bluuebunny/crossref_metadata_2025_split huggingface dataset:
Use of Population Weighted Density Index for Coronavirus Spread in the United States
Authors: Yuce Huseyin , Stauss Hannah , Persad Adrienne 
Published: July 2024

Background: Understanding how population density affected the transmission of COVID-19 is vitally important, since crowded cities were the epicenters for the disease. Since human contact was the main cause of the spread, population-weighted densities have been shown to be a better measure than conventional densities, since the variation in density across subareas matters more than the density in the total area. Objectives: This study investigates the impact of population-weighted density and other demographics on the rate of COVID-19 spread in the United States. Methods: The study considers population-weighted density and many other demographics. The population-weighted density index is the weighted average of density across the tracts, where tracts are weighted by population. Multivariate analysis has been used to determine the elasticity of the spread. Results: Using U.S. county-level data, we calculated the elasticity of COVID-19 spread with respect to population-weighted density to be 0.085 after controlling for other factors. In addition to the density, the proportion of people over 65 years of age, the number of total healthcare workers, and average temperature in each county positively contributed to the case numbers, while education level and income per capita had a negative effect. Discussion: For the spread, understanding the population characteristics and dynamics is as important as understanding the infectious disease itself. This will help policy makers to utilize and reallocate the resources more effectively. If the spread is successfully contained early, there will be less stress placed upon the healthcare system, resulting in better healthcare access for those who are sick. Conclusions: Our analysis suggests that population-weighted density can be a useful tool to control and manage outbreaks, especially within the early stage of the spread. We presented the early dynamics of the spread and recommended a policy measure on how to transfer healthcare workers from low-spread-risk areas to high-spread-risk areas to utilize resources better.
Estimating the Health-Related Quality of Life Benefit of Prophylactic Treatment for COVID-19 in Immunocompromised People: A Multimethod Valuation Study
Authors: Gallop Katy , Hall Rebekah , Watt Michael , Squirrell Daniel , Branscombe Neil , Arnetop Sofie , Lloyd Andrew 
Published: July 2024

Background: Pre-exposure prophylaxis (PrEP) for COVID-19 provides additional protection, beyond vaccines alone, for individuals who are immunocompromised (IC). This may reduce the need for preventative behavioral modification, such as shielding—a behavioral restriction limiting an IC individual to minimize face-to-face interactions and/or crowded places. Therefore, PrEP may improve psychosocial well-being and health-related quality of life (HRQoL) for individuals with IC conditions. Objective: To estimate the potential HRQoL and utility benefit of PrEP for prevention of COVID-19 in individuals with IC conditions who may not have an adequate response of full vaccination (and therefore are at “highest risk” of severe COVID-19) that can be used in future economic evaluations of preventative therapies against COVID-19. Methods: Vignettes describing HRQoL associated with 2 pre-PrEP states (shielding and semi-shielding behavioral restrictions) and a post-PrEP state were developed from a literature review and tested through interviews with clinicians (n = 4) and individuals with IC conditions (n = 10). Vignettes were valued by a general population sample (N = 100) using a visual analog scale (VAS), time trade-off (TTO), and EQ-5D-5L. A sample of individuals with IC conditions (n = 48) valued their current HRQoL and a post-PrEP vignette using VAS and EQ-5D-5L. Results: Individuals with IC conditions reported a mean current EQ-5D-5L score of 0.574, and 0.656 for post-PrEP based on the vignette. PrEP would lead to behavior changes for 75% (30/40) of individuals with IC conditions and an emotional benefit for 93% (37/40) of individuals with IC conditions. Mean values from the general population valuation based on EQ-5D-5L ranged from 0.606 (“shielding”) to 0.932 (“post-PrEP”). Conclusion: This study quantified the expected health state utility benefit of reduced psychosocial burden and behavioral restriction. PrEP would potentially result in a utility gain between 0.082 and 0.326, dependent on valuation approach and expected change in behavioral restrictions, leading to improvements in daily activities and emotional well-being.
Three-dimensional visualization technology for guiding one-step percutaneous transhepatic cholangioscopic lithotripsy for the treatment of complex hepatolithiasis
Authors: Ye Yong-Qing , Cao Ya-Wen , Li Rong-Qi , Li En-Ze , Yan Lei , Ding Zhao-Wei , Fan Jin-Ming , Wang Ping , Wu Yi-Xiang 
Published: July 2024

