent with the survival of organic compounds and/or sufficient for promoting synthesis in impact melt. We also calculate melt production and freezing times for crater sizes found at Enceladus, Europa, and Titan and find that even the smallest craters at these worlds offer the potential to study the evolution of chemical pathways within impact melt. These first-order calculations point to a critical need to investigate these processes at higher fidelity with lab experiments, sophisticated thermodynamic and chemical modeling, and, eventually, in situ investigations by missions.
Les plans d’eau qui n’existent plus réchauffent-ils les cours d’eau ? L’exemple de l’impact d’un étang en assec (commune de Cieux, Haute-Vienne)
Authors: Touchart Laurent , Bartout Pascal 
Published: August 2024

Le but de la recherche est d’évaluer l’impact thermique d’un étang limousin à déversoir de surface de 2,2 ha sur un ruisseau de rang 1, et de comparer ce résultat, d’une part avec l’influence du même plan d’eau mis en assec, d’autre part avec un second étang resté en eau. La recherche s’appuie sur 8 ans de mesures horaires de température de l’eau. Elle est cadrée par une réflexion épistémologique menant à une nouvelle typologie des démarches empiriques existantes (température d’effacement, de rétablissement, de transfert, de reconstruction, d’équilibre, de reconstitution) et remettant en cause l’assimilation trop souvent pratiquée entre les températures d’entrée et de sortie du plan d’eau. De juin à septembre, le ruisseau est en moyenne de 6,0 °C plus chaud en aval qu’en amont quand l’étang est en eau, de 0,8 °C quand il est en assec. En eau, ce sont les minima qui sont le plus augmentés, en assec ce sont les maxima. Un gradient moyen de réchauffement du ruisseau de 0,27 °C/100 m est mesuré d’amont en aval. Comparé avec le réchauffement dû à l’étang sur la même distance, il permet d’estimer que l’évolution naturelle du ruisseau est responsable de 15 % du réchauffement, l’étang en causant 85 %. Sur une distance plus grande prenant en compte l’impact cumulé d’une chaîne de deux étangs, la part de l’évolution naturelle du cours d’eau monte à 26 %.
Bevacizumab for Retinopathy of Prematurity Is Not Associated With Systemic Hypertension
Authors: Akbar Mizna , Avdagic Ema , Carlos Christine , Blair Michael , Yang Carina , Rodriguez Sarah Hilkert 
Published: August 2024

Purpose
To evaluate for an association between systemic hypertension and intravitreal bevacizumab (IVB) for retinopathy of prematurity (ROP) treatment, due to a 2020 case report of a neonate with ROP developing systemic hypertension and posterior reversible encephalopathy syndrome (PRES) after IVB and limited data on long-term safety of IVB.

Methods
A retrospective cohort study was conducted using vital signs for 90 days, comparing IVB to laser treatment. The primary outcome was short-term hypertension, recorded for at least 3 consecutive days following treatment. As a secondary outcome, infants treated with IVB were also compared to infants with severe ROP who experienced spontaneous regression without treatment. Rates of long-term hypertension, based on chart diagnoses at discharge, were also reviewed. Neuroimaging was re-reviewed to evaluate for vasogenic edema consistent with PRES.

Results
Overall, 137 infants with severe ROP were included, of whom 94 required treatment. There were no baseline differences in neonatal comorbidities comparing laser to IVB. There was no difference on unadjusted or adjusted logistic regression comparing odds of short-term hypertension after IVB to laser (adjusted odds ratio: 0.69, 095% CI: 0.25, 1.87). There was no significant difference in the rate of long-term hypertension diagnoses by treatment group.

Conclusions
The lack of association between IVB and short-term systemic hypertension is reassuring. Further studies are warranted to confirm this.