BACKGROUND
Biliary stone disease is a highly prevalent condition and a leading cause of hospitalization worldwide. Hepatolithiasis with associated strictures has high residual and recurrence rates after traditional multisession percutaneous transhepatic cholangioscopic lithotripsy (PTCSL).
AIM
To study one-step PTCSL using the percutaneous transhepatic one-step biliary fistulation (PTOBF) technique guided by three-dimensional (3D) visualization.
METHODS
This was a retrospective, single-center study analyzing, 140 patients who, between October 2016 and October 2023, underwent one-step PTCSL for hepatolithiasis. The patients were divided into two groups: The 3D-PTOBF group and the PTOBF group. Stone clearance on choledochoscopy, complications, and long-term clearance and recurrence rates were assessed.
RESULTS
Age, total bilirubin, direct bilirubin, Child-Pugh class, and stone location were similar between the 2 groups, but there was a significant difference in bile duct strictures, with biliary strictures more common in the 3D-PTOBF group (P = 0.001). The median follow-up time was 55.0 (55.0, 512.0) days. The immediate stone clearance ratio (88.6% vs 27.1%, P = 0.000) and stricture resolution ratio (97.1% vs 78.6%, P = 0.001) in the 3D-PTOBF group were significantly greater than those in the PTOBF group. Postoperative complication (8.6% vs 41.4%, P = 0.000) and stone recurrence rates (7.1% vs 38.6%, P = 0.000) were significantly lower in the 3D-PTOBF group.
CONCLUSION
Three-dimensional visualization helps make one-step PTCSL a safe, effective, and promising treatment for patients with complicated primary hepatolithiasis. The perioperative and long-term outcomes are satisfactory for patients with complicated primary hepatolithiasis. This minimally invasive method has the potential to be used as a substitute for hepatobiliary surgery.
Rats show up to 72 h of significant retention for spatial memory in the radial maze
Authors: Tanaka Chiaki , Taniuchi Tohru 
Published: July 2024

AbstractThis study explored long-term retention of spatial memory in rats using an eight-arm radial maze. Crystal and Babb (Learning and motivation, 39(4), 278–284, 2008) previously demonstrated that rats could retain spatial memory for up to 25 h in the radial maze. Notably, they found performance improved with 48-h intertrial intervals compared with 24-h intervals. Our study investigated the effects of extending intertrial intervals on long-term retention of spatial memory by reducing the potential for proactive interference. Each trial comprised a learning phase, during which subjects were required to sequentially visit four randomly selected arms, followed by a free-choice test that included all eight arms, conducted after increasing the retention and intertrial intervals. The retention intervals were systematically increased from 1 h to 24, 48, and, ultimately, 72 h, with corresponding intertrial intervals expanding from 24 to 48, 120, and 144 h. Performance significantly surpassed chance levels across all conditions, demonstrating that rats are capable of retaining spatial memory for up to 72 h.
Sensorimotor adaptation impedes perturbation detection in grasping
Authors: Müller Carl , Bendixen Alexandra , Kopiske Karl 
Published: July 2024

Abstract
Humans achieve skilled actions by continuously correcting for motor errors or perceptual misjudgments, a process called sensorimotor adaptation. This can occur with the actor both detecting (explicitly) and not detecting the error (implicitly). We investigated how the magnitude of a perturbation and the corresponding error signal each contribute to the detection of a size perturbation during interaction with real-world objects. Participants grasped cuboids of different lengths in a mirror-setup allowing us to present different sizes for seen and felt cuboids, respectively. Visuo-haptic size mismatches (perturbations) were introduced either abruptly or followed a sinusoidal schedule. These schedules dissociated the error signal from the visuo-haptic mismatch: Participants could fully adapt their grip and reduce the error when a perturbation was introduced abruptly and then stayed the same, but not with a constantly changing sinusoidal perturbation. We compared participants’ performance in a two-alternative forced choice (2AFC) task where participants judged these mismatches, and modelled error-correction in grasping movements by looking at changes in maximum grip apertures, measured using motion tracking. We found similar mismatch-detection performance with sinusoidal perturbation schedules and the first trial after an abrupt change, but decreasing performance over further trials for the latter. This is consistent with the idea that reduced error signals following adaptation make it harder to detect perturbations. Error-correction parameters indicated stronger error-correction in abruptly introduced perturbations. However, we saw no correlation between error-correction and overall mismatch-detection performance. This emphasizes the distinct contributions of the perturbation magnitude and the error signal in helping participants detect sensory perturbations.
CHIME/FRB Outriggers: KKO Station System and Commissioning Results
Authors: Lanman Adam E. , Andrew Shion , Lazda Mattias , Shah Vishwangi , Amiri Mandana , Balasubramanian Arvind , Bandura Kevin , Boyle P. J. , Brar Charanjot , Carlson Mark , Cliche Jean-François , Gusinskaia Nina , Hendricksen Ian T. , Kaczmarek J. F. , Landecker Tom , Leung Calvin , Mckinven Ryan , Mena-Parra Juan , Milutinovic Nikola , Nimmo Kenzie , Pearlman Aaron B. , Renard Andre , Rahman Mubdi , Shaw J. Richard , Siegel Seth R. , Smegal Rick J. , Cassanelli Tomas , Chatterjee Shami , Curtin Alice P. , Dobbs Matt , Dong Fengqiu Adam , Halpern Mark , Hopkins Hans , Kaspi Victoria M. , Khairy Kholoud , Masui Kiyoshi W. , Meyers Bradley W. , Michilli Daniele , Petroff Emily , Pinsonneault-Marotte Tristan , Pleunis Ziggy , Rafiei-Ravandi Masoud , Shin Kaitlyn , Smith Kendrick , Vanderlinde Keith , Zegmott Tarik J. 
Published: July 2024

Abstract
Localizing fast radio bursts (FRBs) to their host galaxies is an essential step to better understanding their origins and using them as cosmic probes. The Canadian Hydrogen Intensity Mapping Experiment (CHIME)/FRB Outriggers program aims to add very long baseline interferometry localization capabilities to CHIME, such that FRBs may be localized to tens of milliarcsecond precision at the time of their discovery, more than sufficient for host galaxy identification. The first-built outrigger telescope is the
Outrigger (KKO), located 66 km west of CHIME. Cross-correlating KKO with CHIME can achieve arcsecond precision along the baseline axis while avoiding the worst effects of the ionosphere. Since the CHIME–KKO baseline is mostly east/west, this improvement is mostly in right ascension. This paper presents measurements of KKO’s performance throughout its commissioning phase, as well as a summary of its design and function. We demonstrate KKO’s capabilities as a standalone instrument by producing full-sky images, mapping the angular and frequency structure of the primary beam, and measuring feed positions. To demonstrate the localization capabilities of the CHIME–KKO baseline, we collected five separate observations each, for a set of 20 bright pulsars, and aimed to measure their positions to within 5″. All of these pulses were successfully localized to within this specification. The next two outriggers are expected to be commissioned in 2024 and will enable subarcsecond localizations for approximately hundreds of FRBs each year.
The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). VI. The High-mass Stellar Initial Mass Function of M33
Authors: Wainer Tobin M. , Williams Benjamin F. , Johnson L. Clifton , Weisz Daniel R. , Dalcanton Julianne J. , Seth Anil C. , Dolphin Andrew , Durbin Meredith J. , Bell Eric F. , Chen Zhuo , Guhathakurta Puragra , Koch Eric W. , Lindberg Christina W. , Rosolowsky Erik , Sandstrom Karin M. , Skillman Evan D. , Smercina Adam , TorresVillanueva Estephani E. 
Published: July 2024

Abstract
We measure the high-mass stellar initial mass function (IMF) from resolved stars in M33 young stellar clusters. Leveraging the Hubble Space Telescope’s high resolving power, we fully model the IMF probabilistically. We first model the optical color–magnitude diagram of each cluster to constrain its power-law slope Γ, marginalized over other cluster parameters in the fit (e.g., cluster age, mass, and radius). We then probabilistically model the distribution of mass function (MF) slopes for a highly strict cluster sample of nine clusters more massive than log(Mass/M
⊙) = 3.6; above this mass, all clusters have well-populated main sequences of massive stars and should have accurate recovery of their MF slopes, based on extensive tests with artificial clusters. We find that the ensemble IMF is best described by a mean high-mass slope of

Γ

¯

=
1.49
±
0.18

, with an intrinsic scatter of

σ

Γ

2

=

0.02

0.00

+
0.16

, consistent with a universal IMF. We find no dependence of the IMF on environmental impacts such as the local star formation rate (SFR) or galactocentric radius within M33, which serves as a proxy for metallicity. This