[
J Pediatr Ophthalmol Strabismus
. 2024;61(6):434–441.]
Predictors of No-Show Status: An Analysis of Pediatric Ophthalmology Patients at an Academic Ophthalmology Department in the United States
Authors: Borkhetaria Rucha K. , Hussain Zain S. , Giang Vanna , Ely Amanda L. 
Published: August 2024

Purpose
To identify pediatric patient and appointment characteristics associated with no-show status at a tertiary care pediatric ophthalmology clinic within a U.S. academic ophthalmology department.

Methods
A cross-sectional retrospective chart review was performed for all pediatric patients with a scheduled ophthalmology appointment at the Penn State Eye Center between April 1, 2022 and March 31, 2023. A multivariate logistic regression analysis assessed associations between appointment nonattendance and patient characteristics.

Results

Of 8,083 scheduled visits, 1,445 (17.9%) were no-shows. Factors associated with no-show status included appointment type (new vs return odds ratio [OR]: 1.43, 95% CI: 1.26 to 1.63,
P
< .001); lower median household income (< $41,374 vs > $68,957 OR: 1.89, 95% CI: 1.40 to 2.55,
P
< .001; $41,374 to $68,957 vs > $68,957 OR: 1.27, 95% CI: 1.12 to 1.44,
P
< .001); non-private insurance (self-pay vs private: OR: 5.65, 95% CI: 3.87 to 8.24,
P
< .001, Medicaid vs private: OR: 2.17, 95% CI: 2.32 to 3.16,
P
< .001); commute distance 10 to 30 miles vs < 5 miles (OR: 1.49, 95% CI: 1.11 to 1.99,
P
= .008); race: unavailable vs White (OR: 2.18, 95% CI: 1.66 to 2.85,
P
< .001), Black vs White (OR: 1.86, 95% CI:1.53 to 2.27,
P
< .001), Other vs White (OR: 1.47, 95% CI: 1.27 to 1.70,
P
< .001); ethnicity: Hispanic vs non-Hispanic (OR: 1.92, 95% CI: 1.62 to 2.27,
P
< .001); and language preference: Spanish vs English (OR: 1.86, 95% CI: 1.49 to 2.32,
P
< .001), Nepali vs English (OR: 1.60, 95% CI: 1.06 to 2.43,
P
= .027), other vs English (OR: 1.83, 95% CI: 1.35 to 2.49,
P
< .001). Appointment reminders (phone call,
P
= .013); text message,
P
< .001; other,
P
= .013) all resulted in a greater propensity to show, but email communication alone did not (
P
= .674).

Conclusions
Certain patient and appointment characteristics that are linked to a higher rate of no-show status can inform targeted initiatives to improve health care outcomes, resource utilization, and clinical efficiency in the pediatric ophthalmology community.

[
J Pediatr Ophthalmol Strabismus
. 2024;61(6):442–451.]
APPLICATION ANALYSIS OF PHOTOVOLTAIC INTEGRATED SHADING DEVICES CONSIDERING INDOOR ENVIRONMENT AND ENERGY CHANGE IN GREEN BUILDINGS
Authors: Wang Peng , Wang Wei , Jia Ling , Wang Chenglong , Zhang Wendi , Huang Lei 
Published: August 2024

ABSTRACT
Constructing solar-powered cities with photovoltaic panels installed on building façades saves energy and reduces carbon emissions. Since photovoltaic integrated shading devices (PVSDs) differ from rooftop photovoltaics, their design must consider power generation capacity, indoor thermal environment, and lighting control to maximise the energy-saving potential. This study simulates and evaluates the performance of PVSDs combined lighting control in energy-efficient buildings based on EnergyPlus and addresses the conflict between the indoor environment and photovoltaic power generation by optimising the geometric parameters of photovoltaic systems in China's hot summer and cold winter (HSCW) zones. The findings indicate that the combined lighting control mitigates the detrimental effects of PVSDs on lighting, and the design optimisation makes it possible to acquire positive shading benefits and significantly boost the performance of PVSDs, thus saving more energy than rooftop photovoltaics. The maximum energy-saving rate of a room with 12.5% of its façade wall utilised reached 49.295%. This study provides an example of the practical application and evaluation of PVSDs in HSCW zones.