Γ

¯

measurement is consistent with similar measurements in M31, despite M33 having a much higher SFR intensity. While this measurement is formally consistent with the canonical Kroupa (Γ = 1.30) IMF, as well as the Salpeter (Γ = 1.35) value, it is the second Local Group cluster sample to show evidence for a somewhat steeper high-mass IMF slope. We explore the impacts a steeper IMF slope has on a number of astronomical subfields.
Mapping the Milky Way in 5D with 170 Million Stars
Authors: Speagle 沈 Joshua S. 佳士 , Zucker Catherine , Bonaca Ana , Cargile Phillip A. , Johnson Benjamin D. , Beane Angus , Conroy Charlie , Finkbeiner Douglas P. , Green Gregory M. , Kamdar Harshil M. , Naidu Rohan , Rix Hans-Walter , Schlafly Edward F. , Dotter Aaron , Eadie Gwendolyn , Eisenstein Daniel J. , Goodman Alyssa A. , Han Jiwon Jesse , Saydjari Andrew K. , Ting 丁 Yuan-Sen 源森 , Zelko Ioana A. 
Published: July 2024

Abstract
We present Augustus, a catalog of distance, extinction, and stellar parameter estimates for 170 million stars from 14 mag < r < 20 mag and with ∣b∣ > 10° drawing on a combination of optical to near-infrared photometry from Pan-STARRS, 2MASS, UKIDSS, and unWISE along with parallax measurements from Gaia DR2 and 3D dust extinction maps. After applying quality cuts, we find 125 million objects have “high-quality” posteriors with statistical distance uncertainties of ≲10% for objects with well-constrained stellar types. This is a substantial improvement over the distance estimates derived from Gaia parallaxes alone and in line with the recent results from Anders et al. We find the fits are able to reproduce the dereddened Gaia color–magnitude diagram accurately, which serves as a useful consistency check of our results. We show that we are able to detect large, kinematically coherent substructures in our data clearly relative to the input priors, including the Monoceros Ring and the Sagittarius Stream, attesting to the quality of the catalog. Our results are publicly available at doi:10.7910/DVN/WYMSXV. An accompanying interactive visualization can be found at http://allsky.s3-website.us-east-2.amazonaws.com.
Extraction of Sunspots from Chinese Sunspot Drawings Based on Semisupervised Learning
Authors: Dong Qianqian , Yang Yunfei , Feng Song , Dai Wei , Liang Bo , Xiong Jianping 
Published: July 2024

Abstract
China has six observing stations, providing over 52,000 handwritten sunspot drawings from 1947–2016. The observing stations are the Purple Mountain Astronomical Observatory (PMO), Yunnan Astronomical Observatory (YNAO), Qingdao Observatory Station (QDOS), Sheshan Observatory Station (SSOS), Beijing Planetarium (BJP), and Nanjing University (NJU). In this paper, we propose a new cotraining semisupervised learning method combining a semantic segmentation method named dynamic mutual training (DMT) boundary-guided semantic segmentation (BGSeg), i.e., DMT_BGSeg, which makes full use of the labeled data from PMO and the unlabeled data from the other five stations to detect and segment sunspot components in all sunspot drawings of the six Chinese stations. The sunspot is detected and segmented. Additionally, each sunspot is split into four types of components: pore, spot, umbra, and hole. The testing results show the mIoU values of PMO, YNAO, BJP, NJU, QDOS and SSOS are 85.29, 72.65, 73.82, 64.28, 62.26, and 60.07, respectively. The results of the comparison also show that DMT_BGSeg is effective in detecting and segmenting sunspots in Chinese sunspot drawings. The numbers and areas of sunspot components are measured separately. All of the detailed data are publicly shared on China-VO, which will advance the comprehensive augmentation of the global historical sunspot database and further the understanding of the long-term solar activity cycle and solar dynamo.
SpectAcLE: An Improved Method for Modeling Light Echo Spectra
Authors: Partoush Roee , Rest Armin , Jencson Jacob E. , Poznanski Dovi , Foley Ryan J. , Kilpatrick Charles D. , Andrews Jennifer E. , Angulo Rodrigo , Badenes Carles , Bianco Federica B. , Filippenko Alexei V. , Ridden-Harper Ryan , Li Xiaolong , Margheim Steve , Matheson Thomas , Olsen Knut A. G. , Siebert Matthew R. , Smith Nathan , Welch Douglas L. , Zenteno A. 
Published: July 2024

Abstract
Light echoes give us a unique perspective on the nature of supernovae and nonterminal stellar explosions. Spectroscopy of light echoes can reveal details on the kinematics of the ejecta, probe asymmetry, and reveal details of ejecta interaction with circumstellar matter, thus expanding our understanding of these transient events. However, the spectral features arise from a complex interplay between the source photons, the reflecting dust geometry, and the instrumental setup and observing conditions. In this work, we present an improved method for modeling these effects in light echo spectra, one that relaxes the simplifying assumption of a light-curve-weighted sum, and instead estimates the true relative contribution of each phase of a transient event to the observed spectrum. We discuss our logic, the gains we obtain over light echo analysis methods used in the past, and prospects for further improvements. Lastly, we show how the new method improves our analysis of echoes from Tycho’s supernova (SN 1572) as an example.
On the Origin of Fast-rotating Stars. I. Photometric Calibration and Results of AO-assisted BVRI+Hα Imaging of NGC 330 with SAMI/SOAR
Authors: Navarete Felipe , Ticiani dos Santos Pedro , Carciofi Alex Cavaliéri , Figueiredo André Luiz 
Published: July 2024

Abstract
Hα emission is a clear indicator of circumstellar activity in Be stars, historically employed to assess the classical Be star (CBe) population in young open clusters (YOCs). The YOC NGC 330 in the Small Magellanic Cloud exhibits a large known fraction of CBe stars and was selected for a pilot study to establish a comprehensive methodology for identifying Hα emitters in the Magellanic Clouds, encompassing the entire B-type spectral range. Using the SOAR Adaptive Module Imager (SAMI), we investigated the stellar population of NGC 330 using multiband BVRI+Hα imaging. We identified Hα emitters within the entire V-band range covered by SAMI/SOAR observations (V ≲ 22), comprising the complete B-type stellar population and offering a unique opportunity to explore the Be phenomenon across all spectral subclasses. The stellar radial distribution shows a clear bimodal pattern between the most massive (B5 or earlier) and the lower mass main-sequence objects (later than B6) within the cluster. The former is concentrated toward the cluster center (showing a dispersion of σ = 4.26 ± 0.20 pc), whereas the latter extends across larger radii (σ = 10.83 ± 0.65 pc), indicating mass stratification within NGC 330. The total fraction of emitters is 4.4% ± 0.5%, notably smaller than previous estimates from flux- or seeing-limited observations. However, a higher fraction of Hα emitters is observed among higher mass stars (32.8% ± 3.4%) than within lower mass (4.4% ± 0.9%). Consequently, the putative CBe population exhibits distinct dynamical characteristics compared to the bulk of the stellar population in NGC 330. These findings highlight the significance of the current observations in providing a complete picture of the CBe population in NGC 330.
Formation and Evolution of Transient Prominence Bubbles Driven by Erupting Minifilaments
Authors: Guo Yilin , Hou Yijun , Li Ting , Shen Yuandeng , Wang Jincheng , Zhang Jun , Zheng Jianchuan , Wang Dong , Mei Lin 
Published: July 2024

Abstract
Prominence bubbles, the dark arch-shaped voids below quiescent prominences, are generally believed to be caused by the interaction between the prominences and the slowly emerging or quasi-stable underlying magnetic loops. However, this scenario could not explain some short-lived bubbles with extremely dynamic properties of evolution. Based on high-resolution Hα observations, here we propose that bubbles should be classified into two categories according to their dynamic properties: quasi-steady Type-I bubbles and transient Type-II bubbles. Type-I bubbles could remain relatively stable and last for several hours, indicating the existence of a quasi-stable magnetic topology, while Type-II bubbles grow and collapse quickly within 1 hr without stability duration, which are usually associated with erupting minifilaments. Analysis of several typical Type-II bubbles from different views, especially including an on-disk event, reveals that Type-II bubbles quickly appear and expand at a velocity of ∼5–25 km s−1 accompanied by an erupting minifilament below. The minifilament’s rising velocity is slightly larger than that of the Type-II bubbles’ boundary, which will lead to the collision with each other in a short time, subsequent collapse of Type-II bubbles, and formation of a large plume into the above prominence. We also speculate that only if the angle between the axis of the erupting minifilament and the line of sight is large enough, the interaction between the erupting minifilament and the overlying prominence could trigger a Type-II bubble with a typical arch-shaped but quickly expanding bright boundary